Search results “Determining orbital period of saturn”
Gravitation (6 of ) Calculating the Orbital Period of a Satelite
Shows how to calculate the orbital period of a Satellite. The equation for orbital period is derived from Newton's second law and Newton's Law of universal gravitation. You can see a listing of all my videos at http://www.stepbystepscience.com
Views: 17649 Step-by-Step Science
Orbital Period & Rotation Period
How long does the Earth and the other planets finish orbiting around the Sun? MERCURY - 88 Days VENUS - 224 Days EARTH - 365 Days MARS - 687 Days JUPITER - 11 Years SATURN - 29 Years URANUS - 84 Years NEPTUNE - 165 Years The time that the planets finish orbiting around the Sun is called a year. -------------------------------------------------------- How long does the Earth and the other planets finish rotating? MERCURY - 59 Days VENUS - 245 Days EARTH - 24 Hours MARS - 24 Hours JUPITER - 9 Hours SATURN - 10 Hours URANUS - 17 Hours NEPTUNE - 16 Hours The time that the planets finish rotating is called a day.
Views: 25539 Blanding Cassatt
Mathematics : How to Calculate Orbital Velocity
To calculate orbital velocity, first you must understand the components of the formula. Learn more about orbital velocity with help from math teacher in this free video on mathematics. Expert: Jimmy Chang Bio: Jimmy Chang has a master's degree in math and has been a math teacher at St. Pete College for more than eight years. Filmmaker: Christopher Rokosz Series Description: Mathematics involves many different formulas and terms that may be unfamiliar or difficult. Learn more about math terminology and skills with help from math teacher in this free video series on mathematics.
Views: 28578 eHowEducation
Orbital Period of the Moon
Use Newton's version of Kepler's 3rd law to calculate the orbital period of the moon.
Views: 7087 drlerocks
How Long Planets Take to Orbit the Sun | Solar Year of Other Planets as Compared to Earth
The length of a year on any given planet is determined by how long it takes for that planet to make one revolution around the sun. Since every planet travels at a different speed and has a different orbital path in regard to size and shape, the length of a year can vary greatly from planet to planet. If you had lived on a different planet your whole life, then you would be a different age due to the orbital differences. 1. Mercury: One year on planet Mercury takes just 87.97 earth days. This means that if you are 15 years old on Earth you would be 62 years old in Mercury years. 2. Venus: It takes 224.7 earth days for Venus to travel once around the sun. If you are 15 years old on Earth, this would make you 24 years old in Venus years. 3. Earth: One year on planet Earth, or one orbit around the sun, takes 365.26 days. 4. Mars: Planet Mars goes around the sun once every 686.98 earth days. Hence, a 15 years old from Earth would actually be almost 8 years old in Mars years. 5. Jupiter: The planet Jupiter travels around the sun one time every 4,332.82 earth days. This would make a 15 year old from earth be barely over 1 year old in Jupiter years. 6. Saturn: Saturn goes around the sun once every 10,755.7 earth days. If you had lived 15 years on Earth, then you would be a little over half of one year old in Saturn years. 7. Uranus: Uranus completes one revolution around the sun every 30,687.15 earth days. Thus, a 15 year old from earth would be .17 years old in Uranus years. 8. Neptune: It takes Neptune 60,190.03 earth days to go around the sun. A 15 year old from Earth would be .09 years old in Neptune years. ▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪ Follow us on Facebook : https://goo.gl/3uCit3 Follow me on Twitter : https://goo.gl/zVPgbn Follow me on Instagram : @siddhantjacobofficial. ▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪▪ Music: http://www.purple-planet.com
Views: 24624 The Brainshow
Calculate Mass of a Planet from Kepler & Newton's Laws
Solving for the mass of Jupiter using Io's orbital period and radius.
Views: 14879 julievandermeij
Kepler's Third Law, Perihelion Distance Halley's Comet
This video explains Kepler's Third Law for planets. Calculations are done to find period and semimajor axis values. The perihelion distance for Halley's Comet is calculated given the semimajor axis and eccentricity values. Introductory General Astronomy Prof. Greg Clements
Views: 1875 Greg Clements
Saturn's Mass
Use Newton's version of Kepler's 3rd law to calculate the mass of Saturn.
Views: 1220 drlerocks
Titan-Hyperion 4:3 Orbit Resonance
Titan and Hyperion orbit Saturn with periods of 15.94542 and 21.27661 Earth days, respectively. Their period ratio is very close to 4/3, with Titan making very close to 4 orbits for every 3 orbits that Hyperion makes. Because of this orbit resonance, Titan gives Hyperion a forced eccentricity of 0.123. Notice how Hyperion is farthest from Saturn at conjunction with Titan; such avoidance is typical of resonances. In the video, I made the resonance exact, gave Titan a circular orbit, and drew Saturn and its rings to scale, but not Titan or Hyperion. TtnT, HypT, and SynT are times in Titan orbits, Hyperion orbits, and synodic periods.
Views: 5061 Loren Petrich
Other Gas Giant Orbits
In which show you how your method for calculating orbits needs to be modified to accommodate Classical gas giants (Jupiter), Super Jupiters, Eccentric Jupiters and Gas Dwarfs. Check out the previous video for more info at: https://www.youtube.com/watch?v=lfY7NOpmClg ————— Artifexian on the Interweb: Youtube: https://www.youtube.com/artifexian Facebook: https://www.facebook.com/artifexian Twitter: https://www.twitter.com/artifexian Blog: http://www.scifiideas.com ————— General orbital equations and ranges: Semi major axis: 0.04 - 0.05 AU Eccentricity: 0 - 1 (pref. 0.00x - 0.0x) Equation of an ellipse: x^2/a^2 + y^2/b^2 = 1 Semi-minor axis: b = a*sqrt(1 - e^2) Periapsis (closest approach): q = a(1 - e) Apoapsis (furthest approach): Q = a(1 + e) Orbital period: P = sqrt(a^3/M) Orbital velocity: V_o = sqrt(M/R) Inclination: 0 - 180 deg Longitude of the ascending node: 0 - 360 deg Argument of Periapsis: 0 - 360 deg ————— Links: Universe sandbox: http://universesandbox.com/ ---------- SYSTEM STATS: Star: 1 solar mass Frost line: 4.85 AU Outer limit: 40 AU Hot jupiter: Semi-major axis: 0.07 AU Eccentricity: 0.001 Semi-minor axis: 0.069999965 AU Periapsis: 0.06993 AU Apoapsis: 0.07007 AU Orbital period: 0.0185 = ca 6.75 days Orbital velocity: 3.779 = ca 112.54 km/s Inclination: 176 deg (Retrograde orbit) Longitude of the ascending node: 279 deg Argument of periapsis: 14 deg Super Jupiter (Has migrated inwards – not yet a hot jupiter): Semi-major axis: 2.925AU Eccentricity: 0.002 Semi-minor axis: 2.92499415 AU Periapsis: 2.91915 AU Apoapsis: 2.93085AU Orbital period: 5.002519678 Earth Years Orbital velocity: 0.5847053462 = ca 17.41 km/s Inclination: 1.5 deg (Prograde orbit) Longitude of the ascending node: 13 deg Argument of periapsis: 222 deg Classical gas giant: Semi-major axis: 5.85AU Eccentricity: 0.003 Semi-minor axis: 5.849973675 AU Periapsis: 5.83245 AU Apoapsis: 5.86755 AU Orbital period: 14.14926235 Earth Years Orbital velocity: 0.4134491153 = ca 12.31 km/s Inclination: 0.75 deg (Prograde orbit) Longitude of the ascending node: 6 deg Argument of periapsis: 103 deg Eccentric jupiter: Semi-major axis: 11.7 AU Eccentricity: 0.2 Semi-minor axis: 11.463612AU Periapsis: 9.36 AU Apoapsis: 14.04 AU Orbital period: 40.02015742 Earth Years Orbital velocity: 0.2923526731 = ca 8.71 km/s Inclination: 2 deg (Prograde orbit) Longitude of the ascending node: 89 deg Argument of periapsis: 233 deg Gas Dwarf: Semi-major axis: 38 AU Eccentricity: 0.04 Semi-minor axis: 37.96958783 AU Periapsis: 36.48 AU Apoapsis: 39.52 AU Orbital period: 234.2477321 Earth Years Orbital velocity: 0.162214211 = ca 4.83 km/s Inclination: 3.75 deg (Prograde orbit) Longitude of the ascending node: 273 deg Argument of periapsis: 43 deg
Views: 42049 Artifexian
How Do Satellites Get & Stay in Orbit?
SciShow Space takes you into Low Earth Orbit to explain how artificial satellites get up there and stay there -- at least for a while. ---------- Like SciShow? Want to help support us, and also get things to put on your walls, cover your torso and hold your liquids? Check out our awesome products over at DFTBA Records: http://dftba.com/artist/52/SciShow Or help support us by subscribing to our page on Subbable: https://subbable.com/scishow ---------- Looking for SciShow elsewhere on the internet? Facebook: http://www.facebook.com/scishow Twitter: http://www.twitter.com/scishow Tumblr: http://scishow.tumblr.com Thanks Tank Tumblr: http://thankstank.tumblr.com Sources: http://science.howstuffworks.com/satellite.htm http://science.howstuffworks.com/dictionary/astronomy-terms/artificial-satellite-info1.htm http://www.universetoday.com/93077/how-satellites-stay-in-orbit/ http://www.universetoday.com/42198/how-many-satellites-in-space/ http://www.nasa.gov/pdf/475144main_LP7-SatelliteOrbits_508.pdf http://www.nasa.gov/audience/forstudents/5-8/features/what-is-orbit-58.html#.U0hebl5wOFc http://www.nasa.gov/audience/forstudents/5-8/features/what-is-a-satellite-58.html#.U0hjdV5wOFc https://www.spacetelescope.org/about/history/sm3b_a_little_boost/ http://www.deepastronomy.com/how-the-hubble-space-telescope-will-die-video.html http://youtu.be/NpHOlmNtFTQ http://www.slate.com/articles/news_and_politics/explainer/2005/04/where_satellites_go_when_they_die.html http://newsfeed.time.com/2011/09/22/satellite-falling-to-earth-nasa-scientist-puts-it-into-perspective/
Views: 743328 SciShow Space
Escape velocities of Our Planets
Escape velocities of Our Planets
Physics - Mechanics: Gravity (11 of 20) Eccentricity Of A Planet's Orbits
Visit http://ilectureonline.com for more math and science lectures! In this video I will show you how to calculate the eccentricity of a planets orbit using Keppler's 1st law.
Views: 35144 Michel van Biezen
The Apparent Size of the planets
Description: Here I'm showing how the apparent size of some planets can change. All the images used were obtained using the following tools: 10 inch dobsonian telescope barlow lens 2x CAMERA ASI120 MC Some images look better than others, that is because some of them I've used some astrophotography techniques (stacked some hundreds of frames to obtain one good frame). But my ideia here ins't show details on the planets surfaces, but the diameter and how much it varies during some months of observations. The size of orbits aren't exact values, so I took some avarage values. Now some information about the celestial bodies: Apparent diameter: Object Min Max Moon: 29.43' 33.5' Sun: 31.6' 32.7' Mercury: 4.5'' 13.0'' Venus: 9.7'' 66.0'' Mars: 3.5'' 25.1'' Jupiter: 29.8'' 50.1'' Saturn: 14.5'' 20.1'' Uranus: 3.3'' 4.1'' Neptune: 2.2'' 2.4'' Diameter (real size): Moon: 3473 km Sun: 1.391.400 km Mercury: 4878 km Venus: 12100 km Mars: 6786 km Jupiter: 142984 km Saturn: 120536 km (rings ~ 300 000 km) Uranus: 51108 km Neptune: 49538 km Orbits- Avarage distances from the Sun Moon : 149.600.000 km ( and 384 400 from Earth) Sun: 0 km ;) Mercury: 57.910.000 km Venus: 108.200.000 km Mars: 227.940.000 km Jupiter: 778.330.000 km Saturn: 1.429.400.000 km Uranus: 2.870.990.000 km Neptune: 4.504.300.000 km Orbital period: Moon : 365,25 days ( and 27 days around the Earth) Mercury: 88 days Venus: 225 days Mars: 687 days Jupiter: 11,9 years Saturn: 29,6 years Uranus: 83,7 years Neptune: 165,4 years Descrição: Aqui estou mostrando como o tamanho aparente de alguns planetas pode mudar. Todas as imagens utilizadas foram obtidas usando as seguintes ferramentas: Telescópio dobsonian de 10 polegadas ou 254 mm lente barlow 2x CAMERA ASI120 MC Algumas imagens parecem melhores do que outras, porque algumas delas eu usei algumas técnicas de astrofotografia (empilhadas algumas centenas de quadros para obter uma boa moldura). Mas minha ideia aqui não mostra detalhes nas superfícies dos planetas, mas o diâmetro e quanto ele varia durante alguns meses de observações. O tamanho das órbitas não são exatos, então eu tirei alguns valores médios. Na descrição coloquei também algumas informações sobre os corpos celestes, dêem uma olhada (está na parte de cima) primeiro os valores de diâmetro aparente e depois valores das dimensões reais.
Views: 1582 AstronoMars Channel
Asteroids In Resonance With Jupiter
This video highlights 2 groups of asteroids that have orbits in resonance with Jupiter. To highlight the motion we rotate the view at the same speed as an idealized version of Jupiter, that is, we keep the rotation constant as if the planet was on a circular orbit. The first group highlighted is in the 3:2 resonance, Objects in this group complete 3 orbits in the time that Jupiter takes to complete 2. The periodic interaction with Jupiter's gravity creates the 3 lobed pattern you see where they never come close to the giant planet. This makes their orbits more stable by protecting them from strong interactions with the planet. The second group consists of those which have orbital periods identical to Jupiter, these are primarily found in 2 clusters around the Jovian Lagrange points. These points are 60 degrees ahead and behind Jupiter in its orbit. There are many other mean-motion resonances that influence the dynamics of the asteroid belt, some are very unstable, for example there are almost no asteroids in the 3:1 resonance, also known as the Kirkwood gap. Asteroids which are in this resonance have their orbital eccentricities increase quickly until their orbits cross those of other planets and they suffer a close encounter.
Views: 45790 Scott Manley
Calculating the Gravitational Force
Answer = 126 N 045 - Calculating the Gravitational Force In this video Paul Andersen explains why astronauts are weightless. He also explains how Newton's Universal Law of Gravitation can be used to calculate the gravitational force between objects. Do you speak another language? Help me translate my videos: http://www.bozemanscience.com/translations/ Music Attribution Title: String Theory Artist: Herman Jolly http://sunsetvalley.bandcamp.com/track/string-theory All of the images are licensed under creative commons and public domain licensing: Evans, NASA/Apollo 17 crew; taken by either Harrison Schmitt or Ron.Deutsch: „Blue Marble“, Die Während Des Fluges von Apollo 17 Zum Mond Am 7. Dezember 1972 Entstandene Fotoaufnahme von Der Erde (in Der Zur Besseren Wiedererkennbarkeit Um 180 Grad Gedrehten Version).English: ”The Blue Marble“ Is a Famous Photograph of the Earth Taken on December 7, 1972, by the Crew of the Apollo 17 Spacecraft En Route to the Moon at a Distance of about 29,000 Kilometers (18,000 Statute Miles). It Shows Africa, Antarctica, and the Arabian Peninsula.Español: ”La Canica Azul". Imagen de La Tierra Tomada Desde El Apollo 17.Français : «La Bille Bleue» : Photo de l’Afrique, de l’Antarctique et de La Péninsule Arabique Prise En Route Pour La Lune Par Harrison Schmitt Ou Ron Evans Lors de La Mission Apollo 17 Le 7 Décembre 1972. Ce Vol a Été Le Dernier À Quitter L’orbite Terrestre, et Le Seul Au Cours Duquel Un Géologue, Harrison Schmitt, S’est Rendu Sur La lune.Italiano: Famosa Fotografia Della Terra Ripresa Il 7 Dicembre 1972 Dall’equipaggio Della Missione Apollo 17 Diretta Verso La Luna, Da Una Distanza Di circa 29.000 km.Македонски: „Сината Џамлија“ Е Позната Фотографија На Земјата Направена На 7 Декември 1972 Од Екипажот На Вселенското Летало Аполо 17 Патувајќи Кон Месечината. Сликана Е На Растојание Од 29.000 Километри, А На Неа Се Гледаат Африка, Антарктикот И Арапскиот Полуостров.Português: A Bolinha Azul É Uma Fotografia Famosa Da Terra Tirada a 7 de Dezembro de 1972 Durante a Missão Apollo 17, Quando Se Encontrava a Caminho Da Lua E a 29,000 Quilómetros Da Terra.Русский: Вид Земли С Космического Корабля Аполлон-17. 7 Декабря 1972 года.Українська: Блакитна Іграшкова Куля — Відома Фотографія Землі, Зроблена 7 Грудня 1972 Року Командою Космічного Апарату Čeština: Modrá Skleněnka Je Fotografie Planety Země, Kterou 7. Prosince 1972 Pořídila Posádka Apolla 17 Ze Vzdálenosti Zhruba 45 000 Kilometrů., December 7, 1972. http://www.nasa.gov/images/content/115334main_image_feature_329_ys_full.jpg Alt: http://grin.hq.nasa.gov/ABSTRACTS/GPN-2000-001138.html (direct link). http://commons.wikimedia.org/wiki/File:The_Earth_seen_from_Apollo_17.jpg. “Gravity Force Lab.” PhET. Accessed August 25, 2014. http://phet.colorado.edu/en/simulation/gravity-force-lab. Inductiveload. English: Icon for an Earth Emblem, in the Tango Icon Theme Style., December 6, 2010. Own work. http://commons.wikimedia.org/wiki/File:Emblem-earth.svg. “Moon.” Wikipedia, the Free Encyclopedia, August 25, 2014. http://en.wikipedia.org/w/index.php?title=Moon&oldid=621902801. NASA. English: NASA Astronaut Garrett Reisman, STS-132 Mission Specialist, Takes Advantage of the Weightless Environment on the Middeck of the Earth-Orbiting Space Shuttle Atlantis to Get Creative with His Posture during Flight Day 2 Activities. Photo Credit: National Aeronautics and Space Administration, May 15, 2010. http://spaceflight.nasa.gov/gallery/images/shuttle/sts-132/hires/s132e007185.jpg. http://commons.wikimedia.org/wiki/File:STS132_FD2_Garrett_Reisman_in_middeck.jpg. “Newton’s Law of Universal Gravitation.” Wikipedia, the Free Encyclopedia, August 25, 2014. http://en.wikipedia.org/w/index.php?title=Newton%27s_law_of_universal_gravitation&oldid=622565483.
Views: 202050 Bozeman Science
Saturn's Moon: Rhea Rotation
Rhea is the second-largest moon of Saturn and the ninth largest moon in the Solar System. It was discovered in 1672 by Giovanni Domenico Cassini. Rhea is named after the Titan Rhea of Greek mythology, "mother of the gods". It is also designated Saturn V. Cassini named the four moons he discovered (Tethys, Dione, Rhea and Iapetus) Sidera Lodoicea (the stars of Louis) to honor King Louis XIV. Astronomers fell into the habit of referring to them and Titan as Saturn I through Saturn V. Once Mimas and Enceladus were discovered, in 1789, the numbering scheme was extended to Saturn VII. The names of all seven satellites of Saturn then known come from John Herschel (son of William Herschel, discoverer of the planet Uranus, and two other Saturnian moons, Mimas and Enceladus) in his 1847 publication Results of Astronomical Observations made at the Cape of Good Hope, wherein he suggested the names of the Titans, sisters and brothers of Cronos (Saturn, in Roman Mythology), be used. Rhea is an icy body with a density of about 1.233 g/cm³. This low density indicates that it is made of ~25% rock (density ~3.25 g/cm³) and ~75% water ice (density ~0.93 g/cm³). While Rhea is the ninth largest moon, it is only the tenth most massive moon. Earlier it was assumed that Rhea had a rocky core in the center. However measurements taken during a close flyby by the Cassini orbiter (see below) determined the axial moment of inertia coefficient as 0.4 kg·m². Such a value indicates that Rhea has almost homogeneous interior (with some compression of ice in the center) while the existence of a rocky core would imply a moment of inertia of about 0.34. The triaxial shape of Rhea is also consistent with a homogeneous body in hydrostatic equilibrium. Rhea's features resemble those of Dione, with dissimilar leading and trailing hemispheres, suggesting similar composition and histories. The temperature on Rhea is 99 K (−174°C) in direct sunlight and between 73 K (−200°C) and 53 K (−220°C) in the shade. Rhea is covered with craters, including several large impact basins such as Tirawa. It also has bright wispy markings on its surface. Its surface can be divided into two geologically different areas based on crater density; the first area contains craters which are larger than 40 km in diameter, whereas the second area, in parts of the polar and equatorial regions, has only craters under that size. This suggests that a major resurfacing event occurred some time during its formation. The leading hemisphere is heavily cratered and uniformly bright, On the trailing hemisphere there is a network of bright swaths on a dark background and few visible craters. Discovered by G. D. Cassini Discovery date December 23, 1672 Designations Alternate name Saturn V Adjective Rhean Orbital characteristics Semi-major axis 527 108 km Eccentricity 0.001 258 3 Orbital period 4.518 212 d Inclination 0.345° (to Saturn's equator) Satellite of Saturn Physical characteristics Dimensions 1535.2 × 1525 × 1526.4 km Mean radius 764.30 ± 1.10 km Surface area 7 337 000 km² Mass (2.306 518 ± 0.000 353) × 1021 kg (~3.9 × 10−4 Earths) Mean density 1.233 3 ± 0.005 3 g/cm³ Equatorial surface gravity 0.264 m/s² Escape velocity 0.635 km/s Rotation period 4.518 212 d (synchronous) Axial tilt zero Albedo 0.949 ± 0.003 (geometric) Surface temp. Kelvin: min (53K), max (99K) Apparent magnitude 10
Views: 3801 Kurdistan Planetarium
Getting to Mars: The Hohmann Transfer
How long does it take to get to Mars? What Delta-Vs are required? When should you launch and why is a one way trip easier than a return mission? Mars One Astronaut Candidate Ryan MacDonald explains the Hohmann Transfer orbit. *Part 1 (Orbital Mechanics 101): https://www.youtube.com/watch?v=VGcQhgkXPx0
Views: 37471 Martian Colonist
Gravity, Universal Gravitation Constant - Gravitational Force Between Earth, Moon & Sun, Physics
This physics video tutorial explains how to calculate the force of gravity between two objects as well as the distance between those objects. In addition, this video explains how to calculate the net gravitational force on the moon exerted by the sun and moon. The universal gravitation constant is 6.67 x 10^-11. This video contains plenty of examples and practice problems. New Physics Video Playlist: https://www.youtube.com/playlist?list=PL0o_zxa4K1BU6wPPLDsoTj1_wEf0LSNeR Access to Premium Videos: https://www.patreon.com/MathScienceTutor https://www.facebook.com/MathScienceTutoring/
Saturn's Moon: Phoebe Rotation
Phoebe is an irregular satellite of Saturn. It was discovered by William Henry Pickering on 17 March 1899 from photographic plates that had been taken starting on 16 August 1898 at Arequipa, Peru by DeLisle Stewart. It was the first satellite to be discovered photographically. Phoebe was the first target encountered upon the arrival of CassiniHuygens to the Saturn system in 2004, and is thus unusually well-studied for a natural satellite of its size. Cassini's trajectory to Saturn and time of arrival were specifically chosen to permit this flyby. After the encounter and its insertion orbit, Cassini would not go much beyond the orbit of Iapetus. The moon is named after Phoebe, a Titan in Greek mythology. It is also designated Saturn IX. The IAU nomenclature standards have stated that features on Phoebe are to be named after characters in the Greek myth of Jason and the Argonauts. In 2005, the IAU officially named 24 craters (Acastus, Admetus, Amphion, Butes, Calais, Canthus, Clytius, Erginus, Euphemus, Eurydamas, Eurytion, Eurytus, Hylas, Idmon, Iphitus, Jason, Mopsus, Nauplius, Oileus, Peleus, Phlias, Talaus, Telamon, and Zetes). Dr. Toby Owen of the University of Hawaii at Manoa, chairman of the International Astronomical Union Outer Solar System Task Group said: "We picked the legend of the Argonauts for Phoebe as it has some resonance with the exploration of the Saturn system by Cassini-Huygens. We can't say that our participating scientists include heroes like Hercules and Atalanta, but they do represent a wide, international spectrum of outstanding people who were willing to take the risk of joining this voyage to a distant realm in hopes of bringing back a grand prize." For more than 100 years, Phoebe was Saturn's outermost known moon, until the discovery of several smaller moons in 2000. Phoebe is almost 4 times more distant from Saturn than its nearest major neighbor (Iapetus), and is substantially larger than any of the other moons orbiting planets at comparable distances. All of Saturn's moons up to Iapetus orbit very nearly in the plane of Saturn's equator. The outer irregular satellites follow fairly to highly eccentric orbits, and none is expected to rotate synchronously as all the inner moons of Saturn do (except for Hyperion). See Saturn's satellites families. Phoebe is roughly spherical and has a diameter of 220 kilometres (140 mi), which is equal to about one-fifteenth of the diameter of Earth's moon. Phoebe rotates on its axis every nine hours and it completes a full orbit around Saturn in about 18 months. Its surface temperature is 75 K (-198°C). Most of Saturn's inner moons have very bright surfaces, but Phoebe's albedo is very low (0.06), as dark as lampblack. The Phoebean surface is extremely heavily scarred, with craters up to 80 kilometres across, one of which has walls 16 kilometres high. Phoebe's dark coloring initially led to scientists surmising that it was a captured asteroid, as it resembled the common class of dark carbonaceous asteroids. These are chemically very primitive and are thought to be composed of original solids that condensed out of the solar nebula with little modification since then. However, images from the Cassini-Huygens space probe indicate that Phoebe's craters show a considerable variation in brightness, which indicate the presence of large quantities of ice below a relatively thin blanket of dark surface deposits some 300 to 500 metres (980 to 1,600 ft) thick. In addition, quantities of carbon dioxide have been detected on the surface, a finding which has never been replicated on an asteroid. It is estimated that Phoebe is about 50% rock, as opposed to the 35% or so that typifies Saturn's inner moons. For these reasons, scientists are coming to believe that Phoebe is in fact a captured Centaur, one of a number of icy planetoids from the Kuiper belt that orbit the Sun between Jupiter and Neptune. Phoebe is the first such object to be imaged as. Discovered by W.H. Pickering Discovery date 17 March 1899 / 16 August 1898 Designations Alternate name Saturn IX Adjective Phoebean Orbital characteristics Semi-major axis 12 955 759 km Eccentricity 0.156 241 5 Orbital period 550.564 636 d Inclination 173.04° (to the ecliptic) 151.78° (to Saturn's equator) Satellite of Saturn Physical characteristics Dimensions 230 x 220 x 210 km Mean radius 106.60 ± 1.00 km Mass (0.829 2 ± 0.001 0) × 1019 kg Mean density 1.634 2 ± 0.046 0 g/cm³ Equatorial surface gravity ~0.049 m/s2 Escape velocity ~0.10 km/s Sidereal rotation period 0.386 75 d (9 h 16 min 55.2 s) Axial tilt 152.14° Albedo 0.06
Views: 5691 Kurdistan Planetarium
Elliptical Orbits and the Conservation of Angular Momentum
An introduction into elliptical orbits and the conservation of angular momentum. This is at the AP Physics level or the introductory college level physics level.
Views: 45068 lasseviren1
Solar System Orbit Video
Solar System Orbit Video Solar System orbit video with the orbit periods of all 8 planets correct in respect to each other. This Solar System video shows how each of the planets orbit the Sun in the same anti-clockwise direction, with the inner rocky planets orbiting much faster than the outer gas giant planets. The rotation period (and direction) for each of the Solar System planets is also shown accurately in terms of their relative rotations speeds to each other. Their are 8 planets in the Solar System, and 5 dwarf planets; Solar System Planets (in order of distance from the Sun) Mercury 0.55 Earth Mass 0.40 Astronomical Units (AU) from the Sun (Earth = 1 AU) Venus 0.81 Earth Mass 0.70 AU from the Sun Earth 1.0 Earth Mass 1.0 AU from the Sun Mars 0. Earth Mass 1.5 AU from the Sun Jupiter 318 Earth Mass 5.2 AU from the Sun Saturn 95 Earth Mass 9.5 AU from the Sun Uranus 14 Earth Mass 19.2 AU from the Sun Neptune 17 Earth Mass 30.1 AU from the Sun All of the planets in the Solar System orbit the Sun in the same approximate plane, though they each have a slight inclination from the Sun's equator. This inclination ranges from 3 to 7.1 degrees. The Solar System is thought to have condensed from a rotating cloud of gas and dust. Most likely the remnants of a previously exploded star. The rotating gas and dust slowing began to clump together under the influence of gravity. Eventually the body at the center of the cloud gained enough mass to become sufficiently hot and dense for thermonuclear fusion to begin, and our Sun was born. The planets went on to be formed from the remains of the gas cloud which formed into a flattened disk. As with the Sun, gravity's influence caused larger and larger bodies to come together, eventually forming the 8 planets and hundreds of moons and other bodies that habit the Solar System today. This video does not show the dwarf planets, though they will be included in a future video. There are 5 recognised dwarf planets in the Solar System. Dwarf Planets (In order of distance from the Sun) Ceres (located in the Asteroid belt) - 4.6 year orbital period Pluto (located in the Kuiper belt) - 248 year orbital period Haumea (located in the Kuiper belt - 283 year orbital period Makemake (located in the Kuiper belt) - 309 year orbital period Eris (located in the scattered disk) - 557 year orbital period To see more Solar System and space videos, subscribe to my channel, Solar System Videos. Pluto
Views: 438382 SolarSystemVideos
Calculate Mass of Sun Using Data on Earth's Orbit
This video shows how to calculate the mass of the Sun if the radius of the Earth's orbit and the time for one orbit is known. The force of gravity provides the centripetal force. For the purpose of this approximate calculation it is assumed that the Earth's orbit is a circle. Introductory General Physics I Prof. Greg Clements
Views: 10200 Greg Clements
Neptune's Orbit and Rotation
... http://www.telescopefeed.com/ Neptune's 165-year-long Orbit and 16 hour rotation. Source: http://hubblesite.org/newscenter/archive/releases/2011/19/
Views: 8366 TelescopeFeed
Saturn's Moon: Iapetus Rotation
Iapetus (pronounced /aɪˈæpɨtəs/, or as Greek Ιαπετός), occasionally Japetus (pronounced /ˈdʒæpɨtəs/), is the third-largest moon of Saturn, and eleventh in the solar system, Iapetus is best known for its dramatic 'two-tone' coloration, but recent discoveries by the Cassini mission have revealed several other unusual physical characteristics, such as an equatorial ridge that runs about halfway around the moon. Iapetus was discovered by Giovanni Domenico Cassini, an Italian/French astronomer, in October 1671. He had discovered the moon on the western side of Saturn and tried viewing it on the eastern side some months later, but was unsuccessful. The pattern continued the following year as he was able to observe it on the western side, but not the eastern side. Cassini finally observed Iapetus on the eastern side in 1705 with the help of an improved telescope, finding it two magnitudes dimmer on that side. Cassini correctly surmised that Iapetus has a bright hemisphere and a dark hemisphere, and that it is tidally locked, always keeping the same face towards Saturn. This means that the bright hemisphere is visible from Earth when Iapetus is on the western side of Saturn, and that the dark hemisphere is visible when Iapetus is on the eastern side. The dark hemisphere was later named Cassini Regio in his honour. Iapetus is named after the Titan Iapetus from Greek mythology. In fact, all Saturnian moons are named after Titans. The name was suggested by John Herschel (son of William Herschel, discoverer of Mimas and Enceladus) in his 1847 publication Results of Astronomical Observations made at the Cape of Good Hope, in which he advocated naming the moons of Saturn after the Titans, sisters and brothers of the Titan Cronus (whom the Romans equated with their god Saturn). When first discovered, Iapetus was among four Saturnian moons labelled the Sidera Lodoicea by their discoverer Giovanni Cassini after King Louis XIV (the other three were Tethys, Dione and Rhea). However, astronomers fell into the habit of referring to them using Roman numerals, with Iapetus being Saturn V. Once Mimas and Enceladus were discovered in 1789, the numbering scheme was extended and Iapetus became Saturn VII. And with the discovery of Hyperion in 1848, Iapetus became Saturn VIII, which it is still known by today (see naming of natural satellites). Geological features on Iapetus are named after characters and places from the French epic poem The Song of Roland. Examples of names used include the craters Charlemagne and Baligant, and the northern bright region, Roncevaux Terra. The one exception is Cassini Regio, the dark region of the moon, named after the region's discoverer, Giovanni Cassini. The low density of Iapetus indicates that it is mostly composed of ice, with only a small (~20%) amount of rocky materials. Unlike most moons, its overall shape is neither spherical nor ellipsoid, but has a bulging waistline and squashed poles; also, its unique equatorial ridge (see below) is so high that it visibly distorts the moon's shape even when viewed from a distance. These features often lead it to be characterized as walnut-shaped. Iapetus is heavily cratered, and Cassini images have revealed large impact basins in the dark region, at least five of which are over 350 km wide. The largest, Turgis, has a diameter of 580 km; its rim is extremely steep and includes a scarp about 15 km high. Discovered by G. D. Cassini Discovery date October 25, 1671 Designations Alternate name Saturn VIII Adjective Iapetian, Japetian Orbital characteristics Semi-major axis 3 560 820 km Eccentricity 0.028 612 5 Orbital period 79.321 5 d Inclination 17.28° (to the ecliptic) 15.47° (to Saturn's equator) 8.13° (to Laplace plane) Satellite of Saturn Physical characteristics Dimensions 1494.8×1424.8 km Mean radius 735.60 ± 3 km Surface area 6 700 000 km² Mass (1.805 635 ± 0.000 375) × 1021 kg Mean density 1.083 0 ± 0.006 6 g/cm³ Equatorial surface gravity 0.223 m/s2 Escape velocity 0.572 km/s Rotation period 79.321 5 d (synchronous) Axial tilt zero Albedo 0.05-0.5 Apparent magnitude 10.2-11.9
Views: 10454 Kurdistan Planetarium
Kepler-16: A Planet Orbiting Two Stars
NASA's Kepler Mission Discovers a World Orbiting Two Stars The existence of a world with a double sunset, as portrayed in the film Star Wars more than 30 years ago, is now scientific fact. NASA's Kepler mission has made the first unambiguous detection of a circumbinary planet -- a planet orbiting two stars -- 200 light-years from Earth. Unlike Star Wars' Tatooine, Kepler-16b is cold, gaseous and not thought to harbor life, but its discovery demonstrates the diversity of planets in our galaxy. Previous research has hinted at the existence of circumbinary planets, but clear confirmation proved elusive. Kepler detected such a planet, known as Kepler-16b, by observing transits, where the brightness of a parent star dims from the planet crossing in front of it. "This discovery confirms a new class of planetary systems that could harbor life," Kepler principal investigator William Borucki said. "Given that most stars in our galaxy are part of a binary system, this means the opportunities for life are much broader than if planets form only around single stars. This milestone discovery confirms a theory that scientists have had for decades but could not prove until now." A research team led by Laurance Doyle of the SETI Institute in Mountain View, Calif., used data from the Kepler space telescope, which measures dips in the brightness of more than 150,000 stars, to search for transiting planets. Kepler is the first NASA mission capable of finding Earth-size planets in or near the "habitable zone," the region in a planetary system where liquid water can exist on the surface of the orbiting planet. Read more: http://kepler.nasa.gov/news/index.cfm?FuseAction=ShowNews&NewsID=152 Related news: First Planet Orbiting Two Stars Discovered by the NASA Kepler Spacecraft By Laurance Doyle, an astrophysicist at the SETI Institute, and lead author of a paper that will appear in the journal Science on September 15, 2011 For the first time, astronomers with the NASA Kepler spacecraft mission have discovered a planet orbiting two stars. This is a fundamentally different kind of planetary system than has ever been discovered before. The new system is known as "Kepler-16" and consists of two stars — one about 69% the mass of the Sun, and the other only 20% the mass of the Sun, which circle each other every 41 days. Around both of these circles the Saturn-mass planet, half rock and half gas, known as Kepler-16b, with a period of 229 days. Even though the planet has an orbital period of less than a year, it is still outside the habitable zone of the stars because the stars are much dimmer than our Sun. The discovery that such "circumbinary" planets can exist increases the likelihood of success of the Kepler Mission, which is to detect the first habitable; i.e. Earthlike, planets around other stars. Perhaps half the stars in the galaxy are in double star systems. Understanding that planets can form in close binary systems means that these, too, can be targets in the search for habitable worlds. The research team discovered the circumbinary planet in an eclipsing binary system. This is a double star system in which both stars orbit each other across our line of sight, so that eclipses of the stars occur with regularity. Historically, much of what we know about stars sizes comes from such eclipsing binary systems. In addition, the planet's orbit was found to lie very close to the same orbital plane -- the difference in the tilt of their orbits is less than 1/3 of a degree -- so that the planet also moves across the disc of each star, momentarily blocking some of the light. Such events are called "planetary transits" and most of what we know about the sizes of planets outside the Solar System comes from such transit events. Thus we have the best of both worlds, and Kepler-16 is probably the most accurately measured planetary system outside our own. Some scientists have nicknamed the planet "Tatooine" after the name of the home planet of Luke Skywalker, the hero in the 1970s science fiction movie Star Wars. In the story -- in a hypothetical galaxy far, far away, -- a circumbinary planet's double sunset was first brought to the screen. The public's vision of circumbinary planets thus goes back decades. But today science fiction has become science fact, and that galaxy far, far away has become our own galaxy. A whole new kind of planetary system has been shown to exist and -- like Luke in the story -- the adventure is just getting started. Source: SETI Institute http://www.seti.org/page.aspx?pid=1664 What Laurance Doyle thinks of 'Tatooine' discovery http://www.msnbc.msn.com/id/44538710/ns/technology_and_science-space/ Alien Sunset (Spitzer Space Telescope) http://www.youtube.com/watch?v=5fJeZ1um8uw Mars Movie: I'm Dreaming of a Blue Sunset http://www.youtube.com/watch?v=9B_RaySR5Pc
Views: 15781 AS N
Rare 4-planet system discovered by Kepler
For the full story, visit: http://news.berkeley.edu/2016/05/11/star-has-four-mini-neptunes-orbiting-in-lock-step/ A four-planet system observed several years ago by the Kepler spacecraft is actually a rarity: Its planets, all miniature Neptunes nestled close to the star, are orbiting in a unique resonance that has been locked in for billions of years. For every three orbits of the outermost planet, the second orbits four times, the third six times and the innermost eight times. Such orbital resonances are not uncommon – our own dwarf planet Pluto orbits the sun twice during the same period that Neptune completes three orbits – but a four-planet resonance is. Astronomers from the University of Chicago and University of California, Berkeley, who are reporting the discovery online May 11 in Nature, are particularly interested in this stellar system because our system’s four giant planets – Jupiter, Saturn, Neptune and Uranus – are thought to have once been in resonant orbits that were disrupted sometime during their 4.5-billion-year history. According to co-author Howard Isaacson, a UC Berkeley research astronomer, the Kepler-223 star system can help us understand how our solar system and other stellar systems discovered in the past few decades formed. In particular, it could help resolve the question of whether planets stay in the same place they formed, or whether they move closer to or farther from their star over the eons. Video by Roxanne Makasdjian and Stephen McNally Simulations by Daniel Fabrycky and Cezary Migazewski Music: "Candlepower" by Chris Zabriskie http://www.news.berkeley.edu/ http://www.facebook.com/UCBerkeley http://twitter.com/UCBerkeley http://instagram.com/ucberkeleyofficial https://plus.google.com/+berkeley
Views: 36214 UC Berkeley
What About a Mission to Titan? It's Time to Explore Saturn's Largest Moon
Europa is fine and all, but where we really need to go is Saturn's moon Titan. Let's look at some cool ideas for probes to fully explore this world. Support us at: http://www.patreon.com/universetoday More stories at: http://www.universetoday.com/ Follow us on Twitter: @universetoday Like us on Facebook: https://www.facebook.com/universetoday Google+ - https://plus.google.com/+universetoday/ Instagram - http://instagram.com/universetoday Team: Fraser Cain - @fcain / [email protected] Karla Thompson - @karlaii Chad Weber - [email protected] As you probably know, NASA recently announced plans to send a mission to Jupiter’s moon Europa. If all goes well, the Europa Clipper will blast off for the world in the 2020s, and orbit the icy moon to discover all its secrets. And that’s great and all, I like Europa just fine. But you know where I’d really like us to go next? Titan. Titan, as you probably know, is the largest moon orbiting Saturn. In fact, it’s the second largest moon in the Solar System after Jupiter’s Ganymede. It measures 5,190 kilometers across, almost half the diameter of the Earth. This place is big. It orbits Saturn every 15 hours and 22 days, and like many large moons in the Solar System, it’s tidally locked to its planet, always showing Saturn one side. Before NASA’s Voyager spacecraft arrived in 1980, astronomers actually thought that Titan was the biggest moon in the Solar System. But Voyager showed that it actually has a thick atmosphere, that extends well into space, making the true size of the moon hard to judge. This atmosphere is one of the most interesting features of Titan. In fact, it’s the only moon in the entire Solar System with a significant atmosphere. If you could stand on the surface, you would experience about 1.45 times the atmospheric pressure on Earth. In other words, you wouldn’t need a pressure suit to wander around the surface of Titan. You would, however, need a coat. Titan is incredibly cold, with an average temperature of almost -180 Celsius. For you Fahrenheit people that’s -292 F. The coldest ground temperature ever measured on Earth is almost -90 C, so way way colder. You would also need some way to breathe, since Titan’s atmosphere is almost entirely nitrogen, with trace amounts of methane and hydrogen. It’s thick and poisonous, but not murderous, like Venus. Titan has only been explored a couple of times, and we’ve actually only landed on it once. The first spacecraft to visit Titan was NASA’s Pioneer 11, which flew past Saturn and its moons in 1979. This flyby was followed by NASA’s Voyager 1 in 1980 and then Voyager 2 in 1981. Voyager 1 was given a special trajectory that would take it as close as possible to Titan to give us a close up view of the world. Voyager was able to measure its atmosphere, and helped scientists calculate Titan’s size and mass. It also got a hint of darker regions which would later turn out to be oceans of liquid hydrocarbons. The true age of Titan exploration began with NASA’s Cassini spacecraft, which arrived at Saturn on July 4, 2004. Cassini made its first flyby of Titan on October 26, 2004, getting to within 1,200 kilometers or 750 miles of the planet. But this was just the beginning. By the end of its mission later this year, Cassini will have made 125 flybys of Titan, mapping the world in incredible detail. Cassini saw that Titan actually has a very complicated hydrological system, but instead of liquid water, it has weather of hydrocarbons. The skies are dotted with methane clouds, which can rain and fill oceans of nearly pure methane. And we know all about this because of Cassini’s Huygen’s lander, which detached from the spacecraft and landed on the surface of Titan on January 14, 2005. Here’s an amazing timelapse that shows the view from Huygens as it passed down through the atmosphere of Titan, and landed on its surface. Huygens landed on a flat plain, surrounded by “rocks”, frozen globules of water ice. This was lucky, but the probe was also built to float if it happened to land on liquid instead. It lasted for about 90 minutes on the surface of Titan, sending data back to Earth before it went dark, wrapping up the most distant landing humanity has ever accomplished in the Solar System. Although we know quite a bit about Titan, there are still so many mysteries. The first big one is the cycle of liquid. Across Titan there are these vast oceans of liquid methane, which evaporate to create methane clouds. These rain, creating mists and even rivers. Is it volcanic? There are regions of Titan that definitely look like there have been volcanoes recently. Maybe they’re cryovolcanoes, where the tidal interactions with Saturn cause water to well up from beneath crust and erupt onto the surface.
Views: 43596 Fraser Cain
Jupiter moons Observation  + calculating their period
We propose in this project to observe on successive days the position of each of the four major moons of Jupiter: Io, Europe, Ganymede and Callisto to deduce finally their orbital periods. Materiel used: • Telescope (Celestron / CPC 800 GPS (XLT) Computerized 14” apertures) • Camera (Canon EOS 500D) •Program used: Matlab, Excel, Digitize Plot To Data Vhjlj2.2.1, PS Photoshop My GitHub account where you will find the project: https://github.com/Avedistcha/Astronomy
Planet search: Three new planets discovered orbiting around an ultracool dwarf star - TomoNews
LIEGE, BELGIUM — The search for life beyond our solar system has taken an exciting turn, after a Belgian-led team reported finding planets with the potential to host life. Fox News reports that a team of Belgian astronomers have discovered three new planets in the Aquarius constellation using the Trappist telescope at the La Silia Observatory in Chile. The planets are 40 light years away and similar in size and temperature to Earth. They orbit an ultracool dwarf star, named Trappist-1 after the telescope that discovered it. Trappist-1 is a dim, red star about a tenth the size of our Sun, and only slightly bigger than Jupiter. With a temperature of less than 2,700 Kelvin, it’s also only half as hot as our sun. All three planets could have liquid water on their surfaces and thus be potentially hospitable to life. The two closest planets complete an orbit in 1.5 and 2.4 Earth days, respectively. They receive two to four times more radiation than Earth, and may have areas that can sustain life. The third, with an orbital period ranging from four to 73 days, receives less radiation and may fall within the habitable zone, according to CTV News. Scientists are already studying the planets’ atmospheric conditions using NASA’s Spitzer Space telescope, with the Hubble Space Telescope joining in soon. ----------------------------------------­--------------------- Welcome to TomoNews, where we animate the most entertaining news on the internets. Come here for an animated look at viral headlines, US news, celebrity gossip, salacious scandals, dumb criminals and much more! Subscribe now for daily news animations that will knock your socks off. Visit our official website for all the latest, uncensored videos: http://us.tomonews.net Check out our Android app: http://bit.ly/1rddhCj Check out our iOS app: http://bit.ly/1gO3z1f Get top stories delivered to your inbox everyday: http://bit.ly/tomo-newsletter Stay connected with us here: Facebook http://www.facebook.com/TomoNewsUS Twitter @tomonewsus http://www.twitter.com/TomoNewsUS Google+ http://plus.google.com/+TomoNewsUS/ Instagram @tomonewsus http://instagram.com/tomonewsus -~-~~-~~~-~~-~- Please watch: "Crying dog breaks the internet’s heart — but this sad dog story has a happy ending" https://www.youtube.com/watch?v=4prKTN9bYQc -~-~~-~~~-~~-~-
Views: 22346 TomoNews US
Orbital and Rotational Speed of the Planets in KM and Miles Per Sec/Hour
The closer a planet is to the Sun, the faster it travels along its orbit. This video shows the orbital speed of the planets (Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune, and Pluto) around the sun as well as their equatorial rotational speed. The Big Beat 80 by Kevin MacLeod, Syrinx Starr is licensed under a Creative Commons Attribution license (https://creativecommons.org/licenses/by/4.0/) Web: http://www.manikjoshi.com Facebook: http://www.facebook.com/joshimanik
Views: 50 Manik Joshi
Extraterrestrial Superstorms | Space Time
Viewers like you help make PBS (Thank you 😃) . Support your local PBS Member Station here: https://to.pbs.org/DonateSPACE Earth has its share of monster storms, but even our most powerful hurricanes are a breeze compared to the great, planet-sized tempests of the gas giants. LegalZoom is not a law firm or a substitute for the advice of an attorney. Get 15% off your next purchase at https://www.legalzoom.com/spacetime. ... You can further support us on Patreon at https://www.patreon.com/pbsspacetime Get your own Space Time t­shirt at http://bit.ly/1QlzoBi Tweet at us! @pbsspacetime Facebook: facebook.com/pbsspacetime Email us! pbsspacetime [at] gmail [dot] com Comment on Reddit: http://www.reddit.com/r/pbsspacetime Previous Episode: The One-Electron Universe https://www.youtube.com/watch?v=9dqtW... The great vortices of the Jovian planets are true storms, analogous in many ways to Earth’s hurricanes. There are, of course, some differences. For example, these storms are as big as entire planets. The largest and oldest storm in the solar system is Jupiter’s Great Red Spot, stretching an incredible two to three times the diameter of the planet Earth. Meanwhile the fastest winds ever measured, clocking fifteen hundred miles per hour, once raged in Neptune’s Great Dark Spot. Saturn’s Polar Vortex is a 20,000-mile-wide monster shaped like a hexagon. Even plain-looking Uranus hides USA-sized hurricanes below its methane haze. There are many unsolved mysteries surrounding these epic storms. We may be close to finding some answers, following the Juno spacecraft’s recent flyby of Jupiter’s Great Red Spot. Juno's interactive website: https://www.missionjuno.swri.edu/ Written by Alexandra Yep and Matt O’Dowd Hosted by Matt O' Dowd Produced by Rusty Ward Graphics by Kurt Ross Assistant Editing and Sound Design by Mike Petrow Made by Kornhaber Brown (www.kornhaberbrown.com) Comments answer by Matt: Andres64 https://www.youtube.com/watch?v=9dqtW... Keith Gaughan https://www.youtube.com/watch?v=9dqtW... Vacuum Diagrams https://www.youtube.com/watch?v=9dqtW... youteub akount https://www.youtube.com/watch?v=9dqtW... Don Solaris https://www.youtube.com/watch?v=9dqtW... Special thanks to our Patreon Big Bang, Quasar and Hypernova Supporters: Big Bang CoolAsCats David Nicklas Quasar Tambe Barsbay Max Levine Mayank M. Mehrota Mars Yentur Mark Rosenthal Dean Fuqua Hypernova Eugene Lawson Chuck Zegar Jordan Young Ratfeast John Hofmann Joseph Salomone Martha Hunt Craig Peterson Science Via Markets Barry Hatfield Thanks to our Patreon Gamma Ray Burst Supporters: Peter Durocher Michael Kers Chris Hicks Mark Vasile Patrick Murray Sultan Alkhulaifi Alex Seto Jared Moore Michal-Peanut Karmi Bernardo Higuera Erik Stein Daniel Lyons Kevin Warne JJ Bagnell J Rejc Amy Jie Avi Goldfinger John Pettit Shannan Catalano Florian Stinglmayr Yubo Du Benoit Pagé-Guitard Nathan Leniz Jessica Fraley Loro Lukic Brandon Labonte David Crane Greg Weiss
Views: 373103 PBS Space Time
How Long Does It Take For The Earth To Orbit The Sun?
Museum how long does the earth take to go around sun and what causes seasons url? Q webcache. How long does it take for the earth to go around sun? Youtubehow sun orbit galaxy? At what speed move (beginner how milky way's center? . Error loading player no playable sources found astronomers use the word constellation to describe a. 25 days to complete one revolution around the sun. Sun and earth how long does the earth take to go around sun what causes maas. The radius of this orbit is 150 million km (which is, course, the distance to sun. Some define it as the time takes for a point on earth to be facing sun at given angle (for ins 15 aug 2010. What is the rotation of earth? Universe todayhow long a year on saturn? mercury? how does it take saturn to go around sun? How earth complete one revolution day? Australians surveyed for 1 chapter. An entire region of the sky and all objects in that How long does earth take to go around sun what causeshow many days it for orbit sun? Quora. With an average orbital speed of 9. Saturn travels at an average speed of 21,637 miles 18 dec 2015 we use the word year to describe duration a complete orbit earth around sun. Earth's orbit is the trajectory along which earth travels around sun. 25 days long, but there are 1 dec 2009 how long does it take the earth to spin once on its axis? The plane of the earth's orbit around the sun and the earth's orbit was a perfect circle australians surveyed how long does it take for the earth to go around the sun? Prev random video next. 256 days (1 sidereal year), during which time earth by most predictions, earth's orbit will be relatively stable over long periods 22 jul 2009 the moon orbits the earth, the earth orbits the sun, and the sun orbits the milky way how long does it take this celestial dance to complete? . 28 feb 2016 short version earth's average orbital speed is about 30 kilometers per second. How many days does it take for the earth to make one revolution of sun? Answer takes 365 revolve around sun. 96 million mi), and one complete orbit takes 365. Earth years, or once every 10,755. How long does the earth take to go around sun and what causeshow many days it for orbit sun? Quora. 15 sep 2010 a recent survey on science literacy conducted on behalf of the federation of australian scientistic and technological societies (fasts) and the australian academy of science found that only 61. 69 km s, it takes saturn 29. 457 earth years (or saturn has a lot to do with its considerable distance from the sun 15 feb 2017 to break it down, mercury takes roughly 88 earth days to complete a single mercury orbits the sun at a distance of 57,909,050 km (35,983,015 mi), which not only do temperatures on its surface range from molten hot to saturn revolves or orbits around the sun once every 29. Astronomy essentials how long does it take the earth to complete an orbit around sun for sun? The takes 365 days revolve cccoe. This is known as 25 mar 2016 then there's how long it takes
Views: 681 Sea of Question
How Long Is One Rotation Of Neptune?
Planets closer to the sun complete their orbits faster than planets farther away. 32 degrees wow i'm really surprised!!! the diagram above shows you more about find out information about the planet neptune, the eighth and farthest planet from the sun in the solar system. How long is a day on neptune? one other planets? Nasa space placeorbit & rotation of neptune planet 's year, wikipedia. Because its axial tilt is comparable to earth's, the variation in length of day over course long year not any more extreme 12 sep 2017. Neptune is farther out than mars. Which planet takes longer to orbit the sun mars or neptune. One season on neptune lasts for mercury is the planet with shortest period of revolution approximately 88 earth days. Revolution period (length of year in earth days), 60,190 (164. Earth takes 24 hours to complete one spin, and mars 25. How long is a day on neptune? Universe today. Html "imx0m" url? Q webcache. Neptune moves around the sun in an elliptical or oval shaped orbit; Its orbit period earth years is 163. Googleusercontent search. And the south polar feature, are locked to planet s rotation, which allowed karkoschka precisely determine how long a day lasts on neptune. The amount of time it takes one planet to make a full orbit around the sun is considered year. Neptune's rotation period as it spins on its axis, in earth hours, is 16. 934 hours on mercury a day lasts 1,408 hours, and on venus it lasts 5,832 hours. It is one of the largest improvements in determining rotational period a gas planet almost 350 years ever since 14 jul 2011 honor occasion, people who run hubble space telescope have taken set four anniversary photos big blue planet, every hours or so to capture full rotation (neptune's year may be much longer than ours, but its day lasts only 16 hours). Also, since neptune is not a solid body, its atmosphere also goes under differential rotation. It's now early winter in neptune's triton takes 5. Unlike their rocky counterparts, gas giants have long challenged astronomers when it comes to calculating rotation 27 nov 2008 a day on neptune is 16 hours, 6 minutes and 36 seconds. Its sidereal rotation period (day) is roughly 16. A day on neptune is just 16 hours long space 13229 length calculated. A planet s period of revolution is the time it takes for one complete spin around sun. 26 days rotation on its axis. Here on earth, one year equals 365. Orbit inclination (degrees), 1. Obliquity (tilt of axis degrees), 29. Oct 2011 not long after neptune completed its first orbit around the sun since discovery in 1846, scientists have managed to calculate exact length of one day on distant gas giant planet. Neptune lies about 30 times as far from the sun planets in solar system orbit around on fixed pathways. A day on neptune is about 16 earth hours while a 23. 11 hours, compared to our 24 hour rotation periods. The planet neptune rotation, revolution, distance, composition measuring neptune's spin space birthday makes 165 year
Views: 117 Aile Aile
Sound of Saturn  and Titan Embraced Time Periods (Binaural Beats Meditation )
(Volume maybe needed to be brought down from max level due to distortion) This is the sound of the Time periods of Planet Saturn embraced with moon Titan in our solar system by a binaural beats transformation. Saturn time period = 10759 Earth days Titan time period = 15.945 Earth days From formula f = 1/T frequency = reciprocal of Timeperiod frequency of Saturn = 1/(10759days*24hrs*60min*60sec) in cycles per second =0.000000001075757419 Hz This frequency is far too low for us to hear so we doubled it again and again 31 times octaved audio frequency of Saturn = (2^31)*0.000000001075757419 Hz =2.3101715 Hz To get Titan octaved audio frequency, 2.3101715Hz*(10759days/15.945days) = 1558.8043 Hz We use a Dual embracing formula of these two frequencies of 2.3101715 Hz & 1558.8043 Hz to generate a transformed Binaural sound presented here in this Session. The sound session provided is not meant to replace or substitute the recommendations or advice of your physician or health care provider. This video should not be used for diagnosing or treating a health problem or disease. If you believe you have a medical condition or problem contact your health care provider.
Giant, waterlogged hot Saturn hints at breadth of exoplanet diversity
Giant, waterlogged hot Saturn hints at breadth of exoplanet diversity Water is not only a key ingredient in supporting life, it's also a major clue as to how planets form, and NASA has found a lot of the stuff in the atmosphere of a giant exoplanet called Wasp-39b. The planet is as massive as Saturn but has three times as much water as the famous ringed planet. Although this "hot Saturn" is far from habitable, it does provide insights into the wide variety of planets in the universe. Located 700 light years from Earth in the constellation of Virgo, Wasp-39b is not what one would call a garden spot. Its mass is only 0.28 that of Jupiter, but it's radius is 1.27 greater than the largest planet in our solar system. It's also 20 times closer to its star, Wasp-39, than the Earth is to the Sun, which it orbits once every four days. The planet is tidally locked with one side always facing its parent star, with a dayside temperature of a scorching 1,430° F (776.7° C). Powerful winds circulate this heat from the day to the night side, which means both hemispheres are just as hot. In addition, it probably lacks Saturn's characteristic rings. But it's the amount of water on Wasp-39b that interests a team of scientists led by Hannah Wakeford of the Space Telescope Science Institute in Baltimore, and the University of Exeter. They were confident that traces of water would be found on the exoplanet as such signs have been found in the gas giants of the Solar System, but finding three times as much was a surprise – and a very informative one at that.
Views: 694 Aban Tech
Finding Another Earth Within Reach
From EsoCast. Planet hunters unveil the tricks of the trade for finding planets around nearby stars and scanning them for signs of life. Are we alone? It's the biggest question ever. And the answer is almost within reach. With so many galaxies, and each with so many stars, how could the Earth be unique? In 1995, Swiss astronomers Michel Mayor and Didier Queloz were the first to discover an exoplanet orbiting a normal star. Since then, planet hunters have found many hundreds of alien worlds. Large and small, hot and cold, and in a wide variety of orbits. Now, we're on the brink of discovering Earth's twin sisters. And in the future: a planet with life -- the Holy Grail of astrobiologists. Michel Mayor's team found hundreds of them from Cerro La Silla, ESO's first Chilean foothold. Here's the CORALIE spectrograph, mounted on the Swiss Leonhard Euler Telescope. It measures the tiny wobbles of stars, caused by the gravity of orbiting planets. ESO's venerable 3.6-metre telescope is also hunting for exoplanets. The HARPS spectrograph is the most accurate in the world. So far, it has discovered more than 150 planets. Its biggest trophy: a rich system containing at least five and maybe as many as seven alien worlds. But there are other ways to find exoplanets. In 2006, the 1.5-metre Danish telescope helped to discover a distant planet that is just five times more massive than the Earth. The trick? Gravitational microlensing.?The planet and its parent star passed in front of a brighter star in the background, magnifying its image. And in some cases, you can even capture exoplanets on camera. In 2004 NACO, the adaptive optics camera on the Very Large Telescope took the first image ever of an exoplanet. The red dot in this image is a giant planet orbiting a brown dwarf star. In 2010, NACO went one step further. This star is 130 light-years away from Earth.? It is younger and brighter than the Sun, and four planets circle around it in wide orbits. NACO's eagle-eyed vision made it possible to measure the light of planet c — a gas giant ten times more massive than Jupiter. Despite the glare of the parent star, the feeble light of the planet could be stretched out into a spectrum, revealing details about the atmosphere. Today, many exoplanets are discovered when they transit across their parent stars. If we happen to see the planet's orbit edge-on, it will pass in front of its star every cycle. Thus, tiny, regular brightness dips in the light of a star betray the existence of an orbiting planet. The TRAPPIST telescope at La Silla will help search for these elusive transits. Meanwhile, the Very Large Telescope has studied a transiting planet in exquisite detail. Meet GJ1214b, a super-Earth 2.6 times larger than our home planet. During transits, the planet's atmosphere partly absorbs the light of the parent star. ESO's sensitive FORS spectrograph revealed that GJ1214b might well be a hot and steamy sauna world. Gas giants and sauna worlds are inhospitable to life. But the hunt is not over yet. Soon, the new SPHERE instrument will be installed at the VLT. SPHERE will be able to spot faint planets in the glare of their host stars. In 2016, the ESPRESSO spectrograph will arrive at the VLT and greatly surpass the current HARPS instrument. And ESO's Extremely Large Telescope, once completed, may well find evidence for alien biospheres. On Earth, life is abundant. Northern Chile offers its share of condors, vicuñas, vizcachas and giant cacti. Even the arid soil of the Atacama desert teems with hardy microbes. We've found the building blocks of life in interstellar space. We've learnt that planets are abundant. Billions of years ago, comets brought water and organic molecules to Earth. Wouldn't we expect the same thing to happen elsewhere?
Views: 107779 SpaceRip
Calculation With Kepler's Third Law
How to calculate either the semimajor axis or the orbital period using Kepler's third law. The period is measured in years and the semimajor axis is in astronomical units.
Views: 11288 Jim Hamm
Why Doesn’t Earth Have Rings? And Why Rings Would Be Very Bad
You'd think Saturn has all the luck, with its awesome rings. But it turns out, living on a planet with rings has consequences, like an impending global apocalypse. Support us at: http://www.patreon.com/universetoday More stories at: http://www.universetoday.com/ Follow us on Twitter: @universetoday Like us on Facebook: https://www.facebook.com/universetoday Google+ - https://plus.google.com/+universetoday/ Instagram - http://instagram.com/universetoday Team: Fraser Cain - @fcain / [email protected] Karla Thompson - @karlaii Chad Weber - [email protected] Before we really get started on today’s episode, I’d like to share a bunch of really cool pictures created by my friend Kevin Gill. Kevin’s a computer programmer, 3-D animator and works on climate science data for NASA. And in his spare time, he uses his skills to help him imagine what the Universe could look like. For example, he’s mapped out what a future terraformed Mars might look like based on elevation maps, or rendered moons disturbing Saturn’s rings with their gravity. But one of my favorite sets of images that Kevin did were these. What would it look like if Earth had rings? Kevin and his wife went to a few cool locations, took some landscape pictures, and then Kevin did the calculations for what it would look like if Earth had a set of rings like Saturn. And let me tell you, Earth would be so much better. At least you’d think so, but actually, it might also suck. Last time I checked, we don’t have rings like this. In fact, we don’t have any rings at all. Why not? Considering the fact that Saturn, Jupiter, Uranus and Neptune all have rings, don’t we deserve at least something? Did we ever have rings in the past, or will we in the future? What’s it going to take for us to join the ring club? Short answer, an apocalypse. Before we get into the inevitable discussion of death and devastation, let’s talk a bit about rings. Saturn is the big showboat, with its fancy rings. They’re made of water ice, with chunks as big as a mountain, or as small as a piece of sand. Astronomers have been arguing about where they came from and how old they are, but the current consensus - sortof - is that the rings are almost as ancient as Saturn itself: billions of years old. And yet, some process is weathering the rings, grinding the particles so they appear much younger. Jupiter’s rings are much fainter, and we didn’t even know about them until 1979, when the Voyager spacecraft made their flybys. The rings seem to be created by dust blown off into space by impacts on the planet’s moons. Hey, we’ve got a moon, that’s a sign. The rings around Uranus are bigger and more complex than Jupiter’s rings, but not as substantial as Saturn’s. They’re much younger, perhaps only 600 million years old, and appear to have been caused by two moons crashing into each other, long ago. Again, another sign. We still have the potential for stuff to crash around us. The rings around Neptune are far dustier than any of the other ring systems, and much younger than the Solar System. And like the rings around Uranus, they were probably formed when two or more of its moons collided together. Now what about our own prospects for rings? The problem with icy rings is that the Earth orbits too closely to the Sun. There’s a specific point in the Solar System known as the “frost line” or “snow line”. This is the point in the Solar System where deposits of ice could have survived for long periods of time. Any closer and the radiation from the Sun sublimates the ice away. This point is actually located about 5 astronomical units away from the Sun, in the asteroid belt. Mars is much closer, so it’s very dry, while Jupiter is beyond the frost line, and its moons have plenty of water ice. The Earth is a mere 1 AU from the Sun. That’s the very definition of an astronomical unit, which means it’s well within the frost line. The Earth itself can maintain water because the planet’s magnetosphere acts like a shield against the solar wind. But the Moon is bone dry (except for the permanently shadowed craters at its poles). And if there was an icy ring system around the Earth, the solar wind would have blasted it away long ago. Instead, let’s look at another kind of ring we can have. One made of rock and dust, containing death and sorrow, from a pulverized asteroid or moon. In fact, billions of years ago, we definitely had a ring when a Mars-sized planet crashed into the Earth and spewed out a massive ring of debris. This debris collected together into the Moon we know today. That impact turned the Earth’s surface inside out. It was all volcanoes, everywhere, all the time. It’s also possible we had a second moon in the ancient past, which collided with our current Moon. That would have generated an all new ring of material for millions of years until it was recaptured by the Moon, kicked out of orbit, or fell down onto the Earth.
Views: 32052 Fraser Cain
The Dragonfly Mission to Titan: Exploration of an Ocean World
Saturn’s largest moon is a high priority for exploration. Titan is an ocean world and the only moon in our solar system with a dense atmosphere, which supports an Earth-like hydrological cycle of methane clouds, rain, and liquid that flows across the surface to fill lakes and seas. The complex organic material on Titan's surface makes it an ideal destination for studying the conditions and kinds of chemical interactions that occurred before life developed on Earth. Johns Hopkins Applied Physics Laboratory space scientist and Dragonfly Principal Investigator Elizabeth “Zibi” Turtle describes the science and technology driving the mission, which could revolutionize how we explore the solar system. Dragonfly is a rotorcraft lander – proposed to NASA's New Frontiers Program – designed to take advantage of Titan's environment to sample materials and determine surface composition in different settings. This bold mission concept includes the capability to explore diverse locations to characterize the habitability of Titan's environment, to investigate how far prebiotic chemistry has progressed, and even to search for chemical signatures that could indicate water-based or hydrocarbon-based life. For more on Dragonfly, visit http://dragonfly.jhuapl.edu.
Venus: Death of a Planet
Watch this updated full res 1080p version of our classic show. Why did Earth thrive and our sister planet, Venus, died? From the fires of a sun's birth... twin planets emerged. Then their paths diverged. Nature draped one world in the greens and blues of life. While enveloping the other in acid clouds... high heat... and volcanic flows. Why did Venus take such a disastrous turn? For as long as we have gazed upon the stars, they have offered few signs... that somewhere out there... are worlds as rich and diverse as our own. Recently, though, astronomers have found ways to see into the bright lights of nearby stars. They've been discovering planets at a rapid clip... using observatories like NASA's Kepler space telescope... A French observatory known as Corot ... .And an array of ground-based instruments. The count is approaching 500... and rising. These alien worlds run the gamut... from great gas giants many times the size of our Jupiter... to rocky, charred remnants that burned when their parent star exploded. Some have wild elliptical orbits... swinging far out into space... then diving into scorching stellar winds. Still others orbit so close to their parent stars that their surfaces are likely bathed in molten rock. Amid these hostile realms, a few bear tantalizing hints of water or ice... ingredients needed to nurture life as we know it. The race to find other Earths has raised anew the ancient question... whether, out in the folds of our galaxy, planets like our own are abundant... and life commonplace? Or whether Earth is a rare Garden of Eden in a barren universe? With so little direct evidence of these other worlds to go on, we have only the stories of planets within our own solar system to gauge the chances of finding another Earth. Consider, for example, a world that has long had the look and feel of a life-bearing planet. Except for the moon, there's no brighter light in our night skies than the planet Venus... known as both the morning and the evening star. The ancient Romans named it for their goddess of beauty and love. In time, the master painters transformed this classical symbol into an erotic figure. It was a scientist, Galileo Galilei, who demystified planet Venus... charting its phases as it moved around the sun, drawing it into the ranks of the other planets. With a similar size and weight, Venus became known as Earth's sister planet. But how Earth-like is it? The Russian scientist Mikkhail Lomonosov caught a tantalizing hint in 1761. As Venus passed in front of the Sun, he witnessed a hair thin luminescence on its edge. Venus, he found, has an atmosphere. Later observations revealed a thick layer of clouds. Astronomers imagined they were made of water vapor, like those on Earth. Did they obscure stormy, wet conditions below? And did anyone, or anything, live there? NASA sent Mariner 2 to Venus in 1962... in the first-ever close planetary encounter. Its instruments showed that Venus is nothing at all like Earth. Rather, it's extremely hot, with an atmosphere made up mostly of carbon dioxide. The data showed that Venus rotates very slowly... only once every 243 Earth days... and it goes in the opposite direction. American and Soviet scientists found out just how strange Venus is when they sent a series of landers down to take direct readings. Surface temperatures are almost 900 degrees Fahrenheit, hot enough to melt lead, with the air pressure 90 times higher than at sea level on Earth. The air is so thick that it's not a gas, but a "supercritical fluid." Liquid CO2. On our planet, the only naturally occurring source is in the high-temperature, high-pressure environments of undersea volcanoes. It comes in handy for extracting caffeine from coffee beans... or drycleaning our clothes. You just wouldn't want to have to breathe it. The Soviet Venera landers sent back pictures showing that Venus is a vast garden of rock, with no water in sight. In fact, if you were to smooth out the surface of Venus, all the water in the atmosphere would be just 3 centimeters deep. Compare that to Earth... where the oceans would form a layer 3 kilometers deep. If you could land on Venus, you'd be treated to tranquil vistas and sunset skies, painted in orange hues. The winds are light, only a few miles per hour... but the air is so thick that a breeze would knock you over. Look up and you'd see fast-moving clouds... streaking around the planet at 300 kilometers per hour. These clouds form a dense high-altitude layer, from 45 to 66 kilometers above the surface. The clouds are so dense and reflective that Venus absorbs much less solar energy than Earth, even though it's 30% closer to the Sun.
Views: 2826988 SpaceRip
How Close Can Moons Orbit? Understanding the Roche Limit
The Moon is our constant companion, shining away in the night. But how close could the Moon get before it's not a Moon any more? Before it's torn apart by the Earth's gravity and becomes a terrifying ring of orbital debris? Is Phobos Doomed? Find out here: http://www.youtube.com/watch?v=BJHRyjkmxss Support us at: http://www.patreon.com/universetoday More stories at: http://www.universetoday.com/ Follow us on Twitter: @universetoday Follow us on Tumblr: http://universetoday.tumblr.com/ Like us on Facebook: https://www.facebook.com/universetoday Google+ - https://plus.google.com/+universetoday/ Instagram - http://instagram.com/universetoday Team: Fraser Cain - @fcain Jason Harmer - @jasoncharmer Chad Weber - [email protected] Created by: Fraser Cain and Jason Harmer Edited by: Chad Weber Music: Left Spine Down - “X-Ray” https://www.youtube.com/watch?v=4tcoZNrSveE The Moon is great and all, but I wish it was closer. Close enough that I could see all kinds of detail on its surface without a telescope or a pair of binoculars. Close enough that I could just reach up and grab enough cheese for a lifetime of grilled cheese sandwiches. Sure, there would be all kinds of horrible problems with having the Moon that much closer. Intense tides, a total lack of good dark nights for stargazing, and something else... Oh right, the total destruction of life on Earth. On second thought the Moon can stay right where it is, thank you very much. The Earth’s Moon is located an average distance of 384,400 kilometers away. I say average because the Moon actually follows an elliptical orbit. At its closest point, it’s only 362,600 km, and at its furthest point, it’s 405,400 kilometers. Still, that’s so far that it takes light a little over a second to reach the Moon, traveling almost 300,000 km/s. The Moon is far. But what if the Moon was much closer? How close could it get and still be the Moon? Once again, I need to remind you that this is purely theoretical. The Moon isn’t getting closer to us, in fact, it’s getting further. The Moon is slowly drifting away from us at a distance of almost 4 centimeters per year. Let’s go back to the beginning, when the young Earth collided with a Mars-sized planet billions of years ago. This catastrophic encounter completely resurfaced planet Earth, and kicked up a massive amount of debris into orbit. Well, a Moon’s worth of debris, which collected together by mutual gravity into the roughly spherical Moon we recognize today. Shortly after its formation, the Moon was much closer, and the Earth was spinning more rapidly. A day on Earth was only 6 hours long, and the Moon took just 17 days to orbit the Earth. The Earth’s gravity stopped the Moon’s relative rotation, and the Moon’s gravity has been slowing the Earth’s rotation. To maintain the overall angular momentum of the system, the Moon has been drifting away to compensate. This conservation of momentum is very important because it works both ways. As long as a moon takes longer than a day to orbit its planet, you’re going to see this same effect. The planet’s rotation slows, and the moon drifts further to compensate. But if you have a scenario where the moon orbits faster than the planet rotates, you have the exact opposite situation. The moon makes the planet rotate more quickly, and it drifts closer to compensate. This can’t end well. Once you get close enough, gravity becomes a harsh mistress. There’s a point in all gravitational interactions called the Roche Limit. This is the point at which an object held together by gravity (like the Moon), gets close enough to another celestial body that it gets torn apart. The exact point depends on the mass, size and density of the two objects. For example, the Roche Limit between the Earth and the Moon is about 9,500 kilometers, assuming the Moon is a solid ball. In other words, if the Moon gets within 9,500 kilometers or so, of the Earth, the gravity of the Earth overwhelms the gravity holding the Moon together. The Moon would be torn apart, and turned into a ring. And then the pieces of the ring would continue to orbit the Earth until they all came crashing down. When that happened, it would be a series of very bad days for anyone living on Earth. If an average comet got within about 18,000 km of Earth, it would get torn to pieces. While the Sun can, and does, tear apart comets from about 1.3 million km away. This sounds purely theoretical, but this is actually going to happen over at Mars. Its largest moon Phobos orbits more quickly than a Martian day, which means that it’s drifting closer and closer to the planet. In a few million years, it’ll cross the Roche Limit, tear into a ring, and then all the pieces of the former Phobos will crash down onto Mars. We did a whole episode on this, and we’ll link it up here and in the description.
Views: 25777 Fraser Cain
धरती जैसे दूसरे ग्रह तक का सफर||How Long Would it Take to the Nearest Habitable Planets (Rahasya Tv)
धरती जैसे दूसरे ग्रह तक का सफर || How Long Would it Take to Get to the Nearest Habitable Planets #exoplanet #kepler_452b #nearest exoplanet Kepler-452b Kepler-452b (sometimes nicknamed Earth 2.0 or Earth's Cousin based on its characteristics; known sometimes as Coruscant by NASA, also known by its Kepler Object of Interest designation KOI-7016.01) is an exoplanet orbiting the Sun-like star Kepler-452 about 1,400 light-years (430 pc) from Earth in the constellation Cygnus. It was identified by the Kepler space telescope, and its discovery was announced by NASA on 23 July 2015. However, a study in 2018 by Mullally et al. implied that statistically, Kepler-452 b has not been proven to exist and must still be considered a candidate.It is the first potentially rocky super-Earth planet discovered orbiting within the habitable zone of a star very similar to the Sun. Mass, radius, and temperature Kepler-452b has a probable mass five times that of Earth, and its surface gravity is twice Earth's, though calculations of mass for exoplanets are only rough estimates. If it is a terrestrial planet, it is most likely a super-Earth with many active volcanoes due to its higher mass and density. The clouds on the planet would be thick and misty, covering much of the surface as viewed from space. The planet takes 385 Earth days to orbit its star. Host star The host star, Kepler-452, is a G-type star that is about the same mass of the Sun, only 3.7% more massive and 11% larger. It has a surface temperature of 5757 K, nearly the same as the Sun, which has a surface temperature of 5778 K.The star's age is estimated to be about 6 billion years old, about 1.4 billion years older than the Sun, which is 4.6 billion years old. Orbit Kepler-452b orbits its host star with about 20% more of the Sun's luminosity (1.2 L☉) with an orbital period of 385 days and an orbital radius of about 1.04 AU, nearly the same as Earth's (1 AU). Kepler Space Telescope: Exoplanet Hunter NASA's Kepler Space Telescope is an observatory in space dedicated to finding planets outside our solar system, particularly alien planets that are around the same size as Earth in the "habitable" regions of their parent star. In March 2018, NASA announced that Kepler is running low on fuel and is expected to cease operations within several months. Since the launch of the observatory in 2009, astronomers have discovered thousands of extra-solar planets, or exoplanets, through this telescope alone. Voyager 1 Voyager 1 is a space probe launched by NASA on September 5, 1977. Part of the Voyager program to study the outer Solar System, Voyager 1 launched 16 days after its twin, Voyager 2. Having operated for 40 years, 8 months and 25 days as of May 30, 2018, the spacecraft still communicates with the Deep Space Network to receive routine commands and return data. ☀ ☀ ☀ Please shop anything with these affiliate link, this can help us a lot ☀ ☀ ☀ My Gear ******** Blue Microphones Snowball-GB USB Microphone http://amzn.to/2k7DpVU Asus R-Series R558UQ-DM539D 15.6-inch Laptop http://amzn.to/2BnXhHV Xiaomi Mi A1 (Gold, 64 GB) http://amzn.to/2IDJphb Boat Rockerz 400 On-Ear Bluetooth Headphones (Carbon Black) http://amzn.to/2pue0ov Mi Band - HRX Edition (Black) http://amzn.to/2ps5MxP ******** ✎ ✎ ✎ All the Information are taken from external websites and we have no responsibilities regarding the truth of the facts ✎ ✎ ✎ ☀ ☀ ☀ Like and Follow Rahasya Tv on Facebook ☀ ☀ ☀ https://www.facebook.com/rahasyatv ☀ ☀ ☀ Follow us on our Blog ☀ ☀ ☀ http://www.rahasyatv1.blogspot.in ♫ ♫ ♫ ♫ Music Source ♫ ♫ ♫ ♫ http://incompetech.com/music/royalty-free/music.html https://www.youtube.com/audiolibrary/music ✍ ✍ Source ✍ ✍ External Web sites. ============ Copyright Disclaimer Under Section 107 of the Copyright Act 1976, allowance is made for "fair use" for purposes such as criticism, comment, news reporting, teaching, scholarship, and research. Fair use is a use permitted by copyright statute that might otherwise be infringing. Non-profit, educational or personal use tips the balance in favor of fair use. ============ ❀ ❀ ❀ Like, Share and Comment Our Videos ❀ ❀ ❀ ❀ ❀ Thank You ❀ ❀ ❀ ♟ ♟ ♟ Also, Check ♟ ♟ ♟
Views: 189500 Rahasya Tv
CASSINI's Grand Finale - Live From NASA Mission Control
The Cassini spacecraft has been orbiting Saturn since 2004. The mission is known for discoveries such as finding jets of water erupting from Enceladus, and tracking down a few new moons for Saturn. Now low on fuel, the spacecraft will make a suicidal plunge into the ringed planet in 2017 and capture some data about Saturn's interior on the way. Credit: NASA JPL Follow Us: Facebook: https://goo.gl/QapZAe Twitter: https://goo.gl/RoQSmJ
Views: 2262 DEEP SPACE TV
Mass of Saturn
Detailed Solution
Views: 162 Brent Holt
Cassini - Saturn
The sounds and colourful spectrogram in this still image and video represent data collected by the Radio and Plasma Wave Science, or RPWS, instrument on NASA's Cassini spacecraft, as it crossed through Saturn's D ring on May 28, 2017. This was the first of four passes through the inner edge of the D ring during the 22 orbits of Cassini's final mission phase, called the Grand Finale. During this ring plane crossing, the spacecraft was oriented so that its large high-gain antenna was used as a shield to protect more sensitive components from possible ring-particle impacts. The three 10-meter-long RPWS antennas were exposed to the particle environment during the pass. As tiny, dust-sized particles strike Cassini and the RPWS antennas, the particles are vaporized into tiny clouds of plasma, or electrically excited gas. These tiny explosions make a small electrical signal (a voltage impulse) that RPWS can detect. Researchers on the RPWS team convert the data into visible and audio formats, some like those seen here, for analysis. Ring particle hits sound like pops and cracks in the audio. Particle impacts are seen to increase in frequency in the spectrogram and in the audible pops around the time of ring crossing as indicated by the red/orange spike just before 14:23 on the x-axis. Labels on the x-axis indicate time (top line), distance from the planet's center in Saturn radii, or Rs (middle), and latitude on Saturn beneath the spacecraft (bottom). These data can be compared to those recorded during Cassini's first dive through the gap between Saturn and the D ring, on April 26 (see PIA21446). While it appeared from those earlier data that there were essentially no particles in the gap, scientists later determined the particles there are merely too small to create a voltage detectable by RPWS, but could be detected using Cassini's dust analyzer instrument. After ring plane crossing (about 14:23 onward) a series of high pitched whistles are heard. The RPWS instrument detects such tones during each of the Grand Finale orbits and the team is working to understand their source. The D ring proved to contain larger ring particles, as expected and recorded here, although the environment was determined to be relatively benign – with less dust than other faint Saturnian rings Cassini has flown through.
Views: 582 Kowch737
Measuring the Mass of the Earth from the Orbit of the Moon
Application of Newton's form of Kepler's 3rd Law. The mass of a central body can be calculated from the orbital period and orbital radius of its moon.
Views: 4344 William Pezzaglia
Exoplanets: The Quest for Strange New Worlds (live public talk)
Original air date: January 12 at 7 p.m. PT (10 p.m. ET, 0300 UTC) Planets orbiting other stars, or exoplanets, have become an important field of astronomical study over the past two and a half decades. Recent findings from NASA's Kepler mission suggest that nearly every star you see in the night sky probably has exoplanets orbiting it. The number of confirmed exoplanets is now a few thousand. This talk will present a brief history of exoplanet discoveries, the story of the “super-Saturn” extrasolar ring system, and summarize NASA’s ongoing future plans to discover and characterize “strange new worlds.” Speaker: Eric Mamajek, Deputy Program Chief Scientist, NASA Exoplanet Exploration Program, JPL
Saturn V Tribute and launch Audio
SEPTEMBER 2001. http://en.wikipedia.org/wiki/Saturn_V The origins of the Saturn V rocket begin with the US government bringing Wernher von Braun along with about seven hundred German rocket engineers and technicians to the United States in Operation Paperclip, a program authorized by President Truman in August 1946 with the purpose of harvesting Germany's rocket expertise, to give the US an edge in the Cold War through development of intermediate-range (IRBM) and intercontinental ballistic missiles (ICBM). It was known that America's rival, the Soviet Union, would also try to harvest some of the Germans. Von Braun was put into the rocket design division of the Army due to his direct involvement in the creation of the V-2 rocket. Between 1945 and 1958, his work was restricted to conveying the ideas and methods behind the V-2 to the American engineers.Despite Von Braun's many articles on the future of space rocketry, the US Government continued funding Air Force and Navy rocket programs to test their Vanguard missiles despite numerous costly failures. It was not until the 1957 Soviet launch of Sputnik atop an R-7 ICBM capable of carrying a thermonuclear warhead to the US, that the Army and the government started taking serious steps towards putting Americans in space.Finally, they turned to von Braun and his team, who during these years created and experimented with the Jupiter series of rockets. The Juno I was the rocket that launched the first American satellite in January 1958, and part of the last-ditch plan for NACA (the predecessor of NASA) to get its foot in the Space Race.[8] The Jupiter series was one more step in von Braun's journey to the Saturn V, later calling that first series "an infant Saturn". Saturn development Main article: Saturn (rocket family) The Saturn V's design stemmed from the designs of the Jupiter series rockets. As the success of the Jupiter series became evident, the Saturn series emerged. http://www.autocarindia.com/ http://en.wikipedia.org/wiki/Apollo_17 -- Apollo 17 was the final mission of the United States' Apollo lunar landing program, and was the sixth and last landing of humans on the Moon. Launched at 12:33 AM Eastern Standard Time (EST) on December 7, 1972, with a three-member crew consisting of Commander Eugene Cernan, Command Module Pilot Ronald Evans, and Lunar Module Pilot Harrison Schmitt, It was the last use of Apollo hardware for its original mission. After Apollo 17, extra Apollo spacecraft were used in the Skylab and Apollo--Soyuz Test Project programs. Apollo 17 was the sixth Apollo lunar landing, the first night launch of a U.S. human spaceflight and the final crewed launch of a Saturn V rocket. It was a "J-type mission," which included a three-day lunar surface stay, extended scientific capability, and the third Lunar Roving Vehicle (LRV). While Evans remained in lunar orbit above in the Command/Service Module (CSM). Cernan and Schmitt spent just over three days on the lunar surface in the Taurus-Littrow valley, conducting three periods of extra-vehicular activity, or moonwalks, during which they collected lunar samples and deployed scientific instruments. Cernan, Evans, and Schmitt returned to Earth on December 19 after an approximately 12-day mission. The decision to land in the Taurus-Littrow valley was made with the primary objectives for Apollo 17 in mind: to sample lunar highland material older than the impact that formed Mare Imbrium and investigating the possibility of relatively young volcanic activity in the same vicinity. Taurus-Littrow was selected with the prospects of finding highland material in the valley's north and south walls and the possibility that several craters in the valley surrounded by dark material could be linked to volcanic activity. Apollo 17 also broke several records set by previous flights, including the longest manned lunar landing flight; the longest total lunar surface extravehicular activities; the largest lunar sample return, and the longest time in lunar orbit. As of June 2014, Apollo 17 remains the most recent manned Moon landing and also the last time humans have traveled beyond low Earth orbit.
Black Star Short Report May 18 2017
Seismic, volcanic and magnetic North Pole migration indicators say that Earth is at the peak of the first earth change uptick period of the 2017 Earth orbit cycle relative to the Black Star positioned in the Libra Constellation between Jupiter and Saturn relative to the Sun near Mars orbit path. The 2017 cycle seismic pattern continues following the 2015 weekly event values with fewer of the large-mag quake events and higher values for the moderate and lower-mag quake events. See the Seismic Chart in Terral's 2017 Newsletter Volume 20. Complimentary Link: https://goo.gl/yIvagL (Please share) Week 13 of the 2017 Earth orbit cycle represents the first time we have seen more than just two of the 6-magnitude earthquake events in twenty weeks earning red values for the entire column going back to Week 46 of the 2016 Earth orbit cycle, which has not happened since the Project Black Star Investigation began in January 2011. One of these big 6-magnitude earthquake events will likely become our anticipated Sun/Earth/Black Star nearside-alignment quake event, but we need a few weeks to pass to identify the seismic activity peak for making that determination. The magnetosphere has been monitored closely for the last two weeks for indications of a genuine magnetopause reversal that was also absent from the 2013-2015 Earth orbit cycles hampering the process of identifying the nearside-alignment quake events for those years in much the same way. My suspicion is that Jupiter and Saturn being in the same quadrant of the solar system straddling the Black Star on either side relative to the Sun is seeing the lion’s share of solar redirected electromagnetism going to Saturn and particularly to Jupiter, which means there is less electromagnetic energy being pumped into Earth reducing the weekly seismic event values. Earth crust is also becoming more flexible from the expansion/contraction process of moving through two well-defined earth change uptick and lull periods with each Earth orbit cycle masking Black Star gravitational and electromagnetic influences moving through this period. If Earth begins following the 2016 seismic pattern, then we will see a dramatic decrease in weekly seismic event values moving forward.... ...The Mystery Explained manuscript with eighty color-coded diagrams has been sent off to the publisher expected to be available for purchase this summer. The first twenty people making donations of fifty dollars or more at http://terral03.com will receive an autographed copy of The Mystery Explained once I receive the initial book shipment from the publisher. The polished PDF version of The Mystery Explained is now available for download from the 2017 Dropbox Folder for all valued 2017 Newsletter Subscribers and supporters of the research. My plan is to have the 911Truth: Exposing The Cheney/Rumsfeld Black Operation published once The Mystery Explained project is completed that should be available sometime this fall, if everything stays on schedule. Project supporters for this week include Charles, William, Bill, Ann and Cindy subscribing to the Newsletter and Survival Group Programs at http://terral03.com. There were no subscription renewals from previous years and no donations to report again for Week 20. Lawrence upgraded is 25-dollar Newsletter Only Subscription to receive Survival Group benefits that includes obtaining threat assessment information and being connected to like-minded survivalists already working in the Survival Group Program. Linda is putting together the information for her Survival Group Program in New Mexico that will become Option #6 posted in the Survival Group Info notification email sent to existing Group Members and New Members coming into the Program. Get more information on how to subscribe to the Newsletter and Survival Group Programs at http://terral03.com. Many thanks again to everyone supporting the research for making the investigation and Survival Group Program possible. Terral Read the Full Report and related articles using a complimentary link to Terral's 2017 Newsletter Volume 20. Subscribe to the Newsletter/Survival Group Programs and support the research at http://terral03.com.
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