Variability of D and H in the Martian upper atmosphere observed with the MAVEN IUVS echelle channel

Clarke, J. T.; Mayyasi, Majd; Bhattacharyya, Dolon; Schneider, Nicholas M.; McClintock, William E.; Deighan, Justin; Stewart, A. I. F.; Chaufray, Jean‐Yves; Chaffin, Michael; Jain, Sonal; Stiepen, Arnaud; Crismani, Matteo; Holsclaw, Gregory M.; Montmessin, Franck; Jakosky, B. M.

doi:10.1002/2016ja023479

Cited by 78 publications

(77 citation statements)

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“…The Sun's ~28 day rotation period exposes Mars to varying solar UV flux depending on active regions and their distribution (e.g., Fröhlich & Lean, ). Since D is produced from photodissociation of water isotopologues and subsequent chemical reactions, a small‐scale (day‐to‐day) variability in D brightness may be attributed to the solar rotation cycle (Clarke et al, ). To remove the effects of this variability, averages of the observations were made for each continuous block of 28 days.…”

Section: Resultsmentioning

confidence: 99%

“…Mars hydrogen and water spectral lines are bright and have been observed using ground‐based, space‐based, and remote sensing instruments for decades (Bertaux & Montmessin, ; Clarke et al, , , ; Krasnopolsky, ; Mahaffy et al, ; Novak et al, ; Owen et al, ; Villanueva et al, ; Webster et al, ). Recent discoveries have found there to be a seasonal dependence to the H abundance in the Martian exosphere and lower atmosphere (Aoki et al, ; Chaffin et al, , ; Clarke et al, , ; Fedorova et al, ; Halekas, ; Maltagliati et al, , ; Montmessin et al, ; Villanueva et al, ). Until recently, there were limited observations of D Lyman α emissions from the upper atmosphere of Mars (Bertaux et al, ; Clarke et al, ; Krasnopolsky et al, ).…”

Section: Introductionmentioning

confidence: 99%

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The Variability of Atmospheric Deuterium Brightness at Mars: Evidence for Seasonal Dependence

et al. 2017

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The enhanced ratio of deuterium to hydrogen on Mars has been widely interpreted as indicating the loss of a large column of water into space, and the hydrogen content of the upper atmosphere is now known to be highly variable. The variation in the properties of both deuterium and hydrogen in the upper atmosphere of Mars is indicative of the dynamical processes that produce these species and propagate them to altitudes where they can escape the planet. Understanding the seasonal variability of D is key to understanding the variability of the escape rate of water from Mars. Data from a 15 month observing campaign, made by the Mars Atmosphere and Volatile Evolution Imaging Ultraviolet Spectrograph high‐resolution echelle channel, are used to determine the brightness of deuterium as observed at the limb of Mars. The D emission is highly variable, with a peak in brightness just after southern summer solstice. The trends of D brightness are examined against extrinsic as well as intrinsic sources. It is found that the fluctuations in deuterium brightness in the upper atmosphere of Mars (up to 400 km), corrected for periodic solar variations, vary on timescales that are similar to those of water vapor fluctuations lower in the atmosphere (20–80 km). The observed variability in deuterium may be attributed to seasonal factors such as regional dust storm activity and subsequent circulation lower in the atmosphere.

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Variability of Atmospheric Deuterium Brightness at Mars: Evidence for Seasonal Dependence

et al. 2017

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“…Simultaneous vertical profile measurements of H 2 O, HDO and the atmospheric temperature by NOMAD will help to investigate the escape processes and evaluate upward fluxes and vertical diffusion up to the exobase. Combined with the MAVEN observations of D/H, obtained by direct measurement of the D and H Ly α emissions (Clarke et al 2017), these observations will provide a unique way to understand the escape processes at play from the lower atmosphere up to the uppermost layers.…”

Section: Water Cyclementioning

confidence: 98%

“…NOMAD will also be able to detect such increase of water abundance, and with concurrent observation of H 2 O and HDO, NOMAD will deliver D/H vertical profiles up to the higher layers of the atmosphere. Combining these observations with MAVEN measurements of D and H Ly α emissions (Clarke et al 2017), will allow a global view and understanding of the variability of the D/H ratio within the Martian atmosphere from the surface up to the highest layers of the atmosphere, giving some insights on the history of water on planet Mars. Moreover, NOMAD will enable us to derive temperatures from the CO 2 density measurements (see for example for similar results from the SOIR observations of Venus).…”

Section: Expected Performancementioning

confidence: 99%

NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Vandaele¹,

Moreno²,

Patel³

et al. 2018

Space Sci Rev

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114

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The NOMAD ("Nadir and Occultation for MArs Discovery") spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the comThis paper is dedicated to the memory of M. Allen, V. Formisano, and J. McConnell. position of Mars' atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.

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“…The difference in mass, vertical distribution, and chemistry determines the differential escape of D and H. ACS will simultaneously measure the H 2 O and HDO vertical profiles from the surface up to 60 km. These measurements become increasingly powerful when coupled with the measurements of D and H performed by the MAVEN IUVS instrument at higher altitudes (see Clarke et al 2017). By measuring jointly HDO and H 2 O ACS will uniquely constrain the physics of the HDO cycle.…”

Section: "Novel" Acs Sciencementioning

confidence: 99%

The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

et al. 2017

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The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 µm-the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7-1.6 µm spectral range with a resolving power of ∼20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2-4.4 µm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7-17 µm with apodized resolution varying from 0.2 to 1.3 cm −1 . TIRVIM is primarily dedicated to profiling temperature from the surface up to ∼60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrument, its accommodation on the spacecraft, the optical designs as well as some of the calibrations, and the expected performances for its three channels are described.

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Variability of D and H in the Martian upper atmosphere observed with the MAVEN IUVS echelle channel

Cited by 78 publications

References 34 publications

The Variability of Atmospheric Deuterium Brightness at Mars: Evidence for Seasonal Dependence

The Variability of Atmospheric Deuterium Brightness at Mars: Evidence for Seasonal Dependence

NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

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