Jupiter and Saturn
... • Callisto has a heavily cratered crust of water ice • The surface shows little sign of geologic activity, because there was never any significant tidal heating of Callisto • However, some unknown processes have erased the smallest craters and blanketed the surface with a dark, dusty substance • Ma ...
... • Callisto has a heavily cratered crust of water ice • The surface shows little sign of geologic activity, because there was never any significant tidal heating of Callisto • However, some unknown processes have erased the smallest craters and blanketed the surface with a dark, dusty substance • Ma ...
Uranus and Neptune Uranus Saturn Neptune
... Mean density (gm/cm 3)1.64 Mean distance from the Sun (Earth = 1) 30.0611 Rotational period (hours) 16.11 Orbital period (years) 164.79 Orbital eccentricity 0.0097 Tilt of axis (degrees)29.56 Orbital inclination (degrees) 1.774 Equatorial surface gravity (m/sec 2) 11.0 Albedo 0.41 (Magnitude 7.84) M ...
... Mean density (gm/cm 3)1.64 Mean distance from the Sun (Earth = 1) 30.0611 Rotational period (hours) 16.11 Orbital period (years) 164.79 Orbital eccentricity 0.0097 Tilt of axis (degrees)29.56 Orbital inclination (degrees) 1.774 Equatorial surface gravity (m/sec 2) 11.0 Albedo 0.41 (Magnitude 7.84) M ...
The Gas Giants Astronomy Lesson 13
... to as the gas giants. Like the sun, the gas giants are comprised of mainly hydrogen and helium. Because they are so massive, the gas giants have a much larger gravitational force than the terrestrial planets. This increased gravity prevents the gases of the planet from escaping, so they have thick a ...
... to as the gas giants. Like the sun, the gas giants are comprised of mainly hydrogen and helium. Because they are so massive, the gas giants have a much larger gravitational force than the terrestrial planets. This increased gravity prevents the gases of the planet from escaping, so they have thick a ...
Chapter13_New
... comparable to those in the atmosphere of Uranus (Figure 13.6) and result in the beautiful and interesting cloud features on Neptune. Voyager observations of these features have been combined in a video included in the CD that accompanies this textbook. 3. Pluto The demotion of Pluto from planet to d ...
... comparable to those in the atmosphere of Uranus (Figure 13.6) and result in the beautiful and interesting cloud features on Neptune. Voyager observations of these features have been combined in a video included in the CD that accompanies this textbook. 3. Pluto The demotion of Pluto from planet to d ...
Imaging Uranus
... and a greenish hue. Initially Herschel named the object (which he initially believed to be a comet) after his patron King George III. In some texts of the period the planet is referred to as Georgius Sidum or George’s Star. Once its orbit was calculated it was soon realised that the suspected comet ...
... and a greenish hue. Initially Herschel named the object (which he initially believed to be a comet) after his patron King George III. In some texts of the period the planet is referred to as Georgius Sidum or George’s Star. Once its orbit was calculated it was soon realised that the suspected comet ...
Chapter 9
... Jupiter, Saturn, Uranus, and Neptune • Composed mainly of gaseous and liquid hydrogen and its compounds, these planets lack solid surfaces and may have cores of molten rock • The dwarf planets Pluto and Eris are exceptions to these rules resembling the ice and rock makeup of the giant planets’ large ...
... Jupiter, Saturn, Uranus, and Neptune • Composed mainly of gaseous and liquid hydrogen and its compounds, these planets lack solid surfaces and may have cores of molten rock • The dwarf planets Pluto and Eris are exceptions to these rules resembling the ice and rock makeup of the giant planets’ large ...
Saturn Entry Probe Science Objectives
... Typical Atm-Relative Entry Speeds At the Giant Planets Speeds in km/s; assume “typical” hyperbolic approach V∞ Entry Orbit ...
... Typical Atm-Relative Entry Speeds At the Giant Planets Speeds in km/s; assume “typical” hyperbolic approach V∞ Entry Orbit ...
Ch10_Lecture
... Jupiter, Saturn, Uranus, and Neptune • Composed mainly of gaseous and liquid hydrogen and its compounds, these planets lack solid surfaces and may have cores of molten rock • The dwarf planets Pluto and Eris are exceptions to these rules resembling the ice and rock makeup of the giant planets’ large ...
... Jupiter, Saturn, Uranus, and Neptune • Composed mainly of gaseous and liquid hydrogen and its compounds, these planets lack solid surfaces and may have cores of molten rock • The dwarf planets Pluto and Eris are exceptions to these rules resembling the ice and rock makeup of the giant planets’ large ...
Chapter 10 The Outer Worlds… Jupiter Jupiter Jupiter`s Interior
... • Size of equatorial bulge supports the idea that the interior is mostly water and other hydrogen-rich molecules and that it may have a rock/iron core • It is currently not known if the core formed first and attracted lighter gases that condensed on it, or the core formed by differentiation after th ...
... • Size of equatorial bulge supports the idea that the interior is mostly water and other hydrogen-rich molecules and that it may have a rock/iron core • It is currently not known if the core formed first and attracted lighter gases that condensed on it, or the core formed by differentiation after th ...
11/11/08 Chapter 9 The Outer Worlds… Jupiter Jupiter Jupiter`s
... Jupiter, Saturn, Uranus, and Neptune • Composed mainly of gaseous and liquid hydrogen and its compounds, these planets lack solid surfaces and may have cores of molten rock • Pluto is an exception to these rules resembling the ice and rock makeup of the giant planets’ larger moons • The moons of the ...
... Jupiter, Saturn, Uranus, and Neptune • Composed mainly of gaseous and liquid hydrogen and its compounds, these planets lack solid surfaces and may have cores of molten rock • Pluto is an exception to these rules resembling the ice and rock makeup of the giant planets’ larger moons • The moons of the ...
Chapter 9
... Jupiter, Saturn, Uranus, and Neptune • Composed mainly of gaseous and liquid hydrogen and its compounds, these planets lack solid surfaces and may have cores of molten rock • The dwarf planets Pluto and Eris are exceptions to these rules resembling the ice and rock makeup of the giant planets’ large ...
... Jupiter, Saturn, Uranus, and Neptune • Composed mainly of gaseous and liquid hydrogen and its compounds, these planets lack solid surfaces and may have cores of molten rock • The dwarf planets Pluto and Eris are exceptions to these rules resembling the ice and rock makeup of the giant planets’ large ...
Chapter 9
... Jupiter, Saturn, Uranus, and Neptune • Composed mainly of gaseous and liquid hydrogen and its compounds, these planets lack solid surfaces and may have cores of molten rock • The dwarf planets Pluto and Eris are exceptions to these rules resembling the ice and rock makeup of the giant planets’ large ...
... Jupiter, Saturn, Uranus, and Neptune • Composed mainly of gaseous and liquid hydrogen and its compounds, these planets lack solid surfaces and may have cores of molten rock • The dwarf planets Pluto and Eris are exceptions to these rules resembling the ice and rock makeup of the giant planets’ large ...
ring
... Core: small amount of iron and nickel rock Mantle (largest): water, ammonia & methane ices Atmosphere: hydrogen, helium & methane gases ...
... Core: small amount of iron and nickel rock Mantle (largest): water, ammonia & methane ices Atmosphere: hydrogen, helium & methane gases ...
Document
... parallel to the ecliptic plane, instead of perpendicular. • Component perpendicular to the ecliptic points the opposite direction of revolution: retrograde rotation. • The orbital plane of Uranus’s moons is similarly tilted: thus one can’t explain the odd tilt of the planet by invoking one big impac ...
... parallel to the ecliptic plane, instead of perpendicular. • Component perpendicular to the ecliptic points the opposite direction of revolution: retrograde rotation. • The orbital plane of Uranus’s moons is similarly tilted: thus one can’t explain the odd tilt of the planet by invoking one big impac ...
Neptune & Uranus Notes
... The planet Uranus was discovered by British astronomer William Herschel in 1781 Herschel was engaged in charting the faint stars in the sky when he came across an odd-looking object that he described as “a curious either nebulous star or perhaps a comet” The object appeared as a disk in Hersch ...
... The planet Uranus was discovered by British astronomer William Herschel in 1781 Herschel was engaged in charting the faint stars in the sky when he came across an odd-looking object that he described as “a curious either nebulous star or perhaps a comet” The object appeared as a disk in Hersch ...
Chapter 12: Uranus and Neptune
... Seventh planet from the Sun, Uranus is a gas giant far larger than Earth - but modest in size compared to Jupiter. Uranus has an 84-year orbit, a day of 17 hours 48 minutes, a strangely tilted axis, and a magnetic field that is offset by 60 degrees to the rotation axis. That Uranus has rings was dis ...
... Seventh planet from the Sun, Uranus is a gas giant far larger than Earth - but modest in size compared to Jupiter. Uranus has an 84-year orbit, a day of 17 hours 48 minutes, a strangely tilted axis, and a magnetic field that is offset by 60 degrees to the rotation axis. That Uranus has rings was dis ...
The Outer Planets - Amazon Web Services
... hydrogen and helium is actually in liquid form because of the enormous pressure inside the planets. The outer layers of the gas giants are extremely cold because of their great distance from the sun. Temperatures increase greatly within the planets. All the gas giants have many moons. In addition, e ...
... hydrogen and helium is actually in liquid form because of the enormous pressure inside the planets. The outer layers of the gas giants are extremely cold because of their great distance from the sun. Temperatures increase greatly within the planets. All the gas giants have many moons. In addition, e ...
Document
... structures of the Jovian planets are like? A. Probes have been sent into the interiors of the planets and have returned data about the conditions. B. Astronomers use the Earth's internal structure as a basis of comparison. C. Astronomers examine the composition of the satellites of these planets. D. ...
... structures of the Jovian planets are like? A. Probes have been sent into the interiors of the planets and have returned data about the conditions. B. Astronomers use the Earth's internal structure as a basis of comparison. C. Astronomers examine the composition of the satellites of these planets. D. ...
how to bring two neptune mass planets on the same orbit
... We present the results of three simulations performed using the code FARGO-2D1D (code publicly available at http://fargo.in2p3.fr/). The initial density profile of the disk is : Σ0 = 3430(r/10AU)−2.168 kg.m−2 . Jupiter, Saturn, Neptune and Uranus start on circular orbits at 5.45, 8.18, 11.5 and 14.2 ...
... We present the results of three simulations performed using the code FARGO-2D1D (code publicly available at http://fargo.in2p3.fr/). The initial density profile of the disk is : Σ0 = 3430(r/10AU)−2.168 kg.m−2 . Jupiter, Saturn, Neptune and Uranus start on circular orbits at 5.45, 8.18, 11.5 and 14.2 ...
File
... 3. _____ -- largest, but only 1/30th Mm 4. __________ (the “death star”) a. Innermost of 6 (resonates w/ rings) b. Huge crater -________ (1/3 diam.) 5. ___________ a. ~ ___ % reflective! b. Ice crystals /water “__________”! D. The Small Moons 1. Janus & Epimetheus- ___-_______! 2. _________ -chaotic ...
... 3. _____ -- largest, but only 1/30th Mm 4. __________ (the “death star”) a. Innermost of 6 (resonates w/ rings) b. Huge crater -________ (1/3 diam.) 5. ___________ a. ~ ___ % reflective! b. Ice crystals /water “__________”! D. The Small Moons 1. Janus & Epimetheus- ___-_______! 2. _________ -chaotic ...
Question 2 (9-3 thru 9-4 PPT Questions)
... its angular size is very small and it can’t be seen clearly. The first reliable value for Uranus’ diameter came from a telescope in a high-altitude balloon. 3. An improved determination of Uranus’s diameter was made in 1977 during an occultation of a star by the planet. ...
... its angular size is very small and it can’t be seen clearly. The first reliable value for Uranus’ diameter came from a telescope in a high-altitude balloon. 3. An improved determination of Uranus’s diameter was made in 1977 during an occultation of a star by the planet. ...
m15a02
... previous frame what we might expect? • Yes, the higher rotation rate planets have higher oblateness. This, along with the relatively low, but consistent mass with planet size, suggest, as we saw with Jupiter, small rocky cores with overlying liquid and gaseous atmospheres. • Even in the small images ...
... previous frame what we might expect? • Yes, the higher rotation rate planets have higher oblateness. This, along with the relatively low, but consistent mass with planet size, suggest, as we saw with Jupiter, small rocky cores with overlying liquid and gaseous atmospheres. • Even in the small images ...
Uranus
Uranus is the seventh planet from the Sun. It has the third-largest planetary radius and fourth-largest planetary mass in the Solar System. Uranus is similar in composition to Neptune, and both have different bulk chemical composition from that of the larger gas giants Jupiter and Saturn. For this reason, scientists often classify Uranus and Neptune as ""ice giants"" to distinguish them from the gas giants. Uranus's atmosphere, although similar to Jupiter's and Saturn's in its primary composition of hydrogen and helium, contains more ""ices"", such as water, ammonia, and methane, along with traces of other hydrocarbons. It is the coldest planetary atmosphere in the Solar System, with a minimum temperature of 49 K (−224.2 °C), and has a complex, layered cloud structure, with water thought to make up the lowest clouds, and methane the uppermost layer of clouds. The interior of Uranus is mainly composed of ices and rock.Uranus is the only planet whose name is derived from a figure from Greek mythology, from the Latinized version of the Greek god of the sky, Ouranos. Like the other giant planets, Uranus has a ring system, a magnetosphere, and numerous moons. The Uranian system has a unique configuration among those of the planets because its axis of rotation is tilted sideways, nearly into the plane of its revolution about the Sun. Its north and south poles therefore lie where most other planets have their equators. In 1986, images from Voyager 2 showed Uranus as an almost featureless planet in visible light, without the cloud bands or storms associated with the other giant planets. Observations from Earth have shown seasonal change and increased weather activity as Uranus approached its equinox in 2007. Wind speeds can reach 250 metres per second (900 km/h, 560 mph).