2006
DOI: 10.1134/s0010952506040046
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Results of measurements with the Planetary Fourier Spectrometer onboard Mars Express: Clouds and dust at the end of southern summer. A comparison with OMEGA images

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Cited by 11 publications
(7 citation statements)
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“…Atmospheric wave patterns on the OMEGA O 2 emission maps have been systematically searched in the considered data set. The spatial scale in the direction perpendicular to the wave fronts is about 100 km for the orbit acquired at Ls = 176.69°(comparable to the values observed close to the north pole, Zasova et al, 2006b) and about 130 km for the orbit acquired at Ls = 180.62°. Waves are clearly observed at Ls = 176.69°and 180.62° (Fig.…”
Section: Atmospheric Wavessupporting
confidence: 73%
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“…Atmospheric wave patterns on the OMEGA O 2 emission maps have been systematically searched in the considered data set. The spatial scale in the direction perpendicular to the wave fronts is about 100 km for the orbit acquired at Ls = 176.69°(comparable to the values observed close to the north pole, Zasova et al, 2006b) and about 130 km for the orbit acquired at Ls = 180.62°. Waves are clearly observed at Ls = 176.69°and 180.62° (Fig.…”
Section: Atmospheric Wavessupporting
confidence: 73%
“…Atmospheric waves in the O 2 emission nadir maps have been observed on orbit 68 (Zasova et al, 2006b), close to the terminator on north pole, and orbit 351 at latitudes between 18°and 27°N, coupled to pressure waves at low altitude (Spiga et al, 2007). Atmospheric wave patterns on the OMEGA O 2 emission maps have been systematically searched in the considered data set.…”
Section: Atmospheric Wavesmentioning
confidence: 99%
“…A lower spectral resolution, like that of the TES instrument (Smith, 2004) (6.25 and 12.5 cm -1 ), results in a decrease in the accuracy of temperature profile recovery, since the CO 2 band turns out to be quite nar row under the low pressure in the Martian atmo sphere. The vertical temperature profiles in the Mar tian atmosphere recovered from the IRIS M and PFS experiments can be found in (Santee and Crisp, 1993;Zasova et al, 2001Zasova et al, , 2002Zasova et al, , 2005aZasova et al, , 2005bZasova et al, , 2006Grassi et al, 2005). The temperature profile and aerosol opti cal depth are determined self consistently from one spectrum: the temperature profile is found by the CO 2 15 µm band, and the optical depth is found by the aerosol absorption bands.…”
Section: Study Of Mars In the "Atmosphere" Modementioning
confidence: 99%
“…The atmosphere over great volcanoes on Mars has been studied intensely from measurements of many instruments (Zasova et al, 2001(Zasova et al, , 2006Benson et al, 2003Benson et al, , 2006Wang and Ingersoll, 2002;Pearl et al, 2001;Grassi et al, 2005a) as well as by mesoscale models (Rafkin et al, 2002;Michaels et al, 2006;Moudden and McConnell, 2005;Spiga and Forget, 2009). Olympus Mons on Mars, with its 25 km altitude has a strong impact on the atmospheric circulation, especially if we consider that the scale height H for a temperature variation is of the order of 10-11 km.…”
Section: Introductionmentioning
confidence: 99%