Convective vortices and dust devils at the MSL landing site: Annual variability

Tutkimustuotos: Lehtiartikkelivertaisarvioitu

Tutkijat

  • Henrik Kahanpää

  • C. Newman
  • J. Moores
  • M. -P. Zorzano
  • J. Martin-Torres
  • S. Navarro
  • A. Lepinette
  • B. Cantor
  • M. T. Lemmon
  • P. Valentin-Serrano
  • A. Ullan
  • W. Schmidt

Organisaatiot

  • Finnish Meteorological Institute
  • Ashima Research
  • York University
  • Centro de Astrobiología
  • Luleå University of Technology
  • Instituto Andaluz de Ciencias de la Tierra
  • Malin Space Science Systems
  • Texas A and M University
  • University of Alcalá

Kuvaus

Two hundred fifty-two transient drops in atmospheric pressure, likely caused by passing convective vortices, were detected by the Rover Environmental Monitoring Station instrument during the first Martian year of the Mars Science Laboratory (MSL) landed mission. These events resembled the vortex signatures detected by the previous Mars landers Pathfinder and Phoenix; however, the MSL observations contained fewer pressure drops greater than 1.5 Pa and none greater than 3.0 Pa. Apparently, these vortices were generally not lifting dust as only one probable dust devil has been observed visually by MSL. The obvious explanation for this is the smaller number of strong vortices with large central pressure drops since according to Arvidson et al. [2014] ample dust seems to be present on the surface. The annual variation in the number of detected convective vortices followed approximately the variation in Dust Devil Activity (DDA) predicted by the MarsWRF numerical climate model. This result does not prove, however, that the amount of dust lifted by dust devils would depend linearly on DDA, as is assumed in several numerical models of the Martian atmosphere, since dust devils are only the most intense fraction of all convective vortices on Mars, and the amount of dust that can be lifted by a dust devil depends on its central pressure drop. Sol-to-sol variations in the number of vortices were usually small. However, on 1 Martian solar day a sudden increase in vortex activity, related to a dust storm front, was detected.

Yksityiskohdat

AlkuperäiskieliEnglanti
Sivut1514-1549
Sivumäärä36
JulkaisuJournal of geophysical research-Planets
Vuosikerta121
Numero8
TilaJulkaistu - elokuuta 2016
OKM-julkaisutyyppiA1 Julkaistu artikkeli, soviteltu

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