Marsa 1.5 AU

P 687 d

i (orb) 2o

e 0.09

Prot 1.02 d

i (rot) 25o

R 0.6 RE

M 0.11 ME

3.9 g/cc

g 0.29 gE

vesc 5 km/s

A 0.15

Moons of MarsPhobos Deimos

a = 9380 km 23,500 km

P = 0.32 d 1.26 d

e = 0.02 0.002

Prot = 0.32 d 1.26 d

dim = 27 x 19 km 15 x 11 km

= 1900 2100

vesc = 0.011 km/s 0.006 km/s

A =0.05 0.05

Exploration of Mars• ~1800: Herschel and others discover ice caps and

clouds• 1877: Phobos and Deimos discovered; also Schiaparelli

(It.) refers to ‘canali’• 1890’s: Lowell interprets markings as canals, implying

intelligent Martian life• 1965 Jul: 1st close-up photos by Mariner 4• 1971 Nov: 1st orbital probe in Mariner 9• 1976 Jul: Viking 1 lander – no life• 1997 Jul: Mars Pathfinder• 1997 Sept: Mars Global Surveyor• 2001 Oct: Mars Odyssey • 2004 Jan: Spirit (Rover)• 2006: Mars Reconnaissance Orbiter• 2007: Phoenix lander• 2013: Mars Orbiter Mission (India)

Martian Travel Brochure

The Martians are Coming!

Percival Lowell’s Martian “Canals”

Lowell’s Surface ID’s

Properties of Mars• Iron core of 1500 km in radius• Low magnetic field (about 0.1% of Earth’s),

because molten core has largely cooled• Resurfacing from past volcanic activity• Polar caps of dry ice• No surface water• Thin CO2 atmosphere• Red coloration from oxidized iron minerals

Principal Surface Regions

Views of Mars

Impact Aided Atmospheric Losses?

Crater Distribution at Mars

Victoria Crater

Olympus Mons

The Face at Mars

Cape Verde

Martian Terrain: Dunes

Dry River Beds and Channels

Run-Off of Water?

Water on Mars• Evidence for channels and sea beds (?)• H2O in clouds and polar caps, but only trace• Mars Odyssey implies subsurface water ice

So maybe Mars warmer and wetter in past (even oceans?), and perhaps a lot of that water exists as permafrost below the surface

(although in a warmer Mars, water vapor is close to escaping low gravity of Mars)

Ocean Beds at Mars?!

Martian Weather1) Mars tilt like Earth, hence similar seasons2) Mars has e~0.1, so 10% closer at

perihelion and 10% farther at aphelion S. summer is warmer, receiving 50%

more light compared to N. summer3) Dust storms: greater heating in S. leads

to more convection and lifting of dust; storms can last for several weeks

Understanding Seasons at Mars

Martian Skies

Evolution of the Polar Caps

Methane in the Martian Atmosphere• Methane gas was

recently detected in Mars’ atmosphere using groundbased telescopes

• The methane gas distribution is patchy and changes with time

• Most methane in Earth’s atmosphere is produced by life, raising questions about its origin on Mars

View of Mars colored according to the methane concentration observed in the atmosphere. Warm colors depict high concentrations.

Recent Release of Methane• Methane in the

atmosphere should be destroyed by UV light within a few hundred years

• Methane observed now must therefore have been produced recently

• Variations in space and time suggest that it was recently released from the subsurface in localized areas

UV photons have enough energy to break molecules apart

The Big Picture• Where can the methane

come from? From analogy with Earth, there are two leading theories for the origin of recent subsurface methane at Mars:1. Methane is produced by

water-rock interactions2. Methane is produced by

bacteria, in regions where liquid water is found

Either theory implies that the Martian subsurface is dynamic

• However, Curiosity has so far FAILED to detect any methane

Methane on Mars could be produced chemically through liquid/rock interactions (top) or biologically (bottom)

methane

liquid waterhot rock

surface

methanebacteria

~2 µm

Terrestrial Atmospheres Terrestrials have

secondary atmospheres, which are produced by outgassing from the planet interior

Comets have likely influenced our atmosphere, possibly supplying some water for oceans during an early bombardment era

Atm. Oceans

Mercury --- N

VenusMassive

CO2N

Earth N2, O2 Y

MarsThin CO2

N

Some Details…

o Details of Outgassing: volcanos yield mainly CO2 and H2O

o Comparative Planetology: Venus and Mars have CO2 atmospheres, but not Earth. Earth has oceans, so that the CO2 is in carbonate rocks.

o Why O2 at Earth? Photosynthesis from plants. Earth was O-poor until 2.5 Gyrs ago, and earliest plant fossils are 2 Gyrs old

o Where did H2O go at Venus? Break up water molecules, then escape of H2 gas from planet

Interaction of CO2 and Water

Atmospheres and Phase Diagrams

Changes in the Earth Atmosphere