Life Sustaining What’s needed of stars? Stablility

Worthless Stars

Unstable

Life Sustaining What’s needed for stars? Stablility Long Life

Worthless Stars Unstable Short Life

Too Hot Too Cold Life Zone

Life Zone Life Zone Too Close Tidal Lock One Side Hot Other Side Cold One Side Baked Dry Other Side Glaciers Thin Atmosphere

Life Sustaining What’s needed for stars? Stablility Long Life Life Zone Far From Star

Worthless Stars Unstable Short Life Life Zone Too Close

H2H2 He CH 4 NH 3 H2OH2O N2N2 O2O2 CO Average Speeds at Room Temperature

Jupiter Earth Venus Neptune Uranus Saturn H2H2 He CH 4 NH 3 H 2 O Holding an Atmosphere

Earth Venus Mars Titan Mercury CH 4 NH 3 H 2 O N 2 O 2 CO 2 H2H2 He Holding an Atmosphere

Titan Mercury Moon Ceres Pluto Triton CH 4 NH 3 H 2 O N 2 O 2 CO 2 Holding an Atmosphere

Making Contact seeds of life evolution civilization technology

Two Types of Planets Terrestrial Meteor Craters / Erosion Smaller Jovian Only Clouds Visible Much Bigger Wed 9:20

Jovians are Bigger

Two Types of Planets Terrestrial Meteor Craters / Erosion Smaller Rocky High Density Jovian Only Clouds Visible Much Bigger Mostly Gas Low Density

Terrestrials are more Dense

Two Types of Planets Terrestrial Meteor Craters / Erosion Smaller Rocky High Density Low Mass Jovian Only Clouds Visible Much Bigger Mostly Gas Low Density High Mass

Jovians are more Massive

Two Types of Planets Terrestrial Meteor Craters / Erosion Smaller Rocky High Density Low Mass Few Moons Jovian Only Clouds Visible Much Bigger Mostly Gas Low Density High Mass Many Moons

Jovians have more Moons

Two Types of Planets Terrestrial Meteor Craters / Erosion Smaller Rocky High Density Low Mass Few Moons No Rings Jovian Only Clouds Visible Much Bigger Mostly Gas Low Density High Mass Many Moons Rings

Jovians are farther from the sun.

What About Pluto?

collapse to disk  gravity centrifugal effect

Accretion Process by Which Many Little Things Become Fewer, Bigger Things Condensation Cold Weld

Tues 12:15

Accretion Gravity Planetesimals Jovian Atmospheres

 sweeps up dust while orbiting collisions slow orbit spirals in protosun becomes sun solar wind clears dust planetesimals exposed to heat and solar wind formation limited no more dust

dust free zone expands atmosphere reaches escape velocity solar wind blows away atmosphere planetesimal exposed to heat and solar wind  jovian planet becomes terrestrial orbit stabilizes

H2H2 He CH 4 NH 3 H2OH2O N2N2 O2O2 CO Average Speeds at Room Temperature

Jupiter Earth Venus Neptune Uranus Saturn H2H2 He CH 4 NH 3 H 2 O Holding an Atmosphere

bombardment melts surface heats impact site

Making Terrestrials Solar Wind Loss of Atmosphere Bombardment Fission Differentiation

New Atmosphere Bombardment Slows Surface Hardens Molten Interior Fission  Gas Outgassing CO 2 N 2 SO 2 O2O2

fission outgassing

Earth Venus Mars Titan Mercury CH 4 NH 3 H 2 O N 2 O 2 CO 2 H2H2 He Holding an Atmosphere

Titan Mercury Moon Ceres Pluto Triton CH 4 NH 3 H 2 O N 2 O 2 CO 2 Holding an Atmosphere

Moon Origin Fission Coformation Capture Impact

Fission Moon and Earth split Why?

Coformation Moon and Earth formed simultaneously as Binary Planet Why is the density different? 5.5g/cm 3 3.3g/cm 3

Capture Earth and moon formed far apart passed close Earth captured moon unlikely events required inclination likely to be high

Impact

Sunlight bombards planet. With the right temperature, clouds form from water vapor. Clouds reflect sunlight, lowering temperature. The lower temperature causes more clouds to form.

UV CO 2 N 2 carbon based life plant life photosynthesis limestone rises saturated oxidizes O2O2 O 2 23%76% 2 O 3 3 UV ozone Wave action dissolves CO 2 in ocean.