Download Two distinct types of planets

Physical Properties of Planets
Physical Property of Planets
Density:
- measure of how compressed a substance is
- determined by total mass & volume it occupies
Two distinct types of planets:
Terrestrial Planets (Earth-like)
Jovian Planets (Jupiter-like)
Size:
ρ=
Mass
Volume
Examples:
Water
1.0 g/cm3
Air
0.0013 g/cm3
Styrofoam 0.1 g/cm3
Ice
0.92 g/cm3
Rocks
Lead
Gold
2.5-3.5 g/cm3
12 g/cm3
19 g/cm3
- indicates the composition of object!
Density:
Mass:
Terrestrial Planets:
- large density ("rocky" composition)
Jovian Planets:
- small density ("Gas Giants")
-mostly liquefied gas
Terrestrial Planets:
- small size
- small mass
- large density
- "rocky" composition
- long rotational periods
- hard surfaces with possible atmosphere
-no atmosphere Mercury
-very, very thick atm. Venus
- few, if any moons
Prot:
All 4 Inner Planets
(and some large moons)
No. of Moons:
Mercury
Venus
Earth
Mars
0
0
1
2
Jupiter
Saturn
Uranus
Neptune
Pluto
67+rings
62+rings
27+rings
14+rings
5
Mercury "Spider Crater"
Mercury Global Image
Mercury and Moon comparison
Mercury surface close-up
Venus visual image
Surface of Venus (Venera spacecraft)
Venus Radar Map
Maat Mons volcano from Magellan data
Mars Global Image
Ice on Mars (Phoenix Lander)
Ice on Mars (Phoenix Lander)
Opportunity rover at Endeavour Crater
Subsurface Water on Mars?
Curiosity rover at Gale Crater
Eroded pebbles in sediment = fast flowing water.
Ancient Mars ??
Jovian Planets:
-large size
-large mass
-small density
"Gas Giants"
-mostly liquefied gas
-short rotational periods
-ring systems and many moons
All 4 Large Outer Planets
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiter&Display=Gallery
http://solarsystem.nasa.gov/planets/profile.cfm?Object=Jupiter&Display=Gallery
Jupiter's Rings discovered by Voyager 1
Voyager 1 image of Saturn
(Cassini)
Scattered light seen from behind Saturn (Cassini)
Titan and Epimetheus behind Saturn's rings
Enceladus (300 mi across) in front of Saturn
North Pole of Saturn with “Hexagon”
Saturn in infrared
Recent Storm (2010 - now) on Saturn
Plutonian (Pluto-like) Objects
- Small mass, size
- Small density (mostly ice)
- Very Elliptical orbits with high
high inclinations
- Beyond orbit of Neptune
(Kuiper Belt,
Belt, Oort Cloud)
Cloud)
Neptune's rings (Voyager 2)
Neptune and Triton (Voyager 2)
Plutonian
Plutonian / Dwarf Planets
Name
Eris (2003) *
Pluto (1930)
Makemake (2005)
2007 OR10
Haumea (2004)
Quaoar (2002)
Sedna (2004)
Orcus (2004)
2002 MS4
Salacia
a
68 AU
39 AU
46 AU
67 AU
43 AU
43 AU
530 AU
39 AU
41 AU
42 AU
Formation of the Solar System
Sun, planets and all of solar system
-formed from gravitational collapse
of large cloud of gas & dust
- mostly Hydrogen, Helium
diameter
1450 mi
1430 mi
1200 mi
~800 mi
~780 mi
~700 mi
~650 mi
~610 mi
~600 mi
~575 mi
*
http://www.gps.caltech.edu/~mbrown/planetlila/index.html
http://www.gps.caltech.edu/~mbrown/dwarfplanets/
Name
Varuna (2000)
2013 FY27
2003 AZ84
Varda
Ixion (2001)
Chaos
Likely Candidates
a
43 AU
59 AU
40 AU
46 AU
40 AU
46 AU
Diameter
~475 mi
~475 mi
~465 mi
~430 mi
~420 mi
~380 mi
Properties of Gravitational Collapse
Heating of gas & dust
-gravitational energy released
-increases temperature of cloud
- hotter at center
- cooler at edges
Rotation
-during collapse, rate of rotation
increases
-all parts of the cloud rotate in the
same direction
-causes cloud to flatten into a disk
During Collapse of cloud:
-Three temperature regions
Inner Region:
-temperature rises above 2000oC
-all matter is vaporized
-no solid matter, only free atoms
forms SUN
Midrange Region:
-temperature: 0oC to 2000oC
-heavier elements can form solids
-no light gases or ice (frozen gas)
forms Terrestrial Planets
Outer Region:
-temperature less than 0oC
-heavier elements can form solids
-light gases and ice are present
forms Jovian Planets
http://www.pas.rochester.edu/~joel/papers.html
http://www.pas.rochester.edu/~joel/papers.html