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Characterization of thermal tides at...

Cahoy, Kerri L.

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Characterization of thermal tides at ionospheric altitudes on Mars with Mars Global Surveyor Radio Occultation measurements of electron density.

Record Type:	Language materials, printed : Monograph/item
Title/Author:	Characterization of thermal tides at ionospheric altitudes on Mars with Mars Global Surveyor Radio Occultation measurements of electron density./
Author:	Cahoy, Kerri L.
Description:	157 p.
Notes:	Adviser: G. Leonard Tyler.
Contained By:	Dissertation Abstracts International69-02B.
Subject:	Atmospheric Sciences. -
Online resource:	http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=3302812
ISBN:	9780549488903

Characterization of thermal tides at ionospheric altitudes on Mars with Mars Global Surveyor Radio Occultation measurements of electron density.
Cahoy, Kerri L.

Characterization of thermal tides at ionospheric altitudes on Mars with Mars Global Surveyor Radio Occultation measurements of electron density. - 157 p.

Adviser: G. Leonard Tyler.

Thesis (Ph.D.)--Stanford University, 2008.

Between November 2000 and June 2005, the Mars Global Surveyor (MGS) Radio Occultation Experiment measured 5,229 electron density, n e, profiles at 100--200 km altitude from 60 to 85°N in the spring and summer of Mars Years (MYs) 25, 26, and 27. The n e profiles show zonal structure with observed wave numbers k = 1--6, attributed to nonmigrating tides. For observations within fixed local time intervals, migrating tides contribute to the zonal mean ne. Observations span 03:00--09:00 hr local time in MY 25 and 04:00--14:00 hr in MY 26 and 27, changing at rates less than 1 hr/3°LS.

ISBN: 9780549488903Subjects--Topical Terms:

1019179
Atmospheric Sciences.

Characterization of thermal tides at ionospheric altitudes on Mars with Mars Global Surveyor Radio Occultation measurements of electron density.
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020 $a 9780549488903
035 $a (UMI)AAI3302812
035 $a AAI3302812
040 $a UMI $c UMI
100 1 $a Cahoy, Kerri L. $3 1278959
245 1 0 $a Characterization of thermal tides at ionospheric altitudes on Mars with Mars Global Surveyor Radio Occultation measurements of electron density.
300 $a 157 p.
500 $a Adviser: G. Leonard Tyler.
500 $a Source: Dissertation Abstracts International, Volume: 69-02, Section: B, page: 1192.
502 $a Thesis (Ph.D.)--Stanford University, 2008.
520 $a Between November 2000 and June 2005, the Mars Global Surveyor (MGS) Radio Occultation Experiment measured 5,229 electron density, n e, profiles at 100--200 km altitude from 60 to 85°N in the spring and summer of Mars Years (MYs) 25, 26, and 27. The n e profiles show zonal structure with observed wave numbers k = 1--6, attributed to nonmigrating tides. For observations within fixed local time intervals, migrating tides contribute to the zonal mean ne. Observations span 03:00--09:00 hr local time in MY 25 and 04:00--14:00 hr in MY 26 and 27, changing at rates less than 1 hr/3°LS.
520 $a Chapman theory accounts for the main features of the primary peak electron densities, ne,peak, and heights, z peak, vs. solar zenith angle (SZA). SZA varies between 71 and 89°; as SZA increases, zpeak increases and ne,peak decreases. Over the three MYs z peak ranges from 125 to 160 km and ne,peak from 2.5 to 13.8 x 104 cm-3. The decrease in ne,peak from MY 25 to 27 is consistent with the decreasing 11-year solar activity cycle. Periodic variations in ne,peak as large as 4.5 x 104 cm -3 in MY 26 correspond to the 27-day solar rotational cycle. Estimates of single-layer Chapman model parameters in MY 25, 26, and 27, respectively, are: ne,0 = 19.0, 16.9, 13.3 x 10 4 cm-3; z0 = 120.1, 119.8, 119.2 km; and epsilon = 0.48. 0.42, 0.35. Estimates of the lower secondary peak densities and heights range from 2 to 6 x 104 cm -3 and from 105 to 120 km.
520 $a Differential analysis of individual k amplitudes yields up to +/-6 km vertical displacement of the ionosphere. In MY 26 the apparent phase velocity of the 5--15% zonal structure with k = 3 is consistent with the semidiurnal eastward Kelvin mode, SE1. The total variation of k = 1-6 is up to 60% of n e. Simulations using Mars General Circulation Models predict SE1 at 5--15% in neutral density for conditions similar to the MGS ne data.
590 $a School code: 0212.
650 4 $a Atmospheric Sciences. $3 1019179
650 4 $a Engineering, Aerospace. $3 1018395
650 4 $a Engineering, Electronics and Electrical. $3 626636
690 $a 0538
690 $a 0544
690 $a 0725
710 2 $a Stanford University. $3 754827
773 0 $t Dissertation Abstracts International $g 69-02B.
790 $a 0212
790 1 0 $a Tyler, G. Leonard, $e advisor
791 $a Ph.D.
792 $a 2008
856 4 0 $u http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=3302812