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Photochemical escape of oxygen from Mars: First results from MAVEN in situ data
Author(s) -
Lillis Robert J.,
Deighan Justin,
Fox Jane L.,
Bougher Stephen W.,
Lee Yuni,
Combi Michael R.,
Cravens Thomas E.,
Rahmati Ali,
Mahaffy Paul R.,
Benna Mehdi,
Elrod Meredith K.,
McFadden James P.,
Ergun Robert. E.,
Andersson Laila,
Fowler Christopher M.,
Jakosky Bruce M.,
Thiemann Ed,
Eparvier Frank,
Halekas Jasper S.,
Leblanc François,
Chaufray JeanYves
Publication year - 2017
Publication title -
journal of geophysical research: space physics
Language(s) - English
Resource type - Journals
eISSN - 2169-9402
pISSN - 2169-9380
DOI - 10.1002/2016ja023525
Subject(s) - atmospheric escape , mars exploration program , atmosphere of mars , martian , thermosphere , atmosphere (unit) , atmospheric sciences , extreme ultraviolet lithography , irradiance , ion , photoionization , flux (metallurgy) , earth's magnetic field , physics , environmental science , astrobiology , ionosphere , ionization , chemistry , meteorology , magnetic field , astronomy , optics , organic chemistry , quantum mechanics
Photochemical escape of atomic oxygen is thought to be one of the dominant channels for Martian atmospheric loss today and played a potentially major role in climate evolution. Mars Atmosphere and Volatile Evolution Mission (MAVEN) is the first mission capable of measuring, in situ, the relevant quantities necessary to calculate photochemical escape fluxes. We utilize 18 months of data from three MAVEN instruments: Langmuir Probe and Waves, Neutral Gas and Ion Mass Spectrometer, and SupraThermal And Thermal Ion Composition. From these data, we calculate altitude profiles of the production rate of hot oxygen atoms from the dissociative recombination of O 2 + and the probability that such atoms will escape the Mars atmosphere. From this, we determine escape fluxes for 815 periapsis passes. Derived average dayside hot O escape rates range from 1.2 to 5.5 × 10 25 s −1 , depending on season and EUV flux, consistent with several pre‐MAVEN predictions and in broad agreement with estimates made with other MAVEN measurements. Hot O escape fluxes do not vary significantly with dayside solar zenith angle or crustal magnetic field strength but depend on CO 2 photoionization frequency with a power law whose exponent is 2.6 ± 0.6, an unexpectedly high value which may be partially due to seasonal and geographic sampling. From this dependence and historical EUV measurements over 70 years, we estimate a modern‐era average escape rate of 4.3 × 10 25 s −1 . Extrapolating this dependence to early solar system, EUV conditions gives total losses of 13, 49, 189, and 483 mbar of oxygen over 1–3 and 3.5 Gyr, respectively, with uncertainties significantly increasing with time in the past.