Bit of Administration …. Bit of Administration …. • Reading • Reading – BSNV Chaps. 9 and 15 BSNV Chaps. 9 and 15 – • No Mathieu office hours today (Monday)! • No Mathieu office hours today (Monday)! • Additional observations for Lab 2, through April 5 • Additional observations for Lab 2, through April 5 – Due April 7 in lecture or April 9 at Mathieu office Due April 7 in lecture or April 9 at Mathieu office – • 12- -week exam in two weeks week exam in two weeks - - April 12, 7:15 pm April 12, 7:15 pm • 12 – Review session, Sunday, April 11, 6:30 pm Review session, Sunday, April 11, 6:30 pm –
The Solar System The Solar System • A Sense of Scale A Sense of Scale • Around Earth Around Europe Distance to Moon = 0.1 = Distance to North America
The Solar System The Solar System • A Sense of Scale A Sense of Scale •
The Solar System The Solar System • A Sense of Scale A Sense of Scale •
The Solar System The Solar System • Inventory Inventory • • Sun Sun 99.85% by mass • 99.85% by mass • Planets 0.1 % by mass Planets 0.1 % by mass • • Satellites and Rings Satellites and Rings • • Asteroids Asteroids • • Comets Comets • • Meteroids Meteroids • • Dust Dust • • Solar Wind (ionized gas) Solar Wind (ionized gas) •
The Solar System The Solar System • Inventory Inventory - - “ “Sedna Sedna” ” •
The Solar System The Solar System • General Characteristics of General Characteristics of Major Major Planets Planets - - Dynamical Dynamical • • Nearly circular orbits (Mercury and Mars most eccentric) Nearly circular orbits (Mercury and Mars most eccentric) •
The Solar System The Solar System • General Characteristics of Major Planets General Characteristics of Major Planets - - Dynamical Dynamical • • Nearly circular orbits (Mercury and Mars most eccentric) Nearly circular orbits (Mercury and Mars most eccentric) • o of Earth’s orbital plane • All orbit within 10 All orbit within 10 o of Earth’s orbital plane •
The Solar System The Solar System • General Characteristics of Major Planets General Characteristics of Major Planets - - Dynamical Dynamical • • Nearly circular orbits (Mercury and Mars most eccentric) Nearly circular orbits (Mercury and Mars most eccentric) • o of Earth’s orbital plane • All orbit within 10 All orbit within 10 o of Earth’s orbital plane • • All revolve in the same direction All revolve in the same direction • • All rotate in the same direction (except Venus) All rotate in the same direction (except Venus) •
The Solar System The Solar System • General Characteristics of Major Planets General Characteristics of Major Planets - - Radius Radius •
The Solar System The Solar System • General Characteristics of Major Planets General Characteristics of Major Planets - - Age Age • • Earth Earth - - Oldest rocks 3.9 billion yr (4.5 billion yr inferred) Oldest rocks 3.9 billion yr (4.5 billion yr inferred) • • Moon Moon - - 4.5 billion yr 4.5 billion yr • • Meteorites Meteorites - - 4.6 billion yr 4.6 billion yr • • Sun Sun - - 4.6 billion (theoretical) 4.6 billion (theoretical) • • Universe Universe - - 12 billion yr 12 billion yr •
The Solar System The Solar System • General Characteristics of Major Planets General Characteristics of Major Planets - - Physical Properties Physical Properties • Terrestrial Terrestrial 7 Giant Satellites 7 Giant Satellites Jovian Jovian Location Inner Location Inner Outer Outer Outer Outer 4 km) 5 km) Size Small (10 4 Size Small (10 km) Small (4000 km) Small (4000 km) Large (10 5 Large (10 km) Mass 0.1 - Mass 0.1 - 1.0 1.0 M M Earth 0.01 0.01 M M Earth 15 - 15 - 300 300 M M Earth Earth Earth Earth Density 5 gm cm - Density 5 gm cm -3 3 2- 2 -3 gm cm 3 gm cm - -3 3 1 gm cm - 1 gm cm -3 3 Appearance Rock with craters, Appearance Rock with craters, Rock, ice with craters, Rock, ice with craters, Gaseous, with Gaseous, with volcanos volcanos volcanos volcanos rock cores rock cores Composition Heavy elements Composition Heavy elements Heavy elements, ices Heavy elements, ices Hydrogen, helium Hydrogen, helium Notes: Notes: 1) Densities: Rock = 3 gm cm - -3 3 , Water = 1 gm cm , Water = 1 gm cm - -3 3 1) Densities: Rock = 3 gm cm 2) Composition of Sun and Universe by numbers of atoms: 2) Composition of Sun and Universe by numbers of atoms: 94% H, 6% He, 2% all else 94% H, 6% He, 2% all else Jupiter Saturn Uranus Nepture Mercury Venus Io Europa Ganymede Earth Mars Callisto
The Formation of the Solar System The Formation of the Solar System
The Formation of the Solar System The Formation of the Solar System • Interstellar Clouds Interstellar Clouds • By Mass Mass By • 73% Molecular Hydrogen 73% Molecular Hydrogen • • 25%Atomic Helium 25%Atomic Helium • • 2% Dust (Metals) 2% Dust (Metals) •
ConcepTest! ! ConcepTest The Taurus clouds are thought to be rather cold, with The Taurus clouds are thought to be rather cold, with temperatures of perhaps 30 K. If you wanted to test this temperatures of perhaps 30 K. If you wanted to test this hypothesis by looking for light emitted emitted by the Taurus clouds, in by the Taurus clouds, in hypothesis by looking for light what wavelength would you want to observe? what wavelength would you want to observe? A) X- -ray ray A) X B) Ultraviolet B) Ultraviolet C) Optical C) Optical D) Infrared D) Infrared E) Radio E) Radio
The Formation of the Solar System The Formation of the Solar System • Dense Molecular Cores Dense Molecular Cores • (“Bok Bok Globules”) Globules”) (“ • ≈ 1 M ≈ 1 M o • o • ≈ 50,000 AU ≈ 50,000 AU • • ≈ 10 ≈ 10 o o K K •
The Formation of the Solar System The Formation of the Solar System
The Formation of the Solar System The Formation of the Solar System • Protoplanetary Protoplanetary Disks Disks • • ≈ 0.01 M ≈ 0.01 M o • o • ≈ 100 AU ≈ 100 AU • • ≈ 3000 ≈ 3000 - -> 10 > 10 o K • o K
The Formation of the Solar System The Formation of the Solar System
The Formation of the Solar System The Formation of the Solar System • Condensation Sequence Condensation Sequence • • Condensation Temperature Condensation Temperature • Temperature at which Solid Gas Temperature at which Solid Gas T > 50 o o K K T > 200 T > 200 o o K K T > 1000 T > 1000 o o K K T > 50 Hydrogen (H) Hydrogen (H) Gas Gas Gas Helium (He) Helium (He) H 2 0, Methane (CH 4 ) H 2 0, Methane (CH 4 ) Ice Gas Gas CO 2 , Ammonia (NH 3 ) CO 2 , Ammonia (NH 3 ) Iron (Fe), Silicon (Si Si) ) Iron (Fe), Silicon ( Rock Rock Gas Metal Compounds Metal Compounds
The Formation of the Solar System The Formation of the Solar System • Condensation Sequence Condensation Sequence • V E M J M 1000 K 200 K Rock Rock, Ice No Grains Grains Grains
The Formation of the Solar System The Formation of the Solar System
The Formation of the Solar System The Formation of the Solar System • Grain Grain Collisions Collisions ==> ==> Planetesimals Planetesimals (100 km) (100 km) • random random 100 km 100 km
The Formation of the Solar System The Formation of the Solar System • Planetesimal Planetesimal Accretion Accretion ==> ==> Rocky Planets and Rocky Planets and Jovian Jovian Cores Cores • gravity gravity
The Formation of the Solar System The Formation of the Solar System • Gas Gas Accumulation Accumulation ==> ==> H and He onto H and He onto Jovian Jovian Cores Cores • gravity gravity Protomoons Protomoons
ConcepTest! ! ConcepTest Most comets have orbits that take them well beyond Jupiter. You Most comets have orbits that take them well beyond Jupiter. You would expect their composition to be: would expect their composition to be: A) Rocks and heavy elements only A) Rocks and heavy elements only B) Rocks and ices only B) Rocks and ices only C) Rocks, ices, and hydrogen and helium C) Rocks, ices, and hydrogen and helium
The Formation of the Solar System The Formation of the Solar System
The Formation of the Solar System The Formation of the Solar System • Dispersal of Hydrogen and Helium Gas Dispersal of Hydrogen and Helium Gas • • Solar Wind? Solar Wind? • • Jets? Jets? •
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