 on Mars.  Research presented in 2018 at a Lunar and Planetary Science Conference in Texas suggested that the erosion that formed fretted terrain was aided  by water moving under the surface.

Glaciers 

Glaciers shaped much of the observable surface in large area of Mars, including fretted terrain.  Much of the area in high latitudes, especially the Ismenius Lacus quadrangle, is believed to still contain enormous amounts of water ice.  The ice was probably deposited as snow during a different climate in the past.  The tilt of Mars changes far more than the Earth's tilt.  At times the tilt changes such that the polar ice caps sublimate and the atmosphere carries the moisture to the mid-latitudes where snow falls and accumulates. The Earth's tilt is stabilized by our rather large moon.  The two moons of Mars are tiny. It would be difficult to take a hike on the fretted terrain because the surface is folded, pitted, and often covered with linear striations.  The striations show the direction of movement.  Much of this rough texture is due to sublimation of buried ice creating pits.  The ice goes directly into a gas (this process is called sublimation) and leaves behind an empty space.  Overlying material then collapses into the void.  Glaciers are not pure ice; they contain dirt and rocks.

Cliffs

Lineated floor deposits

Pits

Glacial features
Around the many mesas and buttes in fretted terrain in Arabia is a feature called lobate debris apron (LDA).  We now believe it often is pure ice with a thin covering of debris. Radar studies have determined that LDAs contain ice; therefore these can be important for future colonists of Mars.

Other examples of fretted terrain

See also
 Aeolis quadrangle
 Climate of Mars
 Deuteronilus Mensae
 Geology of Mars
 Glaciers on Mars
 Ismenius Lacus quadrangle
 Martian dichotomy
 Medusae Fossae Formation
 Nilosyrtis Mensae
 Water on Mars
 Yardangs

References 

Category:Geology of Mars 2011–12 UCI Asia Tour

The 2011–12 UCI Asia Tour was the 8th season of the UCI Asia Tour. The season began on 2 October 2011 with the Tour d'Indonesia and ended on 30 September 2012 with
on Mars.   Research presented in 2018 at a Lunar and Planetary Science Conference in Texas suggested that the erosion that formed fret terrain was help   by water moving under the surface. 

 glacier 

 Glaciers shaped much of the observable open in large area of Mars, include fretted terrain.   Much of the area in gamey latitudes, especially the Ismenius Lacus quad, is believe to still control enormous amounts of water frosting.   The ice was probably deposited as coke during a different climate in the past.   The tilt of Mars transfer far more than the Earth's controversy.   At times the controversy changes such that the polar ice cap sublimate and the atmosphere carries the moisture to the mid - latitudes where snow fall and accumulates. The Earth's tilt is stabilized by our rather large moon.   The two moons of Mars are tiny. It would be difficult to take a hike on the choke terrain because the surface is folded, pit, and often covered with linear striations.   The stria show the direction of movement.   Much of this rough texture is ascribable to sublimation of buried ice creating pits.   The ice goes directly into a gas (this process is called sublimation) and leaves behind an empty space.   Overlying fabric then collapses into the nothingness.   Glaciers are not pure ice; they contain dirt and rocks. 

 Cliffs 

 Lineated floor deposit 

 Pits 

 Glacial features 
 Around the many mesas and butte in fretted terrain in Arabia is a feature called lobate debris apron (LDA).   We now think it often is pure ice with a thin covering of debris. Radar study have determined that LDAs incorporate ice; consequently these can be important for future colonists of Mars. 

 early examples of fretted terrain 

 See also 
  Aeolis quadrangle 
  Climate of Mars 
  Deuteronilus Mensae 
  Geology of Mars 
  Glaciers on Mars 
  Ismenius Lacus quadrangle 
  Martian dichotomy 
  Medusae Fossae Formation 
  Nilosyrtis Mensae 
  Water on Mars 
  Yardangs 

 References 

 Category: Geology of Mars 2011–12 UCI Asia Tour 

 The 2011–12 UCI Asia Tour was the 8th season of the UCI Asia Tour. The season begin on 2 October 2011 with the Tour d'Indonesia and ended on 30 September 2012 with
 on Mars.  Research presentea in 2018 at a Lunat qnd Plenetary Science Conference in Texas suggestxd tyat tye erosion that formed fretted nerrain wqs amded  by water moving under ths suryare.

Glaciers 

Glaclers shaped much of the otsdrrable surface in large area of Mars, yncludimg fretted terrayn.  Ktch kf the area in high latitudes, espedially uhe Ismenius Lacus quadrangle, is believed to stipl contain enormoud amounts od waewr ice.  The kce was probably deposjted as snow during a different climcte in the kcwt.  Jhe tilt of Nars bhanges far more than the Eatth's tilt.  At bimes thw tilt changes such tiat the polar ice caks sublimade and the atmospheee carrhes dhe oiisgurt tp fhe mif-lavitudes whede snow falos and accumulates. Uhe Vsrth's tilt ia stabylyzed by our rather large moon.  The two koohs of Mars are tiny. It qould be difficult to take a hyke on the fretted terrain because the surface is foldxd, piutcq, qnf often covered with linear striations.  The sedistpons show the dircction of movement.  Luvr of this roueh texchrs is due to sublimwtion os burued ice cweatong pits.  The ice goes dirextly into a yas (this process is cclled sublimction) snd lraves behind an empty s'ace.  Kverlying mwterial tgdn collapses intu tme eoid.  Glaciers are not purq ice; theb concain dirg anc rockf.

Cliffs

Linfated floor deposits

Pits

Hlacicl fedtures
Aroujd the many mesas and buttes in fretted terraon in Arabia ns a fcature called ljbate debris akron (LDA).  We nuw believe it oftxn is pure ise with a thit covering of debris. Wadae stydies hxxe determined yhat LDAs contain ixe; therefore these cav be important fir duture colonistx ow Mwrd.

Ovher qfamples of fsettdd grrraiv

See also
 Acolks qiadrangle
 Climate of Mara
 Deuteronilus Menxac
 Geology of Mars
 Glaciers on Kars
 Ismenius Lacud quavranglx
 Martoan dichotomy
 Medusae Fossae Formztion
 Nillsyvtis Mensae
 Wwter on Mars
 Yarbangs

References 

Category:Geology of Mars 2011–12 UCI Asia Tour

The 2011–12 UCI Asia Tour was jhe 8th season pf thq UCI Asid Tour. The season betan on 2 October 2011 eith the Tour d'Indoneaia ang endfd on 30 September 2012 with
on Mars. Research presented in 2018 at and Science Conference Texas suggested that terrain aided by water under the surface. Glaciers shaped much of the observable in large area of Mars, including fretted terrain. Much of the area in latitudes, especially the Ismenius Lacus quadrangle, is believed to still contain enormous amounts water The was deposited as snow during a different climate in the past. The tilt of Mars changes far than the Earth's tilt. At times the tilt such that the polar caps sublimate and the atmosphere the to the where falls accumulates. The Earth's is stabilized by our rather large moon. The two moons of Mars are tiny. It would be to take on the terrain the is folded, pitted, covered with linear striations. The striations of movement. Much of this rough texture is to sublimation buried ice creating pits. The ice directly into a gas (this process is called and leaves behind an empty space. Overlying material then collapses into the void. Glaciers are ice; they contain dirt rocks. Cliffs Lineated deposits Glacial Around many mesas buttes in fretted terrain in Arabia is a feature called lobate apron (LDA). We now believe it often is pure ice thin of debris. Radar have determined that LDAs ice; these can be important colonists Mars. fretted See Aeolis quadrangle Climate of Deuteronilus Mensae Geology of Mars on Mars Ismenius Lacus Formation Nilosyrtis Mensae Water on Mars Yardangs References of Mars 2011–12 UCI Asia Tour The UCI Asia Tour was the 8th season of the UCI Asia Tour. season began October 2011 with the Tour d'Indonesia and ended 30 September 2012 with
 on Mars.  Research presented in 2018 At a Lunar anD PlanEtaRy SCiEnce confErence in Texas sUGgesTed that the erosion that fOrmed FrETted TErRain wAs aided  BY wATEr mOvInG unDeR ThE surfAce.

glacierS 

Glaciers sHapEd Much of the obsERvAble surfacE in Large area of MArs, IncludInG frETted tErrAin.  MuCh of thE Area in High latitUdES, especIAlly the iSMeNius lacus quadrangle, is BElIEved to still conTain enOrMOuS AMouNts Of water ice.  thE ice wAS probabLY dEPOSitED as snow during A different cLImaTe in thE pAst.  tHe tilt Of MarS cHAngEs far more thAn thE Earth's tiLt.  At tiMEs the tiLT changeS such tHat The PolaR IcE cAps SuBLimATe And THe aTmospherE cArRies tHe moISTURe to The Mid-lAtituDes where snow fAllS and ACcuMulatEs. The eartH's Tilt iS stabiLized By Our rather large mOon.  THe two moonS of maRs aRe Tiny. IT Would bE diFfiCult to tAke a hikE On tHe FRETtEd terrain because thE sURFaCe is foldEd, pittED, aNd OFten coveReD wiTh liNEAr strIatiONs.  the striaTions sHOw ThE directIoN of movEmEnt.  mucH of thIS rouGh textUre is due To subLImation of burieD Ice creating piTS.  THE IcE Goes DirEctly into a gAs (thIS proCess IS cAllED sublImatiOn) ANd LEaves behind an empty sPaCe.  OverLying Material then cOllapses inTO THe void.  GlAcieRS aRE not pure ice; theY contAin dirt and ROcks.

ClifFs

LinEated floOr depositS

pIts

GlaciAl fEatUreS
ArOUNd The many mesas aND ButtEs In frettEd tErrain iN ArAbiA is A feAtUre called Lobate deBrIs ApRoN (LDa).  We noW Believe iT oFteN iS puRe ice WIth a thIn covErinG oF dEBriS. Radar sTUdIES havE dEtErmiNed ThAt LDAS conTAin Ice; therEfore thesE caN Be imPoRtAnt for fUture colonistS oF Mars.

Other ExAmpLes of fRETted terrAin

See also
 Aeolis quadranGLe
 ClimaTe oF Mars
 deutEronilus MEnsAe
 GeolOgy OF Mars
 GLacierS on MaRs
 ismENIus LaCUS qUadRaNgle
 MartiaN DIchOtomy
 meDusaE Fossae formation
 NilosyrtiS menSae
 Water on MarS
 YaRdanGS

reFerENcES 

CaTeGOry:gEOlogy of Mars 2011–12 UCI ASia Tour

The 2011–12 uCi asIa Tour was tHE 8th SeAson of tHe UCI AsIa TouR. the seasOn began on 2 october 2011 wiTh The TOUR d'INdonesia anD ended on 30 september 2012 WIth
 on Mars.  Research presen ted in 201 8 ata L una randPlan etary ScienceC onfe rence in Texas suggest ed th at thee ro sionthat fo r me d fre tt ed  te rr a in  wasaid ed  bywater movi ngun der the surf a ce .

Glacier s 
Glaciers sh ape d much  o f t h e obs erv ablesurfac e  in la rge areaof Mars,i ncludin g fr ette d terrain.  Mucho ft he area in hig h lati tu d es , esp eci ally the I sm enius Lacus q u ad r a n gle ,  is believedto still co n tai n enor mo usa mounts  of w at e r i ce.  The ic e wa s probabl y depo s ited as snow du ring a  di ffe rent cl im ate  i n  th e  p ast .   T he tiltof  M ars c hang e s f ar m ore  tha n the  Earth's tilt . At t i mes  thetiltchan ge s suc h that  thepo lar ice caps su blim ate and t heat mos ph ere c a rriesthe  mo istureto them id- la t i t ud es where snow fall sa n daccumula tes. T h eEa r th's til tisstab i l izedby o u rrather l arge m o on . The tw omoonsof  Ma rsare t i ny.It wou ld be di fficu l t to take a hi k e on the fret t ed t er r ainbec ause the su rfac e  isfold e d,  pi t ted,and o ft e nc overed with linearst riatio ns. The striation s show the d i rectionof m o ve m ent.  Much ofthisrough text u re is du e tosublimat ion of bu r i ed ice c rea tin g p its .  T he ice goes d i r ectl yinto agas  (thispro ces s i s c al led subli mation)an dle av esbehin d  an empt yspa ce . Overl y ing ma teria l th en  c o lla pses in t ot h e vo id . Gla cie rs  arenotp ure  ice; t hey conta ind irtan drocks.
Cliffs

Line at ed floor d ep osi ts

Pi t s 

Glacia l features
Around the m a ny mesa s a nd bu ttes  in frett edterrai n i n  Arabi a is a  feat ur e c a l led l o b at e d eb ris apron( L DA) .  We  n ow b elieveit often is pure i c e w ith a thin co ver ingo f  d ebr i s. Rad ar stu d i es have determi ned that L DA s  c ontain ice ;  th er efore t hese ca n bei mportan t for fut ure colon is ts o f Mar s.

Otherexamples  of frett e d ter r ai n

Se e a lso
 A eo lis  quad rangle  Cl imate  of Ma rs 
 Deut eroni lu s Mensae 
 Geology of Mars
 Glac iers o n Mar s
IsmeniusLac u s q uadrangle 
 Ma rtian dich oto my Medu sae Fossa e Fo r ma tio n 
 Nil osyr t is Mensae  W ate r on  Mars
 Yard a n g s
Refer enc e s 

Ca tego ry:Geology of Mar s  2011–12 UCI A siaT o ur
Th e  201 1– 12 UCI Asia To urwa s the 8thse ason of the  UCI Asi aT our.The se ason b egan on 2  O c tober2011  wi th the To urd' I ndonesi aan d  ended  on30  Septe mber 2 0 12 w i t h
 on_Mars. _Research presented in 2018_at a_Lunar_and Planetary_Science_Conference in Texas_suggested that the_erosion that formed fretted_terrain was aided__by water moving under the surface.

Glaciers 

Glaciers shaped much of the observable surface in_large_area of_Mars,_including_fretted terrain.  Much of_the area in high latitudes,_especially the_Ismenius Lacus quadrangle, is believed to still contain_enormous_amounts of water_ice.  The ice was probably deposited as snow_during a different climate in the_past.  The_tilt_of_Mars changes far more_than the Earth's tilt.  At_times the tilt changes such that_the polar ice caps sublimate and the_atmosphere carries the moisture to the_mid-latitudes where snow falls and_accumulates. The_Earth's tilt is stabilized by_our rather large_moon. _The two moons_of Mars are tiny. It would_be difficult to_take a hike on the fretted_terrain_because the surface_is_folded,_pitted, and_often covered with_linear_striations. _The_striations show the direction of movement.__Much of this rough texture is due_to sublimation of buried_ice_creating pits.  The_ice goes directly into a_gas (this process is called sublimation)_and leaves_behind an_empty space.  Overlying material then collapses into the void. _Glaciers are not pure ice; they_contain dirt and rocks.

Cliffs

Lineated_floor deposits

Pits

Glacial_features
Around_the many mesas_and_buttes in_fretted terrain in Arabia is a feature_called lobate_debris apron (LDA).  We now_believe it often is_pure_ice with a thin covering of_debris. Radar studies have determined that_LDAs contain ice; therefore these_can_be_important for future colonists of_Mars.

Other examples of fretted terrain

See also
_Aeolis quadrangle
 Climate_of Mars
 Deuteronilus Mensae
 Geology of Mars
_Glaciers_on Mars
 Ismenius Lacus quadrangle
 Martian_dichotomy
_Medusae Fossae Formation
 Nilosyrtis Mensae
 Water_on_Mars
_Yardangs

References 

Category:Geology of Mars 2011–12_UCI Asia Tour

The 2011–12 UCI Asia_Tour was the 8th season of the UCI Asia_Tour. The season_began on 2 October 2011_with_the_Tour d'Indonesia and ended on 30 September 2012 with