Bit of Administration …. ReadingReading –BSNV Chaps. 9 and 15 No Mathieu office hours today...
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Transcript of Bit of Administration …. ReadingReading –BSNV Chaps. 9 and 15 No Mathieu office hours today...
Bit of Administration ….Bit of Administration ….• ReadingReading
– 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 5Additional observations for Lab 2, through April 5– Due April 7 in lecture or April 9 at Mathieu officeDue April 7 in lecture or April 9 at Mathieu office
• 12-week exam in two weeks - April 12, 7:15 pm12-week exam in two weeks - April 12, 7:15 pm– Review session, Sunday, April 11, 6:30 pmReview session, Sunday, April 11, 6:30 pm
The Solar SystemThe Solar System
• A Sense of ScaleA Sense of Scale
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Around Earth
Distance to Moon= 0.1=
Around Europe
Distance to North America
The Solar SystemThe Solar System
• A Sense of ScaleA Sense of Scale
The Solar SystemThe Solar System
• A Sense of ScaleA Sense of Scale
The Solar SystemThe Solar System
• InventoryInventory
• SunSun 99.85% by mass99.85% by mass• Planets 0.1 % by massPlanets 0.1 % by mass• Satellites and RingsSatellites and Rings• AsteroidsAsteroids• CometsComets• MeteroidsMeteroids• DustDust• Solar Wind (ionized gas)Solar Wind (ionized gas)
The Solar SystemThe Solar System• Inventory - “Sedna”Inventory - “Sedna”
The Solar SystemThe Solar System
• General Characteristics of General Characteristics of MajorMajor Planets - Dynamical Planets - Dynamical
• Nearly circular orbits (Mercury and Mars most eccentric)Nearly circular orbits (Mercury and Mars most eccentric)
The Solar SystemThe Solar System
• General Characteristics of Major Planets - DynamicalGeneral Characteristics of Major Planets - Dynamical
• Nearly circular orbits (Mercury and Mars most eccentric)Nearly circular orbits (Mercury and Mars most eccentric)• All orbit within 10All orbit within 10oo of Earth’s orbital plane of Earth’s orbital plane
The Solar SystemThe Solar System• General Characteristics of Major Planets - DynamicalGeneral Characteristics of Major Planets - Dynamical
• Nearly circular orbits (Mercury and Mars most eccentric)Nearly circular orbits (Mercury and Mars most eccentric)• All orbit within 10All orbit within 10oo of Earth’s orbital plane of Earth’s orbital plane• All revolve in the same directionAll revolve in the same direction• All rotate in the same direction (except Venus)All rotate in the same direction (except Venus)
The Solar SystemThe Solar System
• General Characteristics of Major Planets - RadiusGeneral Characteristics of Major Planets - Radius
The Solar SystemThe Solar System
• General Characteristics of Major Planets - AgeGeneral Characteristics of Major Planets - Age
• Earth - Oldest rocks 3.9 billion yr (4.5 billion yr inferred)Earth - Oldest rocks 3.9 billion yr (4.5 billion yr inferred)• Moon - 4.5 billion yrMoon - 4.5 billion yr• Meteorites - 4.6 billion yrMeteorites - 4.6 billion yr• Sun - 4.6 billion (theoretical)Sun - 4.6 billion (theoretical)• Universe - 12 billion yrUniverse - 12 billion yr
The Solar SystemThe Solar System• General Characteristics of Major Planets - Physical PropertiesGeneral Characteristics of Major Planets - Physical Properties
TerrestrialTerrestrial
Location InnerLocation InnerSize Small (10Size Small (1044 km) km)Mass 0.1 - 1.0 MMass 0.1 - 1.0 MEarthEarth
Density 5 gm cmDensity 5 gm cm-3-3
Appearance Rock with craters,Appearance Rock with craters, volcanosvolcanosComposition Heavy elementsComposition Heavy elements
7 Giant Satellites7 Giant Satellites
OuterOuterSmall (4000 km)Small (4000 km)0.01 M0.01 MEarthEarth
2-3 gm cm2-3 gm cm-3-3
Rock, ice with craters,Rock, ice with craters,volcanosvolcanosHeavy elements, icesHeavy elements, ices
JovianJovian
OuterOuterLarge (10Large (1055 km) km)15 - 300 M15 - 300 MEarthEarth
1 gm cm1 gm cm-3-3
Gaseous, withGaseous, withrock coresrock coresHydrogen, heliumHydrogen, helium
Mercury Venus Earth Mars
Jupiter Saturn Uranus Nepture
Notes:Notes:
1)1) Densities: Rock = 3 gm cmDensities: Rock = 3 gm cm-3-3, Water = 1 gm cm, Water = 1 gm cm-3-3
2)2) Composition of Sun and Universe by numbers of atoms: Composition of Sun and Universe by numbers of atoms: 94% H, 6% He, 2% all else94% H, 6% He, 2% all else
Io Europa Ganymede Callisto
The Formation of the Solar SystemThe Formation of the Solar System
The Formation of the Solar SystemThe Formation of the Solar System
• Interstellar CloudsInterstellar Clouds
By By MassMass • 73% Molecular Hydrogen73% Molecular Hydrogen• 25%Atomic Helium25%Atomic Helium• 2% Dust (Metals)2% Dust (Metals)
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 hypothesis by looking for light emittedemitted by the Taurus clouds, in by the Taurus clouds, in what wavelength would you want to observe? what wavelength would you want to observe?
A) X-rayA) X-ray B) UltravioletB) Ultraviolet C) OpticalC) Optical D) InfraredD) Infrared E) RadioE) Radio
ConcepTest!ConcepTest!
The Formation of the Solar SystemThe Formation of the Solar System
• Dense Molecular CoresDense Molecular Cores (“Bok Globules”)(“Bok Globules”)
• ≈ ≈ 1 M1 Moo
• ≈ ≈ 50,000 AU50,000 AU• ≈ ≈ 10 10 ooKK
The Formation of the Solar SystemThe Formation of the Solar System
The Formation of the Solar SystemThe Formation of the Solar System
• Protoplanetary DisksProtoplanetary Disks
• ≈ ≈ 0.01 M0.01 Moo
• ≈ ≈ 100 AU100 AU• ≈ ≈ 3000 -> 10 3000 -> 10 ooKK
The Formation of the Solar SystemThe Formation of the Solar System
The Formation of the Solar SystemThe Formation of the Solar System• Condensation SequenceCondensation Sequence
• Condensation Temperature Condensation Temperature Temperature at which Solid Gas Temperature at which Solid Gas
T > 50 T > 50 ooK T > 200 K T > 200 ooK T > 1000 K T > 1000 ooKK
Hydrogen (H)Hydrogen (H)Helium (He)Helium (He)
HH220, Methane (CH0, Methane (CH44))
COCO22, Ammonia (NH, Ammonia (NH33))
Iron (Fe), Silicon (Si)Iron (Fe), Silicon (Si)Metal CompoundsMetal Compounds
Gas Gas Gas
Ice Gas Gas
Rock Rock Gas
The Formation of the Solar SystemThe Formation of the Solar System• Condensation SequenceCondensation Sequence
1000 K 200 KRock
GrainsRock, Ice
GrainsNo Grains
M M JEV
The Formation of the Solar SystemThe Formation of the Solar System
The Formation of the Solar SystemThe Formation of the Solar System• Grain Grain CollisionsCollisions ==> Planetesimals (100 km) ==> Planetesimals (100 km) randomrandom
100 km100 km
The Formation of the Solar SystemThe Formation of the Solar System
• Planetesimal Planetesimal AccretionAccretion ==> Rocky Planets and Jovian Cores ==> Rocky Planets and Jovian Cores gravitygravity
The Formation of the Solar SystemThe Formation of the Solar System
• Gas Gas AccumulationAccumulation ==> H and He onto Jovian Cores ==> H and He onto Jovian Cores gravitygravity
ProtomoonsProtomoons
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 onlyA) Rocks and heavy elements only B) Rocks and ices onlyB) Rocks and ices only C) Rocks, ices, and hydrogen and heliumC) Rocks, ices, and hydrogen and helium
ConcepTest!ConcepTest!
The Formation of the Solar SystemThe Formation of the Solar System
The Formation of the Solar SystemThe Formation of the Solar System
• Dispersal of Hydrogen and Helium GasDispersal of Hydrogen and Helium Gas• Solar Wind?Solar Wind?• Jets?Jets?