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Natural Science II – ERTH 1040 Solar System J. D. Price Sun Mass: 1.9734 E 30 kg He Rot: 25 d Core T: 14 E 6 ºC (22.5 E 6 ºF) Dia: 1.4 E 6 km Comp: 92% H2, 8% Srf T: 5,500o C (9,932o F) Hertzsprung-Russell Diagram Drawing by EB Watson Output The fate of our star Fusion to C Carbon-helium nucleosynthesis All of the elements heavier than H were fused in the stars. Light elements are most abundant, because they are produced first and foremost. Even elements are more abundant because of the fusion effect Above C - late red giant Neutron capture late red giant (s process) Supernova (r process) Solar system Planet density Mass: Mercury 0.33 E 24 kg Venus 4.87 E 24 kg Earth 5.98 E 24 kg Mars 0.64 E 24 kilograms Av. Dia: 4,878 km (3,030 mi) 12,104 km (7,522 mi) 12,753 km (7,926 mi) 6,785 km (4,217 miles) Rot: 58.65 d N 243 d R 24 hrs N 24.6 hrs N Tilt: 0º 177-178o 23o 27” 25o 12" Rev: 0.24 yrs 0.62 yrs 365 days 5 hrs 1.88 years Atmos: none CO2 N2 with O2 CO2 Surface T: -184o C to 427o C 457o C (855o F) -89o C to 57.7o C -129o C to 0o C (-300o F to 800o F) (-128o F to 136o F) ( -200o F to 32o F) Eq. g: 3.7 m/s2 8.8 m/s2 9.8 m/s2 3.7 m/s2 Esc. V. 4.25 km/s 10.36 km/s 11.18 km/s 5.02 km/s Terrestrials r = 6378 km The structure of Earth is thought to be very similar to the rest of the terrestrial planets. ] Iron (w 10% Nickel) core ] Fe-Mg Silicate mantle ] Al Ca / K-Na Silicate crust The magnetic fields of Earth and Mercury may result from the liquid state of their cores. Earth’s Moon Avg. distance = 380,000 km (238,00 mi) Surface •Dust and orange glass – meteoritic impact •Basalt – dark colored rock NASAGalileo •Anorthosite – light colored rock •Breccias – mixed rock •Impact Theory – Mars-sized object strikes Earth, ejects lunar material © 2006, NASA Moon’s composition indicates that formation must occur after partial differentiation of the earth Lunar History • 4.5-3.8 Ga: Molten surface – maybe 100km deep • 3.8-3.1 Ga: Molten interior –radioactive heating, core segregation, lava floods • 3.1 Ga to present: Cold and quiet –, meteorite modification. Earth and Moon Achondrite fragments of the Moon and Mars Not evidence of life Allan Hills 84001 A fragment of Mars found in the Antarctic ice. The concretions generated vigorous debate - but ultimately determined non-biogenic Carbonate concretions Mars topography Rough south, smooth north Twin Peaks The view from Pathfinder, 1997 ©2005, NASA - JPL Spirit’s travels MER-A Spirit Currently, Spirit is crippled by low output from its solar array (Sol 1736) The MER-A Spirit landed 1/4/2004 UTC Images of Mars This approximate true-color image of outcrop dubbed "Longhorn," and behind it, the sweeping plains of Gusev Crater. On the horizon, the rim of Gusev Crater is clearly visible to south. Sol 210 (August 5, 2004). NASA/JPL/Cornell Image Note: SolA_210_P2398_L257_Longhorn (jpg used) Image Credit: The long road Spirits ascent up Husband Hill Image Credit: NASA/JPL/Cornell/OSU/NMU McMurdo Panorama Dark, porous-textured volcanic rocks on Low Ridge. Two rocks to the right of center, brighter and smoother-looking are thought to be meteorites. bright material is evidence of sulfur-rich salty minerals in the subsurface. Sol: 1000 Image credit: NASA/JPL/Cornell Earth-like processes 2nd pass at rock named Mazatal (sol 85). Blue arrow - leftover portions of the outer dark rind. Yellow arrow - bright edges surrounding the rind. Red arrows - crack that may have once contained fluids out of which minerals precipitated. Mazatzal is a highly coated rock: a top coat of dust, a pinking coating, a dark rind and its true interior. The observed area is 3 centimeters (1.2 inches) across. Image Credit: NASA/JPL/USGS/Cornell Image Note: Mazatzal_closeup_RAT2-A087R1 The MER-B Opportunity landed 1/25/04 UTC Opportunity is still going strong (Sol 1709) "Burns Cliff" after driving right to the base of this southeastern portion of the inner wall of "Endurance Crater." The view combines frames taken by Opportunity's panoramic camera between the rover's 287th and 294th sol (Nov. 13 to 20, 2004). Because of this wide-angle view, the cliff walls appear to bulge out toward the camera. In reality the walls form a gently curving, continuous surface. Image Credit: NASA/JPL/Cornell Image Note: Burns_Cliff_L257T-B313R1 MerB Dune structures near Erebus - “color” image from Opportunity Image Credit: NASA/JPL/Cornell Fluid origins Hematite-rich soil includes rounded “blueberries” on plains of Anatolia. Morphology suggested of fluid origins. Image Credit: NASA/JPL/Cornell Phoenix Lander (08) Exploring the polar frost-soil Verified water with Thermal emission mass spec New data on Martian weather Optical and AF microscopic view of samples MSL 2009 Mars Science Laboratory will extend the investigation Eberswalde Crater Delta Gale Crater Holden crater Mawrth Vallis Mountains Lake Oddity Asteroids Smaller fragments of condensed solid matter Most orbit sun between Mars and Jupiter Infrequently impact planets Drawing by EB Watson NEA’s http://near.jhuapl.edu/ http://neo.jpl.nasa.gov/orbits Near Earth Asteroid Rendezvous http://near.jhuapl.edu/ Near Earth Asteroid Rendezvous Feb 12, 2001 A chilling vision of things to come… 2036 potential impact from Asteroid Apophis (d = 390m) April 13, 2029 enters lowearth space (beneath g.s. satellites). But not hit Earth However, the close encounter will influence its path. If it flies through a 600 m area it will hit the Earth in 2036. (1:5,500 chance) This might hurt a bit… Gas giants Interior Natural Satellites (Moons) All planets beyond Venus have moons Jovian moons – earthlike? Io – active volcanism Europa – Dynamic surface of water ice Calisto – Water Ice potentially underlain by liquid water Q: how are moons different from planets New views from Cassini Saturnian Rings Ultraviolet reflectance from rings - blue coloring in image indicates ice (H2O-CO2) Rings are stoney-icey mini-moons trapped in Saturn’s gravitational field. ©2005, NASA - ESA - JPL New views from Cassini Saturnian moons Iapetus Pheobe Rhea ©2005, NASA - ESA - JPL Prometheus (Shepard) Icy Moons - CICLOPS Dione above rings, Saturn’s colors. CICLOPS Titan - Saturn’s largest satellite Distance from Saturn Distance from Sun Diameter (atmosphere) Diameter (surface) Mass Average density Surface temperature Atmos. P at surface Atmos. composition Orbital period 1 221 870 km 1 427 000 000 km (9.54 AU) 5550 km 5150 km 1/45 that of Earth 1.881 times liquid water 94K (-180 degrees C) 1500 mbar (1.5 times Earth's) Nitrogen, methane, traces of ammonia, argon, ethane 15.95 Earth days ©2005, European Space Agency Huygens’ view on the way down Approaching Titan Titan appears to have a dynamic surface. ©2005, European Space Agency Huygens senses the surface Earth-like dendritic stream channels formed by liquid methane What is the source of methane? ©2005, NASA - ESA - JPL Lake-like features Uranus & Neptune Spectral analysis Drawing by EB Watson Kuiper belt objects Charon Pluto Comets Image of C/2002 C1 (Ikeya-Zhang) March 11.77, 2002 UT with deltagraph 300/1000 8 min. Ektachrome 100 film Copyright ©2002 Michael Jager. http://encke.jpl.nasa.gov/Recent_Images.html Concentrated at the edge of solar system (Oort Cloud) A few make closer orbits to the sun Oort cloud Drawing by EB Watson