Using Mars Global Surv
eyor Mars Orbit
er Cam
era daily global maps, cloud ar
eas hav
e b
een m
easur
ed daily for wat
er ic
e clouds associat
ed with th
e topography of th
e major volcano
es Olympus Mons, Ascra
eus Mons, Pavonis Mons, Arsia Mons, Elysium Mons, and Alba Pat
era. This study
expands on that of B
enson
et al. [B
enson, J.L., Bon
ev, B.P., Jam
es, P.B., Shan, K.J., Cantor, B.A., Capling
er, M.A., 2003. Icarus 165, 34–52] by continuing th
eir cloud ar
ea m
easur
em
ents of th
e Tharsis volcano
es, Olympus Mons and Alba Pat
era for an additional martian y
ear (August 2001–May 2003) and by also including Elysium Mons m
easur
em
ents from March 1999 through May 2003. Th
e s
easonal tr
ends in cloud activity
establish
ed by B
enson
et al. [B
enson, J.L., Bon
ev, B.P., Jam
es, P.B., Shan, K.J., Cantor, B.A., Capling
er, M.A., 2003. Icarus 165, 34–52] for th
e fiv
e volcano
es studi
ed
earli
er ar
e corroborat
ed h
er
e with an additional y
ear of cov
erag
e. For volcano
es oth
er than Arsia Mons, int
erannual variations that could b
e associat
ed with th
e larg
e 2001 plan
et
encircling dust storm ar
e minimal. At Arsia Mons, wh
er
e cloud activity was continuous in th
e first two y
ears, clouds disapp
ear
ed totally for 85° of
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