Interiors of Terrestrial Planets. Mercury MEAN RADIUS: 2439.7 km MASS: 0.055 (Earth=1) DENSITY: 5.43 (g/cm^3) GRAVITY: 0.376 (Earth=1) ORBIT PERIOD: 87.97.

Interiors of Terrestrial Planets

Mercury

•MEAN RADIUS: 2439.7 km •MASS: 0.055 (Earth=1) •DENSITY: 5.43 (g/cm^3) •GRAVITY: 0.376 (Earth=1) •ORBIT PERIOD: 87.97 (Earth days) •ROTATION PERIOD: 58.65 (Earth days) •SEMIMAJOR AXIS OF ORBIT: 0.387 au •ECCENTRICITY OF ORBIT: 0.206

The Resonant Rotation of Mercury

Mercury’s large core may indicate a “mantle-stripping” impact with a similar body.

1 solar day =176 Earth days

1 sidereal day=59 Earth days

Venus•MEAN RADIUS: 6051.9 km •MASS: 0.814 (Earth=1) •DENSITY: 5.24 (g/cm^3) •GRAVITY: 0.903 (Earth=1) •ORBIT PERIOD: 224.7 (Earth days) •ROTATION PERIOD: 243.0 R (Earth days) •SEMIMAJOR AXIS OF ORBIT: 0.723 au •ECCENTRICITY OF ORBIT: 0.007

The External Appearance of Venus

Venus in visible light – cloud shrouded

Venus in the ultraviolet – cloud patterns rotate every 4 days.

Radar Maps of Venus

The Magellan probe provided a high resolution elevation map of Venus, with information on reflectivities that indicate textures.

Craters on Venus

Volcanoes on Venus

The Real Surface of VenusActual pictures from the ground -- the Soviet Venera seriesTemperature: 800 degrees, Pressure: 100 atmospheres

Mars•MEAN RADIUS: 3388.0 km •MASS: 0.108 (Earth=1) •DENSITY: 3.94 (g/cm^3) •GRAVITY: 0.380 (Earth=1) •ORBIT PERIOD: 686.98 (Earth days) •ROTATION PERIOD: 1.026 (Earth days) •SEMIMAJOR AXIS OF ORBIT: 1.524 au •ECCENTRICITY OF ORBIT: 0.093

Clouds, Polar Caps, and Odd MarkingsMars presents many different aspects to us. Its weather and terrain are varied and changeable.

Valles Marineris Canyon

The Volcanoes of Mars

Martian Terrains

Dune Fields

Old cratered highlands

Polar Ice fields

Evidence of Water FlowsWater cannot be a liquid on Mars’

surface now, but billions of years ago it flowed (there may even have been seas.

The Surface Desert of Mars

Mars looks like a desert with about the same land area as the Earth. Its pink skies, however, contain far too little pressure to allow outside living.

The Martian Meteorite

This rock IS from Mars.Does it contains signs of life?Stay tuned….

Martian Moons: Phobos and Deimos

Mars’ moons are very small; almost certainly captured asteroids. Phobos orbits in less than a day – retrograde.

The Atmospheres of the Terrestrial Planets

The Greenhouse Effect

1) In equilibrium, a planet must re-radiate all the energy it absorbs.

2) Solar energy tends to be converted from visible to infrared radiation.

3) Some gases are transparent to visible radiation, but opaque to infrared radiation.

4) When radiation is blocked, you need a bigger temperature gradient to push the energy through.

Evolution of Terrestrial Atmospheres

All the terrestrial planets start off with a substantial atmosphere. Mars lost most of it because of low escape speed. Earth converted most of the carbon dioxide into rocks. Life produced free oxygen. Venus lost the water because it stayed vapor (and solar UV released hydrogen).

Summary of the

Terrestrial Planets

These are the “rocky” worlds of our inner solar system. The other large solid bodies in the solar system are all moons of the outer gas giant planets. They were collected by impacts of smaller bodies, and still bear those scars and effects.