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GEOL3045: Planetary Geology. Lysa Chizmadia Mercury From Mariner 10 to Messenger. Closest planet to Sun 5.8 x 10 7 km (0.38 AU) Diameter = 4880 km Smaller than Ganymede & Titan Mass = 3.3 x 10 23 kg Surface T: 90-700 K 3:2 resonance with the Sun 3 rotations for every 2 orbits - PowerPoint PPT Presentation
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GEOL3045: Planetary Geology
GEOL3045: Planetary Geology
Lysa ChizmadiaMercury
From Mariner 10 to Messenger
Lysa ChizmadiaMercury
From Mariner 10 to Messenger
IntroductionIntroduction Closest planet to Sun
5.8 x 107 km (0.38 AU)
Diameter = 4880 km Smaller than Ganymede &
Titan
Mass = 3.3 x 1023 kg Surface T: 90-700 K 3:2 resonance with the
Sun 3 rotations for every 2
orbits 88 days and 59 days
Closest planet to Sun 5.8 x 107 km (0.38 AU)
Diameter = 4880 km Smaller than Ganymede &
Titan
Mass = 3.3 x 1023 kg Surface T: 90-700 K 3:2 resonance with the
Sun 3 rotations for every 2
orbits 88 days and 59 days
Image from: http://www.nineplanets.org/mercury.html
Orbit highly eccentric Aphelion = 70 million
km Perihelion = 46
million km
Irregularities in orbit Thought to be Vulcan Supports general
theory of relativity
Orbit highly eccentric Aphelion = 70 million
km Perihelion = 46
million km
Irregularities in orbit Thought to be Vulcan Supports general
theory of relativity
Mercury vs. MoonMercury vs. Moon Similarities
Heavily cratered Old surfaces w/
smooth terrains Caloris basin simliar
to Lunar Maria Craters near poles
in permanent shadow Radar data suggest
ice in N pole craters
Similarities Heavily cratered Old surfaces w/
smooth terrains Caloris basin simliar
to Lunar Maria Craters near poles
in permanent shadow Radar data suggest
ice in N pole craters
Differences Mercury has much higher
density 5.43 vs. 3.34 g/cm3
2nd densest body in solar system Indicates very large Fe core
1800-1900 km ~75% volume
w/ very thin silicate crust 500-600 km
Very thin atmosphere From solar wind
Differences Mercury has much higher
density 5.43 vs. 3.34 g/cm3
2nd densest body in solar system Indicates very large Fe core
1800-1900 km ~75% volume
w/ very thin silicate crust 500-600 km
Very thin atmosphere From solar wind
Image from: http://en.wikipedia.org/wiki/Mercury_%28planet%29
Mariner 10Mariner 10
Launched in 1974 3 orbits in 2 years Mapped 45% of surface Discovered escarpments
100’s km high From surface shrinkage of ~0.1% (~1 km)
Reanalysis suggests recent volcanism More data needed to confirm
Launched in 1974 3 orbits in 2 years Mapped 45% of surface Discovered escarpments
100’s km high From surface shrinkage of ~0.1% (~1 km)
Reanalysis suggests recent volcanism More data needed to confirm
Image from: http://www.nineplanets.org/spacecraft.html#marin10
MessengerMessenger Launched in 3 Aug 2004 Will orbit starting in 2011
~March 18th First fly by January 2007
Launched in 3 Aug 2004 Will orbit starting in 2011
~March 18th First fly by January 2007
Images from: http://messenger.jhuapl.edu/gallery/sciencePhotos/view.php?gallery_id=2
Previously unseen side
Matisse Crater
Surface Spectra
MessengerMessenger
Designed to answer following questions: Mercury’s high density Geological history Nature of magnetic field Structure of core Whether there really is ice are poles Determine source of tenuous
atmosphere
Designed to answer following questions: Mercury’s high density Geological history Nature of magnetic field Structure of core Whether there really is ice are poles Determine source of tenuous
atmosphereImage from: http://en.wikipedia.org/wiki/MESSENGER
SummarySummary Mercury closest to Sun
3:2 resonance with Sun Highly eccentric orbit
Confirms general relativity
Similar to Moon Heavily cratered & smooth terrains
Different from Moon Tenuous atmosphere High density Large FeNi core
Mercury closest to Sun 3:2 resonance with Sun
Highly eccentric orbit Confirms general relativity
Similar to Moon Heavily cratered & smooth terrains
Different from Moon Tenuous atmosphere High density Large FeNi core
Formation of Impact Craters
Formation of Impact Craters
Three stages: Three stages:
Images from: http://cmex.ihmc.us/SiteCat/sitecat2/crater.htm
Image from: http://www.chiemgau-impact.com/images/tuetten/image022.jpg
Formation of Complex Craters
Formation of Complex Craters
Images from: http://cache.eb.com/eb/image?id=96799&rendTypeId=4
Crater RaysCrater Rays Filamentus, high-
albedo material Rays are ejecta
from craters
Cratering exercise
Filamentus, high-albedo material
Rays are ejecta from craters
Cratering exerciseImage from: http://www.lpod.org/?page_id=391