Mars Global Surveyor Thermal Emission Spectrometer (TES) observations of dust opacity during aerobraking and science phasing

By Michael D. Smith, J. Pearl, B. Conrath, Philip R. Christensen. 2000

145 citations recorded by the source corpus.

Subfields: Aerospace Engineering, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/a9ad06fab3a2959dbb6a787165ab1f422067da1c

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Aerospace Engineering

1. Michael D. Smith
2. Philip R. Christensen
3. Michael J. Wolff
4. S. Ruff
5. Mark Richardson
6. J. Pearl
7. B. Conrath
8. Hugh H. Kieffer

In Astronomy and Astrophysics

1. Michael D. Smith
2. Philip R. Christensen
3. Michael J. Wolff
4. Mark Richardson
5. Francois Forget
6. S. Ruff
7. V. Hamilton
8. Hugh H. Kieffer

Citations in the corpus

• Assimilation of thermal emission spectrometer atmospheric data during the Mars Global Surveyor aerobraking period (2007, methodology): “The atmospheric retrievals from TES observations which are used for these assimilations are described in more detail by Conrath et al. (2000) and Smith et al. (2000).”
• Bright and dark regions on Mars: Particle size and mineralogical characteristics based on thermal emission spectrometer data (2002, methodology): “Although a linear deconvolution method for surface-atmosphere separation is employed in those studies [Smith et al., 2000a], this method has limitations for examining the spectral characteristics of bright regions.”
• High-resolution thermal inertia derived from the Thermal Emission Imaging System (THEMIS): Thermal model and applications (2006, methodology): “TES atmospheric dust opacity was used for the first Martian year of MGS mapping when there were no global dust storms [Smith et al., 2000; M. D. Smith et al., 2001].”
• Thermal Emission Spectrometer results: Mars atmospheric thermal structure and aerosol distribution (2001, methodology): “Averaged dust opacity was comparable to the previous Mars year observed by TES (1997-1998) [Smith et al., 2000a], but substantially less than that observed during the first Viking year [Martin and Richardson, 1993; Martin, 1986] or by Mariner 9 [Fenton ctal., 1997, Hand et ai., I972].”
• One Martian year of atmospheric observations using MER Mini‐TES (2006, background): “optical depth can only fall by dust settling, which typically has a timescale of a couple months [e.g., Conrath, 1975; Smith et al., 2000].”
• Observations of the initiation and evolution of the 2001 Mars global dust storm (2005, methodology): “The data have been used to derive profiles of atmospheric temperature [Conrath et al., 2000] and aerosol opacities [Smith et al., 2000].”
• Interannual variability in TES atmospheric observations of Mars during 1999–2003 (2004, methodology): “It is made by taking results from the Smith et al. (2000a) algorithm at each latitude and longitude during the season that gives the highest surface temperature and lowest aerosol optical depth.”