Life Sustaining What’s needed of stars? Stablility

Life Sustaining

What’s needed of stars?

Stablility

Worthless Stars

Worthless Stars

Unstable

Life Sustaining

What’s needed for stars?

Stablility

Long Life

Worthless Stars

UnstableShort Life

Too Hot

Too Cold

Life Zone

Life ZoneLife Zone Too CloseTidal LockOne Side HotOther Side ColdOne Side Baked DryOther Side GlaciersThin Atmosphere

Life Sustaining

What’s needed for stars?

Stablility

Long Life

Life Zone Far From Star

Worthless Stars

UnstableShort Life

Life Zone Too

Close

Life Zone Too Close

H2

He

CH4 NH3 H2O N2 O2 CO2

2 4 16 17 18 28 32 44

Average Speeds at Room Temperature

0

5

10

15

20

25

30

35

40

45

0 100 200 300 400 500 600 700 800 900

Temperature (Kelvin)

Velo

city

(km

/sec

)

Jupiter

EarthVenus

NeptuneUranus

Saturn

H2

He

CH4 NH3 H2O

Holding an Atmosphere

0

3

6

9

12

15

0 100 200 300 400 500 600 700 800 900

Temperature (Kelvin)

Vel

ocity

(km

/sec

)

EarthVenus

Mars

TitanMercury

CH4 NH3 H2O

N2

O2

CO2

H2

He

Holding an Atmosphere

0

1

2

3

4

5

0 100 200 300 400 500 600 700 800 900

Temperature (Kelvin)

Vel

ocity

(km

/sec

)

Titan

Mercury

Moon

Ceres

PlutoTriton

CH4 NH3 H2ON2

O2

CO2

Holding an Atmosphere

Making Contact

seeds of life

evolution

civilization

technology

Two Types of PlanetsTwo Types of PlanetsTerrestrial

Meteor Craters / Erosion

Smaller

Jovian

Only Clouds Visible

Much Bigger

Wed 9:20

Jovians are BiggerJovians are Bigger

Two Types of PlanetsTwo Types of PlanetsTerrestrial

Meteor Craters / Erosion

Smaller

Rocky

High Density

Jovian

Only Clouds Visible

Much Bigger

Mostly Gas

Low Density

Terrestrials are more DenseTerrestrials are more Dense

Jovians Terrestrials

Jupiter 1.33 g/cm3

Mercury 5.43 g/cm3

Saturn 0.70 g/cm3

Venus 5.24 g/cm3

Uranus 1.30 g/cm3

Earth 5.515 g/cm3

Neptune 1.64 g/cm3

Mars 3.94 g/cm3

Two Types of PlanetsTwo Types of PlanetsTerrestrial

Meteor Craters / Erosion

Smaller

Rocky

High Density

Low Mass

Jovian

Only Clouds Visible

Much Bigger

Mostly Gas

Low Density

High Mass

Jovians are more MassiveJovians are more Massive

Jovians Terrestrials

Jupiter 318 M

Mercury 0.0553 M

Saturn 95 M

Venus 0.8150 M

Uranus 14.5 M

Earth 1 M

Neptune 17 M

Mars 0.1074 M

Two Types of PlanetsTwo Types of PlanetsTerrestrial

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 MoonsJovians have more Moons

Jovians Terrestrials Jupiter 16 Mercury 0

Saturn 23? Venus 0

Uranus 15 Earth 1

Neptune 8 Mars 2

Two Types of PlanetsTwo Types of PlanetsTerrestrial

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.Jovians are farther from the sun.

Jovians Terrestrials Jupiter 5AU Mercury 0.4AU

Saturn 10AU Venus 0.7AU

Uranus 19AU Earth 1AU

Neptune 30AU Mars 1.5AU

What About Pluto?What About Pluto?Plutonoids Pluto

diameter 0.18 Dmass 0.002 M

density 1.97 g/cm3 moons 1

collapse to disk

gravity

centrifugal effect

AccretionAccretionProcess by Which Many Little Things

Become Fewer, Bigger ThingsCondensation

Cold Weld

Tues 12:15

AccretionAccretion

GravityPlanetesimals

Jovian Atmospheres

sweeps up dust while orbitingcollisions slow

orbitspirals in

protosun becomes sunsolar wind clears dust

planetesimals exposed to heat and solar wind

formation limited

no more dust

dust free zone expands

atmosphere reaches escape

velocitysolar wind

blows away atmosphere

planetesimal exposed to heat and solar wind

jovian planet becomes terrestrial

orbit stabilizes

H2

He

CH4 NH3 H2O N2 O2 CO2

2 4 16 17 18 28 32 44

Average Speeds at Room Temperature

0

5

10

15

20

25

30

35

40

45

0 100 200 300 400 500 600 700 800 900

Temperature (Kelvin)

Velo

city

(km

/sec

)

Jupiter

EarthVenus

NeptuneUranus

Saturn

H2

He

CH4 NH3 H2O

Holding an Atmosphere

bombardment

melts surface

heats impact site

Making TerrestrialsMaking Terrestrials

Solar WindLoss of Atmosphere

BombardmentFission

Differentiation

DifferentiationDifferentiation

DifferentiationDifferentiation

DifferentiationDifferentiation

New AtmosphereNew AtmosphereBombardment Slows

Surface HardensMolten Interior

Fission GasOutgassing

CO2 N2 SO2

O2

fissionoutgassing

fissionoutgassing

0

3

6

9

12

15

0 100 200 300 400 500 600 700 800 900

Temperature (Kelvin)

Vel

ocity

(km

/sec

)

EarthVenus

Mars

TitanMercury

CH4 NH3 H2O

N2

O2

CO2

H2

He

Holding an Atmosphere

0

1

2

3

4

5

0 100 200 300 400 500 600 700 800 900

Temperature (Kelvin)

Vel

ocity

(km

/sec

)

Titan

Mercury

Moon

Ceres

PlutoTriton

CH4 NH3 H2ON2

O2

CO2

Holding an Atmosphere

Moon OriginMoon Origin

Fission

Coformation

Capture

Impact

FissionFission

Moon and Earth split

Why?

CoformationCoformation

Moon and Earth formed simultaneously as Binary

Planet

Why is the density different?5.5g/cm3 3.3g/cm3

CaptureCaptureEarth and moon formed far apart

passed close

Earth captured moon

unlikely events required

inclination likely to be high

ImpactImpact

ImpactImpact

ImpactImpact

ImpactImpact

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

CO2 N2

carbon based lifeplant life

photosynthesislimestone

risessaturatedoxidizes

O2

O2

23% 76%

2 O3

3

UV ozone

Wave action dissolves CO2 in ocean.