Biology
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p53e1564w&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P53E-1564
Biology
[5210] Planetary Sciences: Astrobiology / Planetary Atmospheres, Clouds, And Hazes
Scientific paper
We examined the temperature fields at 0.1 Pa (~70 km) between Ls = 111° and 154° of MY 28 to 30 over the northern polar region of Mars from 30°N to 90°N. The study is based on observations from the Mars Climate Sounder (MCS) [McCleese et al., 2007] on the Mars Reconnaissance Orbiter (MRO) mission [Zurek and Smrekar, 2007]. Daytime temperatures have been selected between LT = 9.6 and LT = 18.0. A stationary wave number 3 pattern is evident between Ls = 111° and 148° (Fig. 1 and Fig. 2). The maxima are significantly narrower, longitudinally, than the minima. During this interval, the two maxima in temperature near longitudes -152°E and 100°E shifted slightly eastward by ~24° and ~5°, respectively. The third maximum at -32°E did not shift in longitude, although it moved northward. All three maxima also changed slightly in temperature as the season advanced. The maximum at 100°E increased by ~5 K, while the other two cooled off (by ~7 K and ~5 K, respectively). The Martian upper atmosphere thermal structure shown in Figs. 1 and 2 has not been described previously. Somewhat similar phenomena have been seen at higher altitudes between ~130 km and ~160 km during northern spring over the region from 60°S to 50°N from MGS aerobraking data [Withers et al, 2003]. It is possible that the structure at ~70 km is also due to topographic forcing of the thermal tide. Fig.1. The thermal field at 0.1 Pa between Ls = 111° - 114°.
Abdou Wedad A.
Benson Jennifer L.
Heavens Nicholas
Kass David Michael
Kleinbohl Armin
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