Use LEFT and RIGHT arrow keys to navigate between flashcards;
Use UP and DOWN arrow keys to flip the card;
H to show hint;
A reads text to speech;
62 Cards in this Set
- Front
- Back
|
TerrestrialPlanets/Gas Planets |
PlanetsGas/Ice GiantPlanets
Giant Planets:outer Solar System (cold)made of ices and gases very low density (puffy)large Terrestrial Planets:inner Solar System (warm)made of rock and iron high density small |
|
|
Jupiter |
Largest planet in the Solar SystemMore than 1300 Earths could fit inside Jupiter
More than 2.5 times the mass of all the other planets combined But, Jupiter would have to be 75 times more massive to be a star(nuclear fusion of H into He) |
|
|
Jupiter's Clouds |
Jupiter is permanently covered with clouds
Fast rotation (once every 10 hours) causes the clouds tobe constantly moving and confined to narrow ranges of latitude |
|
|
Jupiter's Zones and Belts |
belts - dark, reddish bands of clouds
zones - light-colored bands of clouds Belts and zones are created by east- or west-flowing gases with very little north-south motionOval-shaped patterns are rotating storms (like hurricanes) |
|
|
Great Red Spot |
Great Red Spot - huge storm, first observed in 1656
large enough to fit two Earths side by sidecause of the red color is not known White ovals - cool clouds high in the atmosphere Brown ovals - warmer clouds that are lower |
|
|
Red Spot Jr. |
2006
Storms come and go in Jupiter’s atmosphere Creating Red Spot Jr.…became a red spot, named Red Spot Jr., in 2006. |
|
|
Differentperial Rotation |
Differential rotation - rotation speed varies with latitude
Poles: rotation period 9h 55min Equator: rotation period 9h 50min Clouds at some latitudes rotate east, at other latitudes they rotate west creates swirl patterns and keeps storms stabilized |
|
|
Jupiter's Low Density & Atmosphere |
Jupiter’s low density (1330 kg m-3) tells us that it is composed of mainly H and He
Atmospheric composition Number of atoms: 86% H 13% He 1% other: methane, ammonia, water vapor,etc Three major cloud layersColors of the layers aren’t understood |
|
|
Sinking air/rising air |
Until recently (2001 or so) zones were thought to be rising air and belts were thought to be sinking air
The opposite is true, however zones - sinking air belts - rising air Result is still convection |
|
|
Below The Cloud Layers |
Below the cloud layers, Jupiter’s mantle is liquid The gases (mostly H) get denser and denser until the atoms are close enough together to qualify as a “liquid” Temperature and pressure increaseas you go down through the atmosphere Boundary between H gas and H liquid would not be noticeable |
|
|
Four distinct regions in Jupiter’s interior (we think)
|
Below the cloud layers:
Liquid molecular H and He Liquid metallic H (able to conduct electricity like a metal) Liquid water, carbon dioxide, methane, and ammonia (“ices”) Small rock and iron core Central pressure: 70,000,000 atmCentral temperature: 25,000 K |
|
|
Aurae on Jupiter |
Earth’s magnetosphere for comparison
Aurorae on Jupiter Jupiter has a large and very strong magnetic field created by the liquid metallic H layer |
|
|
Jupiter’s Magnetosphere
|
Three lightning storms originating in Jupiter’s water cloud layer, imaged by Galileo.
Each image shows changing multiple lightning flashes. The brightest flashes are as powerful as 30 million 100-watt lightbulbs shining for 1 second. This is much more powerful than any lightning on Earth |
|
|
Comet ShoemakerLevy 9 |
In 1992, comet Shoemaker-Levy 9 passed too closely to Jupiter and was pulled apart into many pieces
In 1994, those pieces of the comet slammed into Jupiter creating a string of impact sites in the upper atmosphere |
|
|
Jupiter’s Moons
|
Jupiter has about 67 moons; the four largest (Galilean satellites) probably formed the same way as the inner planets.
The others are captured planetesimals and smaller pieces of space debris. The inner and six outer moons orbit in the same direction Jupiter rotates (prograde). The rest display retrograde orbit. |
|
|
Jupiter's Moons Continued |
Jupiter has at least
67 moons(finding more all the time) All named after lovers or favorites of Jupiter/Zeus in mythology Four largest moons called the Galilean satellites |
|
|
Io |
Io is the closest Galilean satellite to Jupiter
Mostly rock and ironSurface covered with volcanoes and geysers Surface colors mostly caused by sulfur compounds from volcanoes Thin atmosphere of oxygen, sulfur, and sulfur dioxide |
|
|
Io |
Photographed in 1999 and then 2000 (shown here), the ongoing lava flow from this volcanic eruption at Tvashtar Catena has considerably altered this region of Io’s surface.
|
|
|
Tidal Forces |
Tidal forces between Jupiter and other Galilean satellites squeeze and flex Io
Friction heats the interior of Io, provides gases and melted rock for Io’s geysers and volcanoes Io is tidally locked with Jupiter |
|
|
Europa |
Europa is the next closest Galilean satellite to Jupiter
Also has strong tidal forces from Jupiter and the other moons, causing internal heating Liquid water under its icy surface ?? Also has an iron core and small magnetic field |
|
|
Water volcanism on Europa?
|
Lenticulae - surface domes caused by rising, warmed ice blobs (imagine a very slow lava lamp)
Liquid water = good place to look for other lifeforms in the Solar System Very thin oxygen atmosphere from breakdown of ice |
|
|
Ganymede |
Ganymede: third Galilean satellite from Jupiter
Larger than Mercury Magnetic field twice as strong as Mercurys Inner structure of Ganymede:Iron-rich core Rocky mantle Underground liquid saltwater ocean Dirty ice crust Thin atmosphere Measurements of time-varying secondary magnetic field =Liquid water ocean ? (saltwater is a good conductor) |
|
|
2 types of terrain on Ganymede |
Two types of terrain on Ganymede
Evidence for early tectonic activity ?Ganymede’s crust is frozen solid today, no more plate tectonics Very thin oxygen atmosphere Aurorae on Ganymede |
|
|
Callisto |
Callisto: fourth Galilean satellite
Similar size and density to Ganymede,with thin H and CO2 atmosphere Also has a variable magnetic field, likely caused by saltwater ocean No young, grooved terrainProbably froze very quickly Valhalla Basin is a giant impact basin (crater) |
|
|
Callisto
|
The two insets in this Galileo image show spires that contain both ice and some dark material. The spires, which were probably thrown up by an impact, erode as dark material in them absorbs heat from the Sun.
|
|
|
Other stuff orbiting Jupiter |
Other stuff orbiting Jupiter:
at least 59 smaller moons ringlets 2 tori of charged gas other satellites irregularly shaped many of the outer moons orbit Jupiter backwards= captured asteroids (?)innermost moons probably clumps from one body that was smashed |
|
|
Jupitrers Rings |
rings made of volcanic material from Io and surface material knocked off other moons by impacts
Radiation from Sun and Jupiter continuously push ring pieces out of orbit Rings constantly replenished with new pieces, else rings would be gone |
|
|
Tori |
At least two doughnut-shaped tori (plural for torus) filled with electrically-charged gas (plasma)
One has the same orbit as Io; composed of sulfur and oxygen ions and held in place by Jupiter’s magnetic field The other has the same orbit as Europa; composed of hydrogen and oxygen ions |
|
|
Saturn |
Saturn is similar to Jupiter in many ways belts and zones in its atmosphere (but partially obscured by a haze layer over them)hurricane-like storms
atmosphere is mostly H and He differential rotation |
|
|
Saturn's Mass Relative to Jupiter |
Saturn is less massive than JupiterIt has less gravity, so its atmosphere is puffier
Winds moving 1000mph detected on Saturn |
|
|
Merging Storms on Saturn
|
This sequence of Cassini images shows two hurricanelike storms merging into one on Saturn in 2004. Each storm is about 1000 km (600 mi) across.
|
|
|
Storm Sweeping across Saturn
|
This storm swept around Saturn’s northern mid latitudes throughout 2011.
|
|
|
Saturn's Interior |
Saturn’s interior is similar to Jupiter’s
but its interior is less compressed because it has less mass (less gravity) Saturn has the lowest density of any planet in the Solar System Saturn could float in water if you found a bathtub big enough for it |
|
|
Saturn's Magnetic Field |
Liquid metallic hydrogen layer in Saturn creates a magnetic field just like in Jupiter
Aurorae |
|
|
Saturn's Rings |
Saturn’s rings are tilted by 27°
Our view of rings changes as Saturn orbits the Sun Saturn’s rings are composed of many thin ringlets Ringlets made of small pieces ofice and rock |
|
|
Numerous Thin Ringlets Constitute Saturn’s Inner Rings
|
This Cassini image shows some of the structure of Saturn’s rings, including some of the moonlets orbiting in them. As moons orbit near or between rings, they often cause the ring ices to develop ripples, like the grooves in a phonograph record.
|
|
|
Numerous Thin Ringlets Constitute Saturn’s Inner Rings
|
Debris piles up along the outer edge of Saturn’s B ring just inside the Cassini division.
The shadows of this material indicate how irregular this edge is compared to the body of the ring |
|
|
Numerous Thin Ringlets Constitute Saturn’s Inner Rings
|
From Saturn’s night side, the smaller pieces of debris scatter light from the Sun toward Cassini, including dust-sized particles in the Cassini division. The Cassini division is bright in this image, while the B ring is quite dark. (NASA/JPL/Space Science Institute)
|
|
|
Difference within the rings |
Different rings have particles of different sizes= differences in brightness and color
Even the “gaps” are filled with tiny dust-sized particles Most common particles are centimeter-sized |
|
|
ShepherdMoons |
shepherd moons - small moons whose gravitational forces help keep a ring well-definedTogether, Prometheus and Pandora “shepherd” the particles in the F ringlets
Pandora Prometheus |
|
|
Disturbances alongthe rings |
Ripples and disturbances in the rings can be created by small moons
Dark spokes in the rings: caused by electric charges on the ring particles interacting with Saturn’s magnetic field? Spokes are probably dark because electric charge separates particles(less particles toreflect light) |
|
|
Saturn and Its Outer, Giant Ring
|
This artist’s rendition of Saturn’s giant ring is drawn to scale with an infrared image of Saturn and the rings we normally see. The giant ring spans the region from 6 million km (3.7 million mi) to 18 million km (11.1 million mi) beyond Saturn. Put another way, the giant ring is as wide as 30 Saturns placed side by side.
|
|
|
Saturn's Moons |
Some moons live in the rings,
some clear gaps in the rings, some live outside the rings Saturn has 60 known moons Only 7 are massive enough to be spherical in shape examples of nonspherical moons |
|
|
Titan |
Titan is Saturn’s largest moon
Second largest moon in Solar System (behind Ganymede) Only moon in Solar System with a thick atmosphere (4 times thicker than Earth’s) Atmosphere is mostly nitrogen withclouds of methane that come and go seasonally |
|
|
River beds on Titan |
River beds on Titan
Liquid methane rains out of Titan’s atmosphere Titan’s surface has rivers and lakes of liquid methane and ethane Some of the lakes even have islands |
|
|
Huygens Probe |
Huygens probe parachuted down to the surface of Titan in 2005
mountains imaged as the probe fell through Titan’s atmosphere pebbles on the surface of Titan at landing sitevery few craters = young surface |
|
|
Surface Features on Titan
|
Mimas
Rhea (diameter 1530 km, or 950 mi) is heavily cratered. The bluish regions on the inset are believed to be ices uncovered as a result of impacts. |
|
|
Enceladus
|
Saturn’s 6th largest moonicy, wrinkled surface similar to Jupiter’s Europa and Ganymede
southern hemisphere is crater-free and filled with large ice blocks and blue “tiger stripes” -- all point to liquid water under the surface |
|
|
Encleladus Surface |
Ice volcanoes and geysers are seen on Enceladus’ surface
Also has a small magnetic field (liquid saltwater?)Thin atmosphere composed of H, CO2, N, and CO |
|
|
Uranus |
Uranus has belts and zones like Jupiter and Saturn
Infrared Visible Can only be seen in infrared wavelengths of light Hidden by haze in upper atmosphere Methane clouds come and go |
|
|
Uranus Atmosphere |
Atmosphere mostly H and He with
some water ice clouds and frozen methane clouds Differential rotation like Jupiter and Saturn 3 inner layers(no metallic H layer - not massive enough) Uranus’ axis of rotation is tilted by 98° (perhaps caused by giant impact) |
|
|
Large tilt Of Uranus |
Large tilt = Exaggerated seasons on Uranus
Seasons last a very long time because Uranus takes 84 Earth years to orbit the Sun |
|
|
Uranus Magnetic field |
Uranus’ magnetic field is tilted 59° from the planet’s poles and does not pass through the center of the planet
The magnetosphere wobbles significantly as the planet rotates Magnetic field thought to be caused by ionized ammonia and other molecules in its water layer(ions conduct electricity) |
|
|
Uranus Rings |
Uranus has 13 ringlets and 27 known moonsMany of its moons are shepherd moons
|
|
|
Discovery of the Rings of Uranus
|
Light from a star is reduced as the rings move in front of it. (b) With sensitive light meters, astronomers can detect the variation in light intensity. Such dimming led to the discovery of Uranus’s rings. Of course, the star vanishes completely when Uranus occults it.
|
|
|
Miranda |
Miranda is a“seriously disturbed” moon
May have been broken apart by a giant impact and then came back together Or could have experiencedsevere tidal heating Close-up of cliffs on Miranda. |
|
|
Neptune |
Neptune is very similar to Uranus
Belts and zones, but less haze= more easily visible Atmosphere is mostly H and He and undergoes differential rotation Methane clouds come and go, as do giant storms (dark spots) |
|
|
Interior of Neptune is very similar to interior of Uranus
|
Neptune’s axis is tilted 30°
Its magnetic field is tilted from the planet’s poles and does not pass through the center of the planet Magnetic field also comes from ions in Neptune’s interior water layer |
|
|
Neptune's Rings |
Neptune also has rings and 13 known moons
12 of Neptune’s moons are small and irregularly-shaped Triton is Neptune’s largest moon Spherical shape, but retrograde (backwards) orbit Captured by Neptune? |
|
|
Triton’s South Polar Cap
|
About a dozen high-resolution Voyager 2 images were combined to make this view of Triton’s southern hemisphere. The pinkish polar cap is probably nitrogen frost. A notable scarcity of craters suggests that Triton’s surface was either melted or flooded by icy lava after the era of bombardment that characterized the early history of the solar system.
|
|
|
A Frozen Lake on Triton
|
Scientists think that the feature in the center of this image is a basin filled with water ice. The flooded basin is about 200 km across.
|
|
|
The Capture and Destruction of Triton
|
This series of drawings depicts how (a) Triton was captured by Neptune in a retrograde orbit. (b) The tides that Triton then exerted on the planet caused that moon’s orbit to become quite circular and (c) to spiral inward. (d) Triton will eventually reach Neptune’s Roche limit and (e) be pulled apart to form a ring.
|
