°Œķķ=ċ
•!
•!
•!
•!
¶@ķ
ķIøŠM…ò
°Œķž
I'
Mariner Mars images taken in 1960’s
DustĐ
äKIJķŐŏŒT0ĽķSÆI*
(Smith et al. 2004)
•! ½s†ŘŌŞşļIJķvÇĵFţý³Ť
ĞXg¼ĶAćĝłeğĢłŅı
MĶ¢ó
•! 4ÝķT¼0ĥ 0.1-0.5
•! MķŐŏŒûĸŽĀ¼ŠÄĀ¼Ķ
MğĠI*
•! Oā„^ň:3ĦıMķ²­Ķ
ĵń
MŐŏŒķr#
•! Mķ%²­ijĵŃM–ðĶMğĠqĈ
ďk20kmķ«k[K]
–! CO2ķ«Z&”ĸĩęĪę†Ē
–! ĄʼnŜŗœŀ®²%²ķ[Ŀ_ĥę
ŐŏŒL
ŐŏŒ`
ŐŏŒķLęiijīĚIJĵęiIJĕ7ħS
ÆIJĿ40ĒĿķ«kķ÷ęĞĘń
Solar longitudeĔţSÆŤ
Smith et al. (2002)
Radiative-convective equilibrium
Gierasch, P. J., & R. M. Goody (1972)
6Ž
16Ž
6Ž
16Ž
0Ē
Convective boundary layer
•! ďk3-10kmļIJ
•! SÆŀE€ĶŁįıMğĠI*
Radio occultation
Hinson et al., Icarus 198 (2008) 57–66
°ŒķSÆ
!"#$#%#ţ+-·ķŤ
!"#$#)*%#
'+,,#-.#
'+/(#-.#
!"#$#&%#
!"#$#'(%#
•! °ŒĸéèöķăwµĞM
ğęĬľSÆI*ĞÓĦĠ.+
Ć]Á
•! .-·ķJĶOāļIJķçăĞ
ìĠĵń
+•ķSÆI*
Viking 1ĔĔ22N, 48W (1976 ŭĐ1980 i)
Viking 2ĔĔ48N, 225W (1976 ŭĐ1982 i)
Surface
pressure
Meridional distribution of
temperature
«kČŪ
!u g
!p
=
R !T
fp !y
ĔĔĔ+-·ķÀĔĔĔĔĔĔĔĔĔĔĔĔĔĔĐĐĐĐĐĐĐĐĐĐ+-·ķĔĔĔĔĔĔĔĔĔ
«
“ØČ
«
“ØČ
A·ķ]¡>ij~b>ķzãňĩƒİM–ð
Š^ķËkfĐ
_ţ1984Ť
„^Ê;ŽĀ
Ĕ„^Ê;ŽĀūMĞOā„^ĶŁįıĘĬĬļįĬŃ{
Œ„^ň„ĦıěĬŃĨńķĶĝĝńŽĀ
„^Ê;ŽĀĸ{ŒĤijĶ÷Ě
A·ĔŧŦŦŠ
°ŒĔŨŠĔĔĔĐē²ĦŀĨĠľŀĨę
üŒĔũŦiĔĔĐē²ĦĶĠĠľĶĠę
Mķ.+u¸ĶĝĝńŽĀĸŧŦŦŠĠłę
°ŒIJĸu¸ĞĘįıĿMğĵ«kdĞ›ńĖĐ
üŒIJĸu¸ĶŁįı«kĞŁĠĵłĥŅńĖ
ŐŏŒŏŒšřĐ
•! LĠķaA¼ĵŐŏŒŏŒšřĸMܘĵĿķĶ~ÿĦĵę
•! MŐŏŒŏŒšřĞ.-·ĞĝłJķĀĶ»¹ĕĬĭĦ»¹Ħĵęi
ĿĘń
•! MŐŏŒŏŒšřķ»¹ĶĸĕeğĢłŅĬŐŏŒķ„^%²ĶŁįı
ČĞĥłĶn*ĥŅńiję̙ķŖŊšœŕőŌкĦıęńijÍěłŅ
ıęń
Dust devils
•! Source of background
atmospheric dust ?
Global dust storm
°ŒMķÜ!z
–! ōŞšŕŜŐŏŒŏŒšřĞX’»¹
–! hB«ĕ¢óŐŏŒûĞiėI'
°ŒIJķŐŏŒŏŒšř»¹
ķâþţ1905ŭ1990iŤ
Kahre et al. (2005)
Observation by Mars
Global Surveyor
A×ŐŏŒfķÿ’I'Ŭ
2001iķGlobal dust strom"tķ
A×ŐŏŒķH©
©`
H%
Global dust stromķĘij1°ŒiIJķ
ŐŏŒķH©
H%
©`
ţSzwast et al., 2006Ť
Ancient Martian climate
•! ×ćApĝłĕõ1ķĘńŽ’Ķ¥ķž
ĞA×ĶR@ĦıęĬģijĞ¿<ĥŅńĖģ
ķĉķ°Œĸ¥ķžĞA×ĶR@IJğń
ÂkĶ«IJĘįĬijÍěłŅńĖ
•! žĸ¶@ĿŸjijĦıĘńÂk›įıęńĖ
°Œķš5
Jakosky (Nature, 2001)
•! Noachian’ĶĸA×Ķ¥ķžĞR@ĦĬijyŇŅń
Chassefiere et al. (2007)
Remnant crustal
magnetic field
ĐConnerney et al. (2005)
’°ŒĸCO2ķ«Z&”IJļńĝ
Kasting (Icarus, 1991)
•! Oāж@ŁŃ25ސę’ķ°Œ¸GĶĜęıĿĕCO2Ğ,
ĶĘŅĹ0Ē
ňY¶IJğńĝŬ
•! «Z&”IJA×ìĠЏļįıĿÄĸĬęķIJĕCO2ĞÈĨń
ģijňÍ}ĨńxÙĞĘńĖ
•! «Z&”IJA×ìĠķMĞľłŅńij~bĞVXijĵŃ]¡Ğ
¹ħńĖ]¡ĶŁŃƒĮĢłŅĬĝĸˆ²ÎmIJ«kĞĞŃĕ
M~ĞÈĨńĖȲĞMňľńĬľĶďk‰8ķ«k
ĸ_ĥĠěłŅńĖ
•! ģķģijĸA׫kĶĴĚqĈĨńĝŬ
CO2Èķ&”
•! CO2ÈĞåģńĊCIJĸ«k©µĞ_ĥĠĵńĖ
•! ďďkIJ«kĞĞńijĕAםMĝłUWĶ„^ĥŅń²„^Ŗśő
Ōŏň7ħĶİĬľĶĕďkķ«kĸĞńĖ
•! Oānkж@ķ86Ţ
ĭij0ęCO2MIJĿA׫kĸ0Ē
•!Aם? 2 bar
•!¶@ķOānkňX
•!ĄĶŁńOā2^ĸÍěĵę
CO2È
CO2ÈĵĦ
CO2ÈĘŃ
«k
’°ŒķCO2ŸĄĶŁń«Z&”đ
Forget & Pierrehumbert (Science, 1997)
•! CO2ŸĄĸäKÉňŁĠ…ĨńĖīķĬľA×ĝłUWĶ8ġı
»ĩłŅń²„^ň…ĦıA×ĶĦĕ«Z&”ňĿĬłĨĖ
•! CO2ŸĄĸOāĶ]ĨńʼnŜŗœţ2^µŤňMğĠĦıMň
/ĨńğĿĘńĞĕ0ęCO2MķE6ĶĸĿijĿijMīķĿ
ķķʼnŜŗœĞMğęķIJĕCO2ŸĄĞĿĬłĨ«Z&”ĶŁń%
²ķ[Ğ(ńĖ
–! ĬijěĹ2?ķĄ±ĦCO2MĸʼnŜŗœ0.38ňƒİĖģģĶ
CO2ŸĄň%ěıʼnŜŗœĞ0.65ijĵŃOā:3ûĞ40%©
ńijğĕCO2ŸĄĸUWĶıÕĠäK„^ň60%©łĨĖţģ
ķŁĚĵĄĸ4ÝĶ]ĨńT0ĥ10Ķ¾oĨńŤ
2?ķCO2MĕT0ĥ10ķCO2ŸĄĕ¶@ķ°Œ
èöķOāûķ75%ňXĦĬijğķ«k–ð
CO2ŸĄĘŃĕH2OĘŃ
CO2ŸĄĘŃĕ
H2OĵĦ
CO2ŸĄĵĦ
!Ĕ1-2?ķCO2MĞĘŅĹ0Ē
ĶĵŃīĚ
01234#512617#83951:;#<7=;2#1#=;7";2#>?)#1:5@"AB;2;##
CD@2E;:#;:#13+#)%'/F
Mars GCM with 2-bar CO2 atmosphere
average visible opacity ~ 4.5
-!
-!
A CO2 atmosphere could not have raised the annual mean temperature
above 0°C anywhere on the planet. The collapse of the atmosphere into
permanent CO2 ice caps is predicted for pressures higher than 3 bar.
Consistent with a cold early Mars scenario in which nonclimatic
mechanisms must occur to explain the evidence for liquid water.
Polar caps
+•
.•
H2OŸťCO2Ÿ
•! +•Š.•ijĿĕSÆijijĿĶ‚MÌ_
•! J’Ŀ›ń›R•
–! +•IJĸH2OŸķĽ
–! .•IJĸH2OŸťCO2Ÿ
•! .•ķCO2ŸĸH2Oķcold trapŬ
Mars Odyssey
Neutron Spectrometer (NS) and
High-Energy Neutron Detector
(HEND)
Subsurface ice
Phoenix Mars Lander
AķŸbķf
ÑŪĔMķžÔijķhÖ
´|ňXĦıáÅĥŅńŸj
ļIJķ§ĥ
YÉŪĔzQÞ¬ĝłÛ
ÃĿłŅĬž9‘û
!¶@ķijĭęĬę
hÖ´|ĝ
Schorghofer and Aharonson (2005)
ŐŏŒŠĄŠžÔķËkfķI'
ţMGS/TESĶŁńŤ
ŐŏŒ
ŸĄ
žÔ
Smith, Icarus 167 (2004) 148–165
žÔķSÆñÕķŋŚšŎ
•! +•ķ¤ÿĞňĎ'
•! +-·ķJĶ+•Ğ‹ÒĦı+•CķžÔ¯kĞ‹ĕģŅ
ĞţģķŽ’ķl꫞hªIJËkĶ‚…¼ĶôĹŅńĖ
•! ËkĶôĹŅĬžÔķùĸäöæěķŔœŝšu¸IJ.-·ĺ
•! +-·ķÀĶĸ+•
IJÈĶŁŃžÔ¯kĞ
Ħĕ.+¯k)úĞï
éĨńĬľĕ?VXĵĴ
Ķ̞hªIJËkĝł
+•CĶžÔĞ‚…¼Ķ
ńĖËkķžÔûĸ
īŅļIJķžÔëîķc
šIJ ļńĖ
°ŒķžķL—ĵP
•! ĵĪģģIJ¥ķžĞ¡Ņńķĝ
Gullies
Seepages
White collars
•! ¶@ķ°ŒĸhÖ´|ij
àěńķĝĴĚĝ
Buried glaciersđ
N$T¼n Ïéê‡ß
èöăwµ
+•CķJÐķŠ^
Laskar et al. (2002)
•! Ïé‡ßĞ_ĥĠĵń!•CĞ\*!žÔĞ•CĶÈţJĶĿ
CO2ŸĶÚŇŅıÔ»ĦĵęŤ!·¼ĶžÔ¯k!ŸjĞ
ďËkĶtí
•! Ïé‡ßĞMğĠĵń!•CĞ«*!žÔĞ•CĝłÔ»!
·¼ĶžÔ¯k‹!ŸjĞËkļIJmŃĨ
Mellon & Phillips (2001)
•Dó
Ŕœŝšu¸ĶŁńžëî
•! .-·ķJķĻĚĞ+-·ķJŁŃĝęĬľĕJ·ĝł-·ĺķžÔëîĞĕ.-·ķJĶ&µŁ
ĠåģńĖ
•! iĀÃÅIJĸ+•CĶžňĂľń8ĞĘńĖ
H2OŸĄ
¯¦ĸžÔ
¨6œ
G@7:5;""97#;:#13+#C)%%HF
J
J
Permanent CO2 cap at the South pole
ąęijģņĶ>?)Ÿ
ąęijģņĶK)?Ÿ
£čĥŅİİĘń›R
>?)•ķùĐ
I9J297E#;:#13+#C)%%HF
CO2›R•ķĜĝĢIJ
›RH2OŸĿR@ĝ
•! Water in the southern polar cap : remnant from the past
where the southern water ice was stable?
•! How stable is the current southern water ice cap?
Montmessin et al. (2007)

Document 7437567

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