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Further Observations of Regional Dust Storms and Baroclinic Eddies in the Northern Hemisphere of Mars

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Further Observations of Regional Dust Storms and Baroclinic Eddies in the Northern Hemisphere of Mars ARTICLE IN PRESS Icarus xxx (2009) xxx–xxx Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Further observations of regional dust storms and baroclinic eddies in the northern hemisphere of Mars David P. Hinson a,b,*, Huiqun Wang c a Carl Sagan Center, SETI Institute, 515 N. Whisman Rd., Mountain View, CA 94043, USA b Department of Electrical Engineering, Stanford University, 350 Serra Mall, Stanford, CA 94305, USA c Atomic and Molecular Physics Division, Smithsonian Astrophysical Observatory, 60 Garden St., Cambridge, MA 02138, USA article info abstract Article history: We have investigated the near-surface meteorology in the northern hemisphere of Mars through detailed Received 24 April 2009 analysis of data obtained with Mars Global Surveyor in January–August 2005. The season in the northern Revised 22 August 2009 hemisphere ranged from midsummer through winter solstice of Mars Year (MY) 27. We examined Accepted 24 August 2009 composite, wide-angle images from the Mars Orbiter Camera and compiled a catalog of the dust storms Available online xxxx that occurred in this interval. As in previous martian years, activity in the northern hemisphere was dom- inated by regional ‘‘flushing” dust storms that sweep southward through the major topographic basins, Keywords: most frequently in Acidalia Planitia. We also used atmospheric profiles retrieved from radio occultation Mars, Atmosphere experiments to characterize eddy activity near the surface at high northern latitudes. There are strong Mars, Climate Atmospheres, Dynamics correlations between the two sets of observations, which allowed us to identify three factors that influ- ence the timing and location of the regional dust storms: (1) transitions among baroclinic wave modes, which strongly modulate the intensity of meridional winds near the surface, (2) storms zones, which impose strong zonal variations on the amplitude of some baroclinic eddies, and (3) stationary waves, which further modulate the wind field near the surface. The flushing dust storms ceased abruptly in midautumn, possibly in response to source depletion, CO2 condensation, a shift in the period of the baro- clinic eddies, and changes in the tidal wind field near the surface. Our results extend the meteorological record of the northern hemisphere, substantiate the findings of previous investigations, and further illu- minate the climatic impact of baroclinic eddies. Ó 2009 Elsevier Inc. All rights reserved. 1. Introduction a remarkable degree of spatial and temporal coherence, and winds sufficient to initiate dust storms. This paper reports new results concerning two important Further observations of baroclinic eddies were acquired when aspects of the weather in the northern hemisphere of Mars: baro- MGS attained a nearly-circular, polar orbit and began remote sens- clinic eddies and regional dust storms. We have characterized ing of the atmosphere. The Thermal Emission Spectrometer (TES) these phenomena through coordinated analysis of composite monitored atmospheric temperatures, dust, clouds, and water va- images and radio occultation data from Mars Global Surveyor por with essentially complete global coverage over a span of about (MGS). These two sets of observations are highly complementary 3 martian years (e.g. Smith, 2004). TES temperature profiles have in their sensitivity to diverse aspects of martian meteorology. been analyzed extensively to map the spatial structure and sea- This investigation builds on a foundation of knowledge assem- sonal evolution of baroclinic eddies as well as an assortment of bled in numerous previous studies. Meteorological data from the other atmospheric waves (Wilson et al., 2002; Hinson et al., Viking Landers revealed that eastward-traveling baroclinic eddies 2003; Banfield et al., 2003, 2004; Wang et al., 2005; Wang, 2007). dominate the dynamics near the surface at high northern latitudes Radio occultation experiments were also conducted routinely as during autumn, winter, and spring (e.g. Ryan et al., 1978; Leovy, part of the MGS radio science (RS) investigation (e.g. Hinson et al., 1979; Barnes, 1980, 1981; Leovy et al., 1985; James, 1985; Zurek 1999). Although their latitude coverage is limited, the RS measure- et al., 1992; Collins et al., 1996). These martian weather systems ments offer valuable insight into the behavior of baroclinic eddies have a characteristic spatial scale of several thousand kilometers, for two reasons. First, the RS results include accurate measure- ments of geopotential height on surfaces of constant pressure, which yield unique information about meridional winds near the * Corresponding author. Address: Carl Sagan Center, SETI Institute, 515 N. Whisman Rd., Mountain View, CA 94043, USA. Fax: +1 650 9617099. surface (Hinson, 2006, Figs. 5 and 6). Second, the temperature per- E-mail address: [email protected] (D.P. Hinson). turbations and eddy heat flux are confined to a shallow layer near 0019-1035/$ - see front matter Ó 2009 Elsevier Inc. All rights reserved. doi:10.1016/j.icarus.2009.08.019 Please cite this article in press as: Hinson, D.P., Wang, H. Further observations of regional dust storms and baroclinic eddies in the northern hemisphere of Mars. Icarus (2009), doi:10.1016/j.icarus.2009.08.019 ARTICLE IN PRESS 2 D.P. Hinson, H. Wang / Icarus xxx (2009) xxx–xxx the surface (Hinson, 2006, Figs. 8–10), which is resolved far better Circulation Model (MGCM) (Wang et al., 2003; Wilson et al., 2006; by radio occultation than by infrared sounding. These characteris- Basu et al., 2006). tics of the temperature field and meridional heat flux are consis- The impact of a flushing dust storm is accentuated by its cou- tent with eddies that arise from baroclinic instability (e.g. Gill, pling with the Hadley circulation, which can result in rapid 1982; Barnes, 1984), in which the disturbance extracts available changes in dust opacity and thermal structure on a global scale potential energy from the zonal-mean basic state. (e.g. Cantor et al., 2001; Wang et al., 2003; Cantor, 2007; Wang, The MGS Mars Orbiter Camera (MOC) has provided extensive 2007). In this way a sequence of cross-equatorial dust storms can observations of a distinctive type of dust storm that occurs in the trigger an appreciable change in the global state of the atmosphere, major topographic basins of the northern hemisphere during as indicated by the sudden appearance of a planet-encircling haze autumn and winter (Cantor et al., 2001; Wang et al., 2003, 2005; and a characteristic intensification of the Hadley circulation. This Cantor, 2007; Wang, 2007). These storms originate through lifting type of event has been observed during midautumn and midwinter and advection of dust by baroclinic eddies at high northern lati- of many martian years (e.g. Cantor et al., 2001; Wang et al., 2003; tudes. On some occasions these ‘‘frontal” storms spread southward Liu et al., 2003; Smith, 2004, 2009; Cantor, 2007; Wang, 2007), and as dust is entrained into the near-surface winds of the Hadley cir- MGCMs have made significant progress in simulating the initiation culation, and the resulting ‘‘flushing” or ‘‘cross-equatorial” storm and development of this type of dust storm (e.g. Wang et al., 2003; can progress from high northern latitudes into the tropics in a span Wilson et al., 2006; Basu et al., 2006). of a few days. The diurnally-varying, near-surface winds associated In this paper we extend the existing record of weather in the with thermal tides and topographic circulations appear to play an northern hemisphere through analysis of MGS data obtained dur- important role in the transition between the frontal and flushing ing January–August 2005, part of its final martian year of opera- stages of these dust storms (Wang et al., 2003; Wilson et al., 2006). tions. This interval corresponds to midsummer through winter Essential features of these flushing dust storms have been solstice of MY 27. We use a combination of MOC composite images determined through analysis of MOC images and TES temperature and RS atmospheric profiles to investigate key atmospheric phe- measurements spanning several martian years (Wang et al., 2003, nomena, including both flushing dust storms and baroclinic eddies. 2005; Wang, 2007). These storms occur more commonly in Acida- This is the first detailed examination of martian meteorology in lia than in Utopia or Arcadia (e.g. Wang et al., 2005), although Uto- this period. pia was the locus of activity in autumn of Mars Year (MY) 26 The MOC observations from MY 24–26 have been analyzed (Wang, 2007). (In assigning numbers to martian years we adopt extensively (e.g. Cantor et al., 2001; Wang and Ingersoll, 2002; the convention that MY 1 began on 11 April 1955 (Clancy et al., Wang et al., 2003, 2005; Cantor, 2007; Wang, 2007), but the subset 2000), at the vernal equinox in the northern hemisphere of Mars.) of data considered here has received little attention. Section 2 The dust-storm distribution is clearly influenced by a zonal asym- reviews basic features of these data and the procedure used in metry in the baroclinic eddies, which appears in the form of a lon- constructing composite images. Section 3 shows a selection of gitude band where the eddy amplitude is significantly larger than images and describes the regional dust storms that occurred in the zonal average (e.g. Wang et al., 2005, Fig. 10). This phenome- the northern hemisphere during autumn of MY 27, building on non, known as a ‘‘storm zone” (Hollingsworth et al., 1996), appears the initial results reported by Cantor (2007, Section 5.7). most commonly though intermittently near 280E, to the northeast The RS instrument on MGS was the only atmospheric sounder of Alba Mons and to the northwest of Acidalia Planitia (e.g. Banfield in operation during autumn of MY 27. As with the MOC images, et al., 2004; Wang et al., 2005). the RS data from MY 24–26 have received considerably more Sequences of flushing dust storms generally appear within two attention (e.g.
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