Chapter 8. Satellites (moons), Rings, and Plutoids. Reading assignment: Chapter 8

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1 Chapter 8 Satellites (moons), Rings, and Plutoids Reading assignment: Chapter 8

2 Jovian planets satellites There are: Six large satellites, similar in size to our Moon 12 medium-sized to 1500km Many small satellites Jupiter 69 satellites Saturn 62 satellites Uranus 27 satellites Neptune 13 satellites Jupiter s Satellites (Galilean satellites or moons) Io - Jupiter s satellite with active volcanoes! Europa - Jupiter s satellite covered with layer of frozen water strong indications of an ocean of liquid water beneath Ganymede and Callisto - similar in size to our moon, just a bit larger. Ganymede is the largest satellite in the solar system. It may have an ocean of liquid water under the frozen surface Four largest Jupiter satellites - Galilean moons

3 Jupiter Saturn Uranus Neptune Medium and large satellites in the Jovian planets All these satellites have sufficient mass: Selfgravity force them to be spherical Some are now or were in the past geologically active. Most of them have substantial amounts of ice.

4 The largest satellite in the Solar system Second largest

5 Jupiter s Galilean Moons An Unusual Family Moon Io Europa Ganymede Callisto

6 What makes Jupiter s Galilean satellites unusual? Io has several active volcanoes. Europa may have an ocean of liquid water under its icy crust. Ganymede (And perhaps Callisto) may also have sub-surface oceans? How can we account for the unusual features? At that distance from the Sun ( ~5 AU), shouldn t they be completely frozen and showing no activity?

7 Io s Volcanoes Volcanoes were discovered in images from Voyager s spacecraft So far about 80 active volcanoes have been identified using data mainly from Voyager and Galileo spacecrafts Volcanic eruptions mainly composed of sulfur and sulfur dioxide Volcanic plumes about 150 km high and 300 km wide (large because of low gravity) Variety of volcanic hot spots Large lava lakes made of liquid sulfur It is the most volcanic active body in the Solar System Io has a rocky mantle and an iron/iron sulfide core

8 Io: Two images separated by 15 years (The left one taken by Voyager and the last one on the right by the Galileo spacecraft)

9 The plumes of Io s volcanoes, the material ejected from the satellite, the Io torus and the low frequency radio emission The gasses ejected from the volcanic activity are ionized by the UV radiation from the Sun and form a torus of ionized material around the orbits of Io. This ionized material are accelerated by Io and interact with the magnetic field of the planet and triggers the low frequency radio emission Io orbital period is about 42 hours. Jupiter rotational period is about 10 hours. Because of the fast rotation, the magnetic field of Jupiter sweep pass Io and induce an electric field in the satellite. This electric field accelerate the electrons. The electrons go down toward the planet in spirals along the magnetic field. Some are reflected before the hit the atmosphere and start spiraling back away from the planet and emit the low radio frequency. Io torus Electrons spiraling down in Io flux tube What causes the volcanic activities in Io?

10 The elliptical orbit of Io Tidal Heating Io is squished and stretched as it orbits Jupiter. This process releases heat and rises the internal temperature Why is its orbit so elliptical?

11 The Jovian Moons Elliptical orbit: Orbital resonance between the orbital periods of Io, Europa and Ganymede The 3 closest satellites line up every 7 Earth days (resonance) Tugging in the same direction distorts the orbit from a circle to an ellipse 1 orbit of Ganymede = 2 orbits of Europa = 4 orbits of Io

12 Smooth Europa Icy surface covering a large rocky core: Surface is very smooth & young. Fractured into ice rafts & floes a few kilometers across, Repaved by water or geysers through the cracks in the ice. Just a few impact craters: Young surface

13 Europa Surface is ice covered Extensive & complex network of cracks in icy crust. The darker color of the cracks is due to the salts dissolved in the water coming from below the crust Indications of internal geologic activity

14 Europa ( a 200 km square area)

15 Europa Salty water oceans below a thick layer of ice? (twice as much water as Earth!!) Mostly salty water, some magnesium sulfate, sulfurs (red color)

16 Tidal stresses crack Europa s surface ice. Similar to icebergs, large chunks of ice that have been broken and reassembled

17 Does Europa have liquid water? What lies beneath Europa s frozen crust surface? One possibility: km of convective ice above a rocky core The most probably scenario based on measurement of Europa s magnetic field: Thin ice crust a few km thick over a 100 km deep water ocean. (Diameter of Europa=3138 km) The liquid conductive layer distort the magnetic field around Europa. That distortion was detected by the Galileo spacecraft.

18 Europa How Europa can maintain liquid water? Tidal heating due to the elliptical orbit of Europa around the large mass of Jupiter Thermal vents may bring the heat from the core Heat may keep the interior temperature above freezing point Possibility of life? The existence of liquid water does not imply the emergence of life. The salty water is a hostile environment. But we have seen on Earth that life can be present in environment that were considered hostile

19 Titan Saturn s largest satellite Properties: Second largest satellite in Solar System Mass: ~0.02 Earthmass Radius: 0.4 R Earth Density: ~1.9 g/cm³ (1900 kg/m³) Icy mantle over a rocky core. This is the only satellite (moon) in the solar system that has a heavy atmosphere

20 Titan Titan is the only satellite in the solar system to have a permanent atmosphere. It has a methane-ammonia atmosphere The last spacecraft to explore Titan was Cassini (It was commanded to enter and burn in the atmosphere of Saturn in Sept. 2017). The Huygens probe relased from Cassini landed on it surface. Rocky surface and evidence of erosion by liquid/slush. The atmosphere is thick, the surface of Titan cannot be seen in the visual part of the spectrum. On the right, an IR image taken by Cassini s telescopes

21 Titan s Thick Atmosphere Surface temperature: 94 K (-290 F) Pressure: 1.5 bar (1.5 times sea level Earth pressure) Composition: ~98% N 2 (nitrogen) ~2% CH 4 (methane) Argon Hydrocarbons: Ethane = C 2 H 6 Acetylene = C 2 H 2 Ethylene = C 2 H 4 Propane = C 3 H 8 Clouds of methane & N 2 ices More recently, using Cassini instruments: Detection of hydrogen cyanide (CHN) and Benzene (C 6 H 6 ) in clouds in the atmosphere Also using ALMA data: Detection of acrylonitrite (vinyl cyanide, CH 2 CHCN) (possible cell membranes?) in the atmosphere

22 Titan s Atmosphere (Deduced from Voyager 1 spacecraft observation)

23 The Huygens probe The Huygens lander was carried by the Cassini spacecraft mission. The image to the right is an actual image from the surface of Titan returned by the Huygens probe. Colors are close to true colors. Rocks are probably icy rocks

24 The methane/ethane lakes in Titan. Radar images taken by Cassini

25 Lakes on Titan (radar maps) Titan s Liquid Lakes Cassini radar have been able to image several smooth regions that have been identified as lakes of liquid methane/ethane

26 Titan, a reflection of sunlight in a methane lake. (Image taken by Cassini spacecraft)

27 Titan interior Model of the interior deduced from gravitational field measurements during the numerous Cassini flybys. A layer of liquid water under the ice combined with very complex organic molecules make it interesting. Possibility of life?

28 Enceladus (Saturn s satellite) Jets of water gas triggered by hydrothermal vents: Possibility of life?

29 Saturn s satellite Mimas and Star Wars Death Star Image returned by Voyager spacecraft in 1980 (Fly-by) Star Wars movie released in 1977

30 Triton Triton - Neptune s largest moon It has a retrograde orbit. It orbits in direction opposite to Neptune rotation Probably a captured object from the Kuiper belt. Pluto is a Kuiper belt object Voyager 2 detected geysers of nitrogen gas rising several km high The jets of nitrogen gas may come from liquid nitrogen heated by some internal source of heat A very thin atmosphere of nitrogen Temperature about 37 K

31 Rings All of the Jovian planets have rings The most spectacular are Saturn s rings They are very thin, just a few km Rings are not solid objects They are comprised of many small solid particles All the particles are in orbit around the planet Water ice is the primary constituent Why do rings form? The tidal forces of the large planet break apart a close enough moon or satellite

32 Rings Rings consist of billions of small particles or moonlets orbiting close to their planet The size of particle ranges from the size of grain of sand to house-sized boulders

33 Rings The orbits of the particles that make up the rings follow Kepler s laws inner particles revolve faster than those farther out ring are not rotating as a solid body, rather individual moonlets are revolving around the planet If ring particles are widely spaced, they move independently If the particles are close to each other, there is a gravitationally interaction between them The gravitational attraction (resonance) of the satellites (or moons) clear gaps in rings

34 Saturn and its main rings (False colors) The Cassini division is caused by a resonance with the orbital period of Mimas, one of Saturn s satellites The Cassini division is easily visible with a moderate size telescope. It can be seen with any of the 8 or bigger telescopes at the UF Teaching observatory

35 Saturn s ring in false colors to enhance the composition

36 A recent image of Saturn and its rings taken by the Cassini spacecraft (October 2013)

37 An image of Saturn s rings taken by Cassini spacecraft when Saturn eclipsed the Sun in 2006 It shows a set of faint rings outside the main rings (The pale blue dot at 9-10 o clock is the Earth)

38 Origin of Rings Breakup of shattered satellite Remains of particles that were unable to come together and form satellite Gravity plays important role differential force of gravity -- tidal forces tear bodies apart inhibit loose particles from coming together

39 The differential force of gravity: Tidal effect DF g DF g

40 The Roche Limit Roche Limit - the closest distance an object can come to another large mass object without being pulled apart by tidal forces Roche limit

41 Roche Limit If the density of the planet is similar to the density of the satellite (moon) Then, the Roche limit = R planet A large moon orbiting inside the Roche limit will be destroyed. Roche Limits for some planets: Earth - 18,470 km (Distance to Moon =385,000 km ) Jupiter - 175,000 km Saturn - 147,000 km Uranus - 62,000 km For comparison, Saturn outer diameter of A ring is 137,000. It is inside the Roche limit (D is Density)

42 Comparing Jovian Ring Systems Compared to Saturn, the ring system of other Jovian planets: have fewer particles are smaller in extent have darker particles The rings of Uranus were discovered in 1977 when the planet passed in front of a star and the rings dimmed the light from the star The rings of Jupiter and Neptune were discovered by the Voyager spacecrafts Other unsolved mysteries regarding rings: Uranus rings are eccentric and slightly tilted from its equatorial plane. Neptune has partial rings.

43 The Roche limit of the Jovian planets (Distance of the rings from the planets, in planets radius)

44 Pluto, a dwarf planet Discovered in 1930 by Clyde Tombaugh (at Lowell observatory) Pluto is located about 40 times the Earth s distance from the Sun (40AU) Charon, the first satellite discovered was found in Image taken with ground-based telescope Pluto has a total of 5 satellites The New Horizons mission launched in January 2006 arrived in July 14, 2015 (Fly-by). Similar in mass and size to Neptune s large moon Triton Probably formed in the Kuiper belt (comet birth place) The Kuiper belt is located outside the orbit of Neptune, at distances between AU Pluto has a highly inclined orbital plane Orbital period 248 years Average density 2000 kg/m³ Pluto has only 20% the mass of our Moon Mass about mass of Earth Diameter 1160 km, 0.18 diameter of Earth In 2003 it was renamed as a dwarf planet by the International Astronomical Union (IAU) Hubble ST image of Pluto

45 A recent Hubble telescope image of Pluto and its 5 satellites The name of the satellite P4 is Kerberos. Satellite P5 was discovered in 2012and was named Styx. The International Astronomical Union (IUA) is the organization that names celestial objects such as satellites, asteroids, exoplanets. stars, etc

46 Modeled images of Pluto obtained by processing 24 images taken by the Hubble Space Telescope. The process produced a mathematical description of its surface

47 Recent images of Pluto from the New Horizon spacecraft The New Horizons mission arrived at Pluto on July 14, 2015 (Fly by). It took about 10 years to make the trip. It is the first spacecraft to reach Pluto. It has been returning the first detailed images of Pluto. Tombaugh Regio ( The Heart ) (Named after Clyde Tombaugh, Pluto discover). The surface of Pluto shows few impact craters. Almost no craters in the Tombaugh Regio

48 New Horizon image of Sputnik Planum Sputnik Planum shows no impact craters. Its surface must be younger than 10 millions years old Region showing some impact craters

49 Details of Pluto surface. Images from New Horizon This structures cause by convection of nitrogen ice

50 Pluto haze layers and foggy hazes About a dozen haze layers in the atmosphere above Pluto surface. The atmosphere extend for about 40 km. Composition of atmosphere: nitrogen, carbon monoxide, methane Blue skies. The sunlight scattered in the atmosphere of Pluto produces a halo of bluish color The image was taken when the spacecraft passed in front of Pluto and the Sun was being occulted by Pluto

51 An image of Charon from the New Horizon spacecraft Darker, reddish color in North pole Probably the South pole may be similar

52 Kuiper belt Located outside the orbit of Neptune A region of the solar system located between AU from the Sun Bodies in the Kuiper belt are composed of ices, mainly methane, ammonia and water ices. Pluto, Eris, Makemake and Haumea are examples of Kuiper belt objects Some short period comet (Periods<200 years) are also object that belong to the Kuiper belt. The Kuiper belt

53 Kuiper Belt Objects (plutoids) compared The discovery of Eris in 2005 showed that Pluto was not unique. These objects, along with Pluto and others, seem to be the largest of the Kuiper Belt objects, also known as trans-neptunian objects or plutoids. Several hundred have been found. It is estimated that several thousands may form the Kuiper belt Eris also has a satellite. The composition of these objects is mainly ices. Their composition is different from the composition of the terrestrial and Jovian planets

54 A possible ninth planet The object that was nicknamed Ninth Planet is about 10 times the mass of the Earth. The distance from the Sun is about 20 times farther than Neptune. It is estimated than it will take 10,000 to 20,000 years to orbit the Sun Caltech astronomers Konstantin Batygin (right) and Mike Brown found evidence of the ninth planet by modeling the orbits of several objects located beyond the Kuiper belt. In order to account for the distorted and high eccentric orbits of these 6 objects, it is required the existence of an object with 10 times the mass of the Earth and located in the modeled orbit. The results were published in the January 20, 2016 issue of the Astronomical Journal

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