The Mars Atmosphere and Volatile Evolution (MAVEN) Mission

Jakosky, B. M.; Lin, R. P.; Grebowsky, J. M.; Luhmann, J. G.; Mitchell, David; Beutelschies, G.; Priser, T.; Acuña, M. H.; Andersson, L.; Baird, Darren; Baker, D. N.; Bartlett, R. O.; Benna, M.; Bougher, S. W.; Brain, David; Carson, D. D.; Cauffman, Sandra; Chamberlin, Phillip C.; Chaufray, Jean‐Yves; Cheatom, Oscar; Clarke, J. T.; Connerney, J. E. P.; Cravens, T. E.; Curtis, D. W.; Delory, G. T.; Demcak, Stuart; DeWolfe, A. W.; Eparvier, F. G.; Ergun, R. E.; Eriksson, Anders; Espley, J. R.; Fang, Xiaohua; Folta, David; Fox, Jane L.; Gomez-Rosa, Carlos; Habenicht, S.; Halekas, J. S.; Holsclaw, Gregory M.; Houghton, M. B.; Howard, R. A.; Jarosz, M.; Jedrich, Nicholas M.; Johnson, Micah; Kasprzak, W. T.; Kelley, M. S.; King, Todd; Lankton, M. R.; Larson, D. E.; Leblanc, François; Lefèvre, Franck; Lillis, R. J.; Mahaffy, P. R.; Mazelle, C.; McClintock, W. E.; McFadden, J. P.; Montmessin, Franck; Morrissey, James R.; Peterson, W. K.; Possel, W.; Sauvaud, J. A.; Schneider, Nicholas M.; Sidney, Wayne; Sparacino, S.; Stewart, A. I. F.; Tolson, R.; Toublanc, D.; Waters, C.; Woods, Thomas N.; Yelle, R. V.; Zurek, Richard W.

doi:10.1007/s11214-015-0139-x

Cited by 678 publications

(616 citation statements)

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“…This has been predicted by many models for the last 45 years, which are too numerous to cite here [e.g., McElroy, 1972;McElroy et al, 1977;Fox and Dalgarno, 1979;Krasnopolsky, 2002;Matta et al, 2013;Bougher et al, 2014;, and confirmed by measurements made by the Neutral Gas and Ion Mass Spectrometer (NGIMS) instrument [e.g., Mahaffy et al, 2015] on the Mars Atmosphere and Volatiles EvolutioN (MAVEN) spacecraft [e.g., Jakosky et al, 2015]. This has been predicted by many models for the last 45 years, which are too numerous to cite here [e.g., McElroy, 1972;McElroy et al, 1977;Fox and Dalgarno, 1979;Krasnopolsky, 2002;Matta et al, 2013;Bougher et al, 2014;, and confirmed by measurements made by the Neutral Gas and Ion Mass Spectrometer (NGIMS) instrument [e.g., Mahaffy et al, 2015] on the Mars Atmosphere and Volatiles EvolutioN (MAVEN) spacecraft [e.g., Jakosky et al, 2015].…”

Section: Introductionmentioning

confidence: 56%

Photochemical determination of O densities in the Martian thermosphere: Effect of a revised rate coefficient

Fox

Johnson

Ard

et al. 2017

Geophysical Research Letters

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We investigate the production and loss rates of O2+ in the photochemical equilibrium region of the Martian ionosphere near the subsolar point. We adopt neutral and ion densities measured by the Mars Atmosphere and Volatiles EvolutioN (MAVEN) Neutral Gas and Ion Mass Spectrometer (NGIMS), electron densities and temperatures measured by the Langmuir Probe and Waves, and ion temperatures measured by the Supra‐Thermal and Thermal Ion Composition instruments on the MAVEN spacecraft. Contrary to the conventional wisdom, we find that loss of O2+ by dissociative recombination is balanced mainly by production due to the reaction of O+ with CO2, with a smaller contribution due to the reaction of CO2+ with O. We find that the O densities derived from this calculation are larger than those measured by the NGIMS instrument by a factor that averages about 4 over the range of 130–155 km. This general conclusion is supported by a newly measured rate coefficient for the reaction of O with CO2+, which is smaller by a factor of about 6 than the only value in the literature, which was measured 47 years ago.

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Section: Introductionmentioning

confidence: 56%

Photochemical determination of O densities in the Martian thermosphere: Effect of a revised rate coefficient

Fox

Johnson

Ard

et al. 2017

Geophysical Research Letters

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“…A dedicated aeronomy and solar wind interaction mission similar to MAVEN (Mars Atmosphere and Volatile Evolution Mission) launched to Mars in 2013 (Jakosky et al 2015) is still to be conducted. Such a VEX-like mission with lower periapsis that drifts in latitude around Venus so as to cover both the north and south poles, noon and midnight sectors, and terminator regions-and of course that observes during a full solar cycle is desired.…”

Section: Future Missions and Open Questionsmentioning

confidence: 99%

Solar Wind Interaction and Impact on the Venus Atmosphere

et al. 2017

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Venus has intrigued planetary scientists for decades because of its huge contrasts to Earth, in spite of its nickname of "Earth's Twin". Its invisible upper atmosphere and space environment are also part of the larger story of Venus and its evolution. In 60s to 70s, several missions (Venera and Mariner series) explored Venus-solar wind interaction regions. They identified the basic structure of the near-Venus space environment, for example, existence of the bow shock, magnetotail, ionosphere, as well as the lack of the intrinsic magnetic field. A huge leap in knowledge about the solar wind interaction with Venus was made possible by the 14-year long mission, Pioneer Venus Orbiter (PVO), launched in 1978. More recently, ESA's probe, Venus Express (VEX), was inserted into orbit in 2006, operated for 8 years.Owing to its different orbit from that of PVO, VEX made unique measurements in the polar and terminator regions, and probed the near-Venus tail for the first time. The near-tail hosts dynamic processes that lead to plasma energization. These processes in turn lead to the loss of ionospheric ions to space, slowly eroding the Venusian atmosphere. VEX carried an ion spectrometer with a moderate mass-separation capability and the observed ratio of the escaping hydrogen and oxygen ions in the wake indicates the stoichiometric loss of water from Venus. The structure and dynamics of the induced magnetosphere depends on the prevailing solar wind conditions. VEX studied the response of the magnetospheric system on different time scales. A plethora of waves was identified by the magnetometer on VEX; some of them were not previously observed by PVO. Proton cyclotron waves were seen far upstream of the bow shock, mirror mode waves were observed in magnetosheath and whistler mode waves, possibly generated by lightning discharges were frequently seen. VEX also encouraged renewed numerical modeling efforts, including fluid-type of models and particle-fluid hybrid type of models, describing the plasma interaction on scales ranging from ion gyro radius to the entire induced magnetosphere. In this review article, we review what has been found from space physics measurements around Venus (from the solar wind down to the ionopause), with a particular emphasis on updated results since the Venus Express mission. We conclude the article by a short discussion on the remaining open scientific questions and the future of this field.

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“…The Mars Atmosphere and Volatile EvolutioN (MAVEN) mission was designed to study the response of Mars' upper atmosphere to solar influences 7 , which also renders it capable of detecting the influence of IDPs. This capability was clearly demonstrated during the exceptionally close pass of comet C/2013 A1 (Siding Spring) by Mars in 2014, and the ensuing meteor shower 8,9,10,11 .…”

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confidence: 99%

Detection of a persistent meteoric metal layer in the Martian atmosphere

et al. 2017

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Article:Cristmani, MMJ, Schneider, NM, Plane, JMC orcid.org/0000-0003-3648-6893 et al. (13 more authors) (2017) Detection of a persistent meteoric metal layer in the Martian atmosphere. Nature Geoscience, 10 (6). pp. 401-404. ISSN 1752-0894 https://doi.org/10.1038/ngeo2958 © 2016 Macmillan Publishers Limited. All rights reserved. This is an author produced version of a paper published in Nature Geoscience. Uploaded in accordance with the publisher's self-archiving policy.eprints@whiterose.ac.uk https://eprints.whiterose.ac.uk/ Reuse Unless indicated otherwise, fulltext items are protected by copyright with all rights reserved. The copyright exception in section 29 of the Copyright, Designs and Patents Act 1988 allows the making of a single copy solely for the purpose of non-commercial research or private study within the limits of fair dealing. The publisher or other rights-holder may allow further reproduction and re-use of this version -refer to the White Rose Research Online record for this item. Where records identify the publisher as the copyright holder, users can verify any specific terms of use on the publisher's website. TakedownIf you consider content in White Rose Research Online to be in breach of UK law, please notify us by emailing eprints@whiterose.ac.uk including the URL of the record and the reason for the withdrawal request. 11,14,15,16,17 and all data used herein are available on the NASA Planetary Data System. Detection of a persistent meteoric metal Detection and Variability of Mg +Emission from Mg + was reliably detected in every periapse limb scan obtained over one Mars year (two Earth years; Figures 1, 3) whenever the Mg + layer was appropriately illuminated and the instrument orientation did not introduce excessive scattered solar continuum (for these purposes, stray light). The Mg + emission feature, centered on 280 nm, is due to resonant scattering of solar UV photons rather than direct excitation during ablation. Mg + brightnesses were extracted from a model spectrum fit (Figure 1a,b), using line positions and atomic constants of known emitters in this spectral region plus a stray light solar spectrum 15,16,18 .The Mg + emission brightness was converted to local ion density through an Abel transform, common in the study of optically thin airglow emissions 19 (see SI). The Mg + layer has a mean peak concentration of ~250 cm -3 and is typically found near an altitude of 90 km (Figure 2). Reported altitudes carry a 2.5 km uncertainty consistent with slit averaging in 5 km bins 16 . Figure 3 shows the derived densities in a fixed altitude range over the course of the mission. Brightness measurements carry Poisson random uncertainties propagated through a multiple linear regression technique and Abel transform. In addition, the brightnesses are subject to 30% systematic uncertainty in absolute calibration (not shown in figure error sizes) 14 . The random and systematic uncertainties propagate linearly into densities and other derived quantities.Observations of Mg + density demonstrate ...

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The Mars Atmosphere and Volatile Evolution (MAVEN) Mission

Cited by 678 publications

References 78 publications

Photochemical determination of O densities in the Martian thermosphere: Effect of a revised rate coefficient

Photochemical determination of O densities in the Martian thermosphere: Effect of a revised rate coefficient

Solar Wind Interaction and Impact on the Venus Atmosphere

Detection of a persistent meteoric metal layer in the Martian atmosphere

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