Which planet in our soar system spins on its axis faster than any of the other planets?
"with Jupiter than with the other giant planets, some have claimed that ""jovian planet"" is a more accurate term for them. Many of the exoplanets are much closer to their parent stars and hence much hotter than the giant planets in the Solar System, making it possible that some of those planets are a type not observed in the Solar System. Considering the relative abundances of the elements in the universe (approximately 98% hydrogen and helium) it would be surprising to find a predominantly rocky planet more massive than Jupiter. On the other hand, models of planetary-system formation have suggested"
"As a result, it does not experience significant seasonal changes, in contrast to, for example, Earth and Mars. Jupiter's rotation is the fastest of all the Solar System's planets, completing a rotation on its axis in slightly less than ten hours; this creates an equatorial bulge easily seen through an Earth-based amateur telescope. The planet is shaped as an oblate spheroid, meaning that the diameter across its equator is longer than the diameter measured between its poles. On Jupiter, the equatorial diameter is longer than the diameter measured through the poles. Because Jupiter is not a solid body, its upper"
"spins 642 times per second and, until the discovery of PSR J1748-2446ad in 2005, was identified as the fastest-spinning pulsar. In August 1989, the observatory directly imaged an asteroid for the first time in history: 4769 Castalia. The following year, Polish astronomer Aleksander Wolszczan made the discovery of pulsar PSR B1257+12, which later led him to discover its three orbiting planets. These were the first extrasolar planets discovered. In 1994, John Harmon used the Arecibo Radio Telescope to map the distribution of ice in the polar regions of Mercury. In January 2008, detection of prebiotic molecules methanimine and hydrogen cyanide"
"potential ""rogue planets"" are excluded. In the Solar System, all the planets orbit the Sun in the same direction as the Sun rotates (counter-clockwise as seen from above the Sun's north pole). At least one extrasolar planet, WASP-17b, has been found to orbit in the opposite direction to its star's rotation. The period of one revolution of a planet's orbit is known as its sidereal period or ""year"". A planet's year depends on its distance from its star; the farther a planet is from its star, not only the longer the distance it must travel, but also the slower its"
"speed, because it is less affected by its star's gravity. No planet's orbit is perfectly circular, and hence the distance of each varies over the course of its year. The closest approach to its star is called its periastron (perihelion in the Solar System), whereas its farthest separation from the star is called its apastron (aphelion). As a planet approaches periastron, its speed increases as it trades gravitational potential energy for kinetic energy, just as a falling object on Earth accelerates as it falls; as the planet reaches apastron, its speed decreases, just as an object thrown upwards on Earth"
"Beta Pictoris b orbits its host star every 21 years at a distance of 9.2 AU (about the same as Saturn's distance, which is about 9.55 AU). It receives 11% of the amount of sunlight that Earth does from the Sun. In 2014, the rotation period of Beta Pictoris b was calculated from the broadening of its carbon monoxide infrared absorption line. This makes it, , the first extrasolar planet to have its rotation rate measured. With a rotation period of 8.1 hours, it is the fastest-spinning planet known. Its rotation period is faster than that of Jupiter, which has"
"S2 the fastest known ballistic orbit, reaching speeds exceeding 5,000 km/s (11,000,000 mph, or 1/60 the speed of light) and acceleration of about 1.5 m/s (almost one-sixth of Earth's surface gravity). The motion of S2 is also useful for detecting the presence of other objects near to Sagittarius A*. It is believed that there are thousands of stars, as well as dark stellar remnants (stellar black holes, neutron stars, white dwarfs) distributed in the volume through which S2 moves. These objects will perturb S2's orbit, causing it to deviate gradually from the Keplerian ellipse that characterizes motion around a single"
"burning its core hydrogen for another 75 million years and the secondary around 500 million years. Both stars will cool and expand once their core hydrogen is exhausted, becoming red giants. The brighter component, Theta Coronae Borealis A, is a blue-white star that spins extremely rapidly—at a rate of around 393 km per second. This rapid spinning is thought to be the cause of a gaseous disk that surrounds the star: such stars are known as Be shell stars, recognizable because the gas radiates emission lines that give a characteristic pattern in the star's spectrum. Of spectral type B6Vnn, Theta"
"() is the ruling planet of Gemini and is exalted in Virgo and/or Aquarius. In classical Roman mythology, Mercury is the messenger of the gods, noted for his speed and swiftness. Echoing this, the scorching, airless world Mercury circles the Sun on the fastest orbit of any planet. Mercury takes only 88 days to orbit the Sun, spending about 7.33 days in each sign of the zodiac. Mercury is so close to the Sun that only a brief period exists after the Sun has set where it can be seen with the naked eye, before following the Sun beyond the"
"with spectral types of K and M and masses less than half the sun's. There are also around 60 hotter stars in the region, including the eruptive variable V346 Tauri. Like the star Pleione in the Pleiades open cluster, 25 Ori is a Be star with a gaseous circumstellar disk. The SIMBAD astronomical database lists its spectral class as B1Vn. 25 Orionis is a fast rotator, clocking a rotational velocity of 316 km/s, significantly faster than Achernar's speed of 251 km/s in the constellation Eridanus. Having a radius of , the star rotates on its axis roughly once every 23"
"per second, PSR B1937+21 was the fastest spinning neutron star known. As of 2010, PSR B1937+21 remains the second fastest spinning pulsar known. In addition to extending the range of periods observed in pulsars by a factor of 20, it also extended the range of magnetic fields observed by a factor of 100, with a magnetic field of 4.2 gauss (42 kT). As the first discovered millisecond pulsar, PSR B1937+21 ""sparked a 'theory frenzy'"" by providing a new laboratory in which to study pulsars, neutron stars more generally, and perhaps even some other astrophysical problems such as gravitational waves. For"
"PSR J1748-2446ad ! style=""background-color: #FFFFC0;"" colspan=""2"" | Astrometry PSR J1748-2446ad is the fastest-spinning pulsar known, at 716 Hz, or 716 times per second. This pulsar was discovered by Jason W. T. Hessels of McGill University on November 10, 2004 and confirmed on January 8, 2005. It has been calculated that the neutron star contains slightly less than two times the mass of the Sun, within the typical range of neutron stars. Its radius is constrained to be less than 16 km. At its equator it is spinning at approximately 24% of the speed of light, or over 70,000 km per"
"amplitude of the velocity changes, a mass of at least 2.26 times that of planet Jupiter is deduced for the planet. It revolves around the host star in a somewhat elongated orbit. If it were located in the Solar System, this orbit would stretch from just outside the orbit of Venus (at 117 million km or 0.78 astronomical unit [AU] from the Sun) to just outside the orbit of the Earth (at 162 million km or 1.08 AU). Because the planet is at least 720 times more massive than the Earth, it is predicted that Iota Horologii b is more"
"these appear to be optical companions. This system is a member of the thin disk population and is following an orbit through the Milky Way galaxy with an eccentricity of 0.12. It comes as close to the Galactic Center as and as distant as . This orbit carries it no more than about 330 ly (100 pc) above the galactic plane. It is considered a runaway star because it has a high peculiar velocity of 35.5 km s relative to the typical motion of stars in its vicinity. In 2012, an extrasolar planet designated Omicron Ursae Majoris Ab and orbiting"
"as a brown dwarf. This system is a member of the eponymous AB Doradus Moving Group, a loose stellar association of about 30 stars that are all approximately the same age and moving in the same general direction. It is likely that all of these stars formed in the same giant molecular cloud. AB Doradus AB Doradus is a pre-main-sequence quadruple star system in the constellation Dorado. The primary is a flare star that shows periodic increases in activity. The primary star in this system spins at a rate 50 times that of the Sun, and consequently has a strong"
"from the star. Both of these planets are in more eccentric orbits than any of the planets in the Solar System (including Pluto). Upsilon Andromedae d resides in the system's habitable zone. The orbital parameters of this three planet system have been fully determined. The system is not coplanar, with each other or with the stellar rotation, as in our solar system. Simulations shows that the measured configuration of the planets produces indeed stable orbits for at least 100 million years, where planets ""b"" and ""d"" remain roughly coplanar. General relativity is expected to have strong effects on planet ""b"","
"on its axis. Pleione is spinning so fast that it is close to the estimated breakup velocity for a B8V star of about 370–390 km/s. Another Be star whose rotational velocity is extremely fast is Alpha Arae at 470 km/s—a speed so extreme that it is on the verge of exploding. What makes Pleione particularly unique is that it alternates between three different phases: 1) normal B star, 2) Be star and 3) Be shell star. The cause is likely the surrounding gaseous disk which in many Be stars will appear, then disappear, possibly reforming at a later time. Material"
"PSR J0337+1715 PSR J0337+1715 is a millisecond pulsar discovered in a Green Bank Telescope drift-scan survey from 2007. It is spinning nearly 366 times per second, 4200 light years away in the constellation Taurus. It is co-orbiting very closely with another star, a white dwarf, with a period of 1.6 days. There is a second white dwarf further out (within one astronomical unit) which is orbiting both the pulsar and the inner white dwarf, and has an orbit with a period of 327 days. It thus provides an opportunity to test the nature of gravity and the strong equivalence principle,"
"Moons revolve around their planet, planets revolve about their star (such as the Earth around the Sun); and stars slowly revolve about their galaxial center. The motion of the components of galaxies is complex, but it usually includes a rotation component. Most planets in our solar system, including Earth, spin in the same direction as they orbit the Sun. The exceptions are Venus and Uranus. Uranus rotates nearly on its side relative to its orbit. Current speculation is that Uranus started off with a typical prograde orientation and was knocked on its side by a large impact early in its"
"times Earth's orbital velocity. The star was the fastest moving star ever seen in an X-ray binary system until the recent discovery of system 47 Tuc X9. On the other hand, the black hole orbits at 'only' . The black hole in this compact pairing is at least three times more massive than the Sun, while its red dwarf companion star has a mass only 20% that of the Sun. The pair is separated by roughly a million kilometers – for comparison the distance to the Sun from Earth is about 150 million kilometers. MAXI J1659-152 MAXI J1659-152 is a"
"Historical brightest stars The Solar System and all of the visible stars are in different orbits about the core of the Milky Way galaxy. Thus, their relative positions change over time, and for the nearer stars this movement can be measured. As a star moves toward or away from us, its apparent brightness changes. Sirius is currently the brightest star in Earth's night sky, but it has not always been so. Canopus has persistently been the brightest star over the ages; other stars appear brighter only during relatively temporary periods, during which they are passing the Solar System at a"
"Sirius in fiction The planetary systems of stars other than the Sun and the Solar System are a staple element in much science fiction. Sirius, a double star system with the binary designation Sirius AB, is the brightest stellar object in the night sky. Its component stars are Sirius A (the primary—twice as massive and 25 times more luminous than the Sun) and Sirius B (the secondary—a faint white dwarf). The distance separating Sirius A from its companion varies between 8.1 and 31.5 AU, reflecting the eccentricity of their mutual orbits. The system contains no known extrasolar planets (see ""Traveller"""
"been discovered. Pulsar PSR J1748-2446ad, discovered in 2005, is, as of 2012, the fastest-spinning pulsar currently known, spinning 716 times a second. Current theories of neutron star structure and evolution predict that pulsars would break apart if they spun at a rate of c. 1500 rotations per second or more, and that at a rate of above about 1000 rotations per second they would lose energy by gravitational radiation faster than the accretion process would speed them up. However, in early 2007 data from the Rossi X-ray Timing Explorer and INTEGRAL spacecraft discovered a neutron star XTE J1739-285 rotating at"
"angular momentum of the star are 1900 and 400 times, respectively, larger than those of the Sun. This causes significant classical and relativistic deviations from Kepler's laws. In particular, the fast rotation causes large nodal precession because of the star's oblateness and the Lense–Thirring effect. In April 2014, the first measurement of a planet's rotation period was announced: the length of day for the super-Jupiter gas giant Beta Pictoris b is 8 hours (based on the assumption that the axial tilt of the planet is small.) With an equatorial rotational velocity of 25 km per second, this is faster than"
"has a high peculiar velocity of relative to the normal galactic rotation. Runaway stars can be produced through several means, such as through an encounter with another binary star system. Binary systems form a relatively small fraction of the total population of runaway stars. Beta Muscae Beta Muscae, Latinized from β Muscae, is a binary star in the southern circumpolar constellation of Musca. With a combined apparent visual magnitude of 3.07, it is the second brightest star (or star system) in the constellation. Judging by the parallax results, it is located at a distance of roughly from the Earth. This"
"the planet a circular orbit. In comparison, planet Mercury orbits the Sun at .3871 AU every 87.97 days. Mercury also has an elliptical orbit, with an eccentricity of .2056. Kepler-8 Kepler-8 is a star located in the constellation Lyra in the field of view of the Kepler Mission, a NASA-led operation tasked with discovering terrestrial planets. The star, which is slightly hotter, larger, and more massive than the Sun, has one gas giant in its orbit, Kepler-8b. This gas giant is larger than Jupiter, but is less massive, and thus more diffuse. The planet's discovery was announced to the public"
"it doesn't include Gliese 710 which in about 1.35 million years time is expected to be close enough to have a magnitude of -2.7. Historical brightest stars The Solar System and all of the visible stars are in different orbits about the core of the Milky Way galaxy. Thus, their relative positions change over time, and for the nearer stars this movement can be measured. As a star moves toward or away from us, its apparent brightness changes. Sirius is currently the brightest star in Earth's night sky, but it has not always been so. Canopus has persistently been the"
"The less massive member is an O8 main sequence star of approximately . It moves in its orbit at a speed of over 300 km/s and is considered to be a relativistic binary, which causes the apses of the orbit to change in a predictable way. The closeness of the two stars causes them to become deformed, and this means that the observed brightness of the system varies slightly every six days during its orbit. The total amplitude of the variation is only 0.02 magnitudes. Among its neighbors are some of the most massive and luminous stars in the galaxy,"
"Epsilon Tauri b Epsilon Tauri b (abbreviated ε Tauri b or ε Tau b), also named Amateru, is a super-Jupiter exoplanet orbiting the K-type giant star Epsilon Tauri approximately 155 light-years (47.53 parsecs, or nearly km) away from the Earth in the constellation of Taurus. It orbits the star further out than Earth orbits the Sun. It has moderate eccentricity. The planet orbits one of the four giant stars in the Hyades cluster that is 2.7 times the mass of our Sun, making it the most massive planet-harboring star. This provides evidence that it was an A-type star when it"
"has the shortest known spin period of any white dwarf, completing a full revolution every 33.08 seconds. This spin is decreasing at a rate of 1.78 ns per year, which is unusually high. The secondary star has a stellar classification of K4-5 V, making it a main sequence star that is generating energy at its core through the thermonuclear fusion of hydrogen. It has about 37% of the Sun's mass but 79% of the Sun's radius. This system displays flare activity that has been observed across multiple bands of the electromagnetic spectrum, including X-rays. Mass is being lost from the"
"MAXI J1659-152 MAXI J1659-152 is a rapidly rotating black-hole/star system, discovered by NASA's Swift space telescope on September 25, 2010. On March 19, 2013, ESA's XMM-Newton space telescope has helped to identify a star and a black hole that orbit each other at the rate of once every 2.4 hours. The black hole and the star orbit their common center of mass. Because the star is the lighter object, it lies farther from this point and has to ""travel around its larger orbit at a breakneck speed of two million kilometers per hour"", 500 to 600 km/s, or about 20"
"orbital body are ""not periodic and can be fully explained in terms of slow changes in the pulsar’s dispersion measure."" PSR B1257+12 PSR B1257+12, previously designated PSR 1257+12, alternatively designated PSR J1300+1240, also named Lich, is a pulsar located 2,300 light years from the Sun in the constellation of Virgo. The pulsar has a planetary system with three known extrasolar planets, named ""Draugr"" (PSR B1257+12 b or PSR B1257+12 A), ""Poltergeist"" (PSR B1257+12 c or PSR B1257+12 B) and ""Phobetor"" (PSR B1257+12 d or PSR B1257+12 C), respectively. They were both the first extrasolar planets and the first pulsar planets"
"retain their velocity (70 km/s, compared to the 17 km/s orbital velocity at Io), and are thus ejected in jets leading away from Io. Io orbits within a belt of intense radiation known as the Io plasma torus. The plasma in this doughnut-shaped ring of ionized sulfur, oxygen, sodium, and chlorine originates when neutral atoms in the ""cloud"" surrounding Io are ionized and carried along by the Jovian magnetosphere. Unlike the particles in the neutral cloud, these particles co-rotate with Jupiter's magnetosphere, revolving around Jupiter at 74 km/s. Like the rest of Jupiter's magnetic field, the plasma torus is tilted"