PS4.4 | Scientific results from the Emirates Mars Mission primary mission
EDI
Scientific results from the Emirates Mars Mission primary mission
Convener: Bruce Jakosky | Co-conveners: Krishnaprasad ChirakkilECSECS, Maryam YousufECSECS
Orals
| Tue, 25 Apr, 08:30–12:30 (CEST)
 
Room 1.34
Posters on site
| Attendance Tue, 25 Apr, 16:15–18:00 (CEST)
 
Hall X4
Posters virtual
| Attendance Tue, 25 Apr, 16:15–18:00 (CEST)
 
vHall ST/PS
Orals |
Tue, 08:30
Tue, 16:15
Tue, 16:15
The Emirates Mars Mission spacecraft orbiting Mars will complete its primary science mission (one Mars year) in early 2023. Scientific observations emphasize measurements of the behavior of the atmosphere, including the lower atmosphere down to the surface (and including interactions with the surface), the upper atmosphere and ionosphere, and the magnetosphere and interactions with the solar wind. The focus is on understanding diurnal, geographical (latitude/longitude/local solar time), and temporal variations, and the physical and dynamical coupling between the different components of the atmosphere and upper atmosphere, throughout a Mars year. This session will focus on the major scientific results from the mission and plans for the extended mission.

Orals: Tue, 25 Apr | Room 1.34

Chairpersons: Krishnaprasad Chirakkil, Maryam Yousuf
Results from the Emirates Mars Mission: Orals I
08:30–08:35
08:35–08:55
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EGU23-4883
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ECS
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solicited
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Highlight
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On-site presentation
Hessa Almatroushi, Justin Deighan, Greg Holsclaw, Christopher Edwards, and Michael Wolff and the EMM Science Team

In April 2023, the Emirates Mars Mission (EMM) completes its primary science mission observing the Martian atmosphere with global coverage examining the diurnal and seasonal variations throughout one full Martian year. The mission has disseminated publicly more than 1 TB of scientific data combined from three scientific instruments studying the atmosphere of Mars from ultraviolet, visible, and infrared bands. The measurements are taken from a highly elliptical orbit (20,000 km periapse and 43,000 km apoapse) providing unprecedented local and seasonal time coverage over most of the planet. Here we summarize the discoveries and key results from the primary science mission of EMM revealing atmospheric behavior and connections that challenge existing models and assumptions that we have of the Martian atmosphere and form new global perspective of the planet. We will also highlight the status of the mission and recent updates on its extended science phase.

How to cite: Almatroushi, H., Deighan, J., Holsclaw, G., Edwards, C., and Wolff, M. and the EMM Science Team: Emirates Mars Mission - Hope Probe - in a Martian Year, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-4883, https://doi.org/10.5194/egusphere-egu23-4883, 2023.

08:55–09:05
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EGU23-9200
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On-site presentation
Michael Chaffin, Justin Deighan, Sonal Jain, Greg Holsclaw, Raghuram Susarla, Hoor AlMazmi, Krishnaprasad Chirakkil, John Correira, Scott England, Frank Eparvier, J. Scott Evans, Matt Fillingim, Rob Lillis, Fatma Lootah, Ed Thiemann, Shannon Curry, and Hessa AlMatroushi

The surface of the planet Mars exhibits a record of dessiccation and oxidation, the legacy of significant water escape to space as hydrogen and oxygen. This H escape can be constrained using ultraviolet observations of the planet's upper atmosphere, where neutral atomic hydrogen scatters UV sunlight. In the time since its orbit insertion in early 2021, the Emirates Mars Ultraviolet Spectrometer (EMUS) on the Emirates Mars Mission (EMM) has been observing this hydrogen at 102.6 nm and 121.6 nm, H Lyman beta and Lyman alpha. Here we present H escape rates retrieved from these observations, obtained using a 3D radiative transfer model that simulates the brightness of both spectral lines, combining their information content to constrain the atmospheric state. In agreement with past results, we find that H escape peaks around Southern Summer solstice, after perihelion, exhibiting a more than 10x increase relative to Northern Summer conditions. Importantly, our retrievals extract information about both the hydrogen density and temperature, and do not require independent assumptions about the upper atmosphere temperature. We will discuss prospects for extending these retrievals beyond the current EMM dataset as well as implications for the long-term evolution of the Mars atmosphere.

How to cite: Chaffin, M., Deighan, J., Jain, S., Holsclaw, G., Susarla, R., AlMazmi, H., Chirakkil, K., Correira, J., England, S., Eparvier, F., Evans, J. S., Fillingim, M., Lillis, R., Lootah, F., Thiemann, E., Curry, S., and AlMatroushi, H.: Hydrogen Escape Rates 2021-2023 Retrieved from Emirates Mars Mission Observations, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-9200, https://doi.org/10.5194/egusphere-egu23-9200, 2023.

09:05–09:15
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EGU23-10598
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On-site presentation
Sonal Jain, Justin Deighan, Michale Chaffin, Greg Holsclaw, Rob Lillis, Matthew Fillingim, Scott England, Hoor Al Mazmi, Fatma Lootah, Roger Yelle, Sumedha Gupta, Nick Schneider, and Hessa Al Matroushi
The major scientific objective of the Emirates Mars Mission (EMM) is to explore the global atmospheric dynamics of the Martian atmosphere both in short term (diurnal) and long term (seasonal). The Emirates Mars Ultraviolet Spectrometer (EMUS) instrument on board the EMM makes two-dimensional images ( in extreme and far ultraviolet wavelengths: 90-170 nm) of the Martian disk and exosphere to characterize the neutral densities in the thermosphere and exosphere of Mars. In this paper, we will present the first results from the stellar occultation measurements made by the EMUS instruments in October 2022. These occultation observations were not part of the original science planning and were added as a bonus EMM science. A total of seven stellar occultations were performed during the two EMM orbits spanning between 24 to 27 October. These measurements were the first stellar occultation of Mars in the EUV wavelengths (90-110 nm). Due to the higher sensitivity of the EMUS instrument, the occultation measurements were able to probe the atmosphere with an altitude sampling of 2 km or lower. The occultation measurements by SPICAM/MEx and IUVS/MAVEN were limited to 160 km due to wavelengths limited to a longward of 110 nm.  However, the use of EUV wavelengths in the EMUS stellar occultation provided atmospheric probing up to 190 km thus enabling neutral density retrieval up to the exobase region of Mars. The CO2 densities are retrieved from 90-185 km and the temperature profiles were retrieved using the constraint of hydrostatic equilibrium to the CO2 densities. We shall discuss results from the EMUS occultation campaign specifically the observed variability in the CO2 density and temperature during the occultation campaign.

How to cite: Jain, S., Deighan, J., Chaffin, M., Holsclaw, G., Lillis, R., Fillingim, M., England, S., Al Mazmi, H., Lootah, F., Yelle, R., Gupta, S., Schneider, N., and Al Matroushi, H.: The first EMM/EMUS stellar occultation measurements of the Martian atmosphere in both extreme and far ultraviolet wavelengths, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-10598, https://doi.org/10.5194/egusphere-egu23-10598, 2023.

09:15–09:25
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EGU23-8470
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On-site presentation
Robert Lillis, Abigail Azari, Yingjuan Ma, Krishnaprasad Chirakkil, Justin Deighan, Michael Chaffin, Sonal Jain, Gregory Holsclaw, David Brain, Hessa Al Matroushi, Scott England, Nick Schneider, Shaosui Xu, Hoor Al Mazmi, Jasper Halekas, Robin Ramstad, Jared Espley, Jacob Gruesbeck, and Shannon Curry

Benefiting from a large orbit and high sensitivity, the Emirates Mars mission EMUS instrument has provided the first opportunity to regularly image Mars’ discrete FUV aurora synoptically.  EMUS has collected nearly 1000 synoptic observations of the Mars nightside have revealed at least three distinct types of discrete Aurora: 1) crustal field aurora, appearing in regions of mostly radial crustal magnetic fields, 2) patchy discrete aurora, observed away from strong crustal fields, and 3) sinuous discrete aurora, extending from the terminator typically thousands of kilometers onto the nightside, away from crustal fields.

Sinuous Discrete Aurora (SDA) is observed in approximately 5% of observations and is characterized by 2 primary attributes: morphology and the local time of its intersection with the terminator. Morphologies include serpentine, approximately linear, and short/lumpy. Dusk-side SDA does not occur preferentially for any particular interplanetary magnetic field (IMF) orientation, while Dawn and Midnight SDA appear to show a preference for northeastward IMF directions measured in situ by the MAVEN spacecraft. Dusk SDA observed about twice as often as Dawn or Midnight SDA. 

SDA reflect conditions whereby particular magnetic topologies connect the nightside atmosphere to a source of abundant electrons, whether dayside photoelectrons or sufficiently energetic magnetotail/sheath electrons.  In particular, midnight sinuous discrete aurora appear to be a projection of the tail current sheet, a persistent but highly variable feature of Mars’ double-lobed magnetotail resulting from the draping of the IMF around the conducting obstacle of Mars’ dayside ionosphere.  This interpretation is supported by magnetohydrodynamic (MHD) simulations, showing that the orientation of the tail current sheet approximately matches the orientation of midnight SDA.

EMM EMUS promises to be an invaluable tool in helping to understand the drivers of Martian Aurora.

How to cite: Lillis, R., Azari, A., Ma, Y., Chirakkil, K., Deighan, J., Chaffin, M., Jain, S., Holsclaw, G., Brain, D., Al Matroushi, H., England, S., Schneider, N., Xu, S., Al Mazmi, H., Halekas, J., Ramstad, R., Espley, J., Gruesbeck, J., and Curry, S.: Sinuous Aurora at Mars: exploring a new phenomenon with data and models, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-8470, https://doi.org/10.5194/egusphere-egu23-8470, 2023.

09:25–09:35
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EGU23-2149
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On-site presentation
Matthew Fillingim, Robert Lillis, Anna Mittelholz, Hessa AlMatroushi, Hoor AlMazmi, Michael Chaffin, Peter Chi, Krishnaprasad Chirakkil, John Corriera, Justin Deighan, Scott England, Scott Evans, Heidi Haviland, Greg Holsclaw, Sonal Jain, Catherine Johnson, Steven Joy, Benoit Langlais, Fatma Lootah, and Susarla Raghuram

The Emirates Mars Ultraviolet Spectrometer (EMUS) onboard the Emirates Mars Mission spacecraft, which observes ultraviolet emission between approximately 100 and 170 nm, has observed multiple instances of nightside aurora at Mars. Variations in the auroral brightness and morphology have been observed to change on timescales of tens of minutes. The brightest aurorae are typically seen following space weather events, i.e., coronal mass ejection and stream interaction region impacts. The InSight Fluxgate Magnetometer (IFG) on the Interior Explorations using Seismic Investigations, Geodesy and Heat Transport (InSight) lander measured the magnetic field at the surface of Mars. IFG has measured variations in the nightside surface magnetic field, presumably due to variations in ionospheric and magnetospheric currents. Periodic and aperiodic variations in the surface field have been observed, including with timescales of a few minutes to tens of minutes. The magnitude of the fluctuations is often larger following space weather events. We examine the connection between the presence of aurora as observed by EMUS and surface magnetic field fluctuations as measured by IFG. Coincident EMUS and IFG observations show enhanced surface magnetic field fluctuations during times when aurorae were present. Additionally, the timescale of fluctuations in the auroral brightness are similar to the timescale of surface magnetic field fluctuations for non-coincident observations. These results suggest that IFG measured the surface magnetic field effect of time varying ionospheric auroral currents.

How to cite: Fillingim, M., Lillis, R., Mittelholz, A., AlMatroushi, H., AlMazmi, H., Chaffin, M., Chi, P., Chirakkil, K., Corriera, J., Deighan, J., England, S., Evans, S., Haviland, H., Holsclaw, G., Jain, S., Johnson, C., Joy, S., Langlais, B., Lootah, F., and Raghuram, S.: Auroral currents from EMM and InSight: A comparison of EMM-EMUS auroral observations and InSight-IFG magnetic field fluctuations, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-2149, https://doi.org/10.5194/egusphere-egu23-2149, 2023.

09:35–09:45
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EGU23-1815
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Virtual presentation
Michael Wolff, Andrew Jones, Mikki Osterloo, Ralph Shuping, Christopher Edwards, Mariam Al Shamsi, Joey Espejo, Charles Fisher, Christopher Jeppesen, and Justin Knavel

The EXI instrument onboard the Emirates Mars Mission (EMM) spacecraft has been operating for a full Martian year.  Using the elliptical orbit, EXI has observed the atmosphere and surface of Mars at both regional and global scales while providing a unique diurnal sampling.  This diurnal coverage is available over much of the planet on a time scale of approximately ten days.  The observations are typically taken in both the ultraviolet and visible: 260, 320, 437, 546, and 635 nm, with an effective spatial resolution of 2–4 km per native pixel.  This presentation will provide an overview of EXI’s on-orbit activities and performance during the first Mars year of science operations, a summary of the diurnal behavior of seasonal trends in water ice clouds, and some examples of the combined analysis of EXI and Emirates Mars InfraRed Spectrometer (EMIRS) observations.  More specifically, we will cover the following:

 

  • The multiple types of observational modes employed, statistics of the images obtained and available in the EMM Science Data Center, and the radiometric performance of the camera as measured by the standard star observation program.

 

  • The diurnal trends are associated with the seasonal behavior of water ice clouds through a Martian year, including the aphelion and perihelion seasons.

 

  • The advantages and challenges of combining the EXI and EMIRS observations for atmospheric and surface studies, where the Instantaneous Field of View differs by one-to-two orders of magnitude.

 

Funding for the development of the EMM mission was provided by the UAE government and to co-authors outside of the UAE by the Mohammed bin Rashid Space Center (MBRSC).

How to cite: Wolff, M., Jones, A., Osterloo, M., Shuping, R., Edwards, C., Al Shamsi, M., Espejo, J., Fisher, C., Jeppesen, C., and Knavel, J.: One Martian Year of Observations by the Emirates eXploration Imager (EXI): Operations Summary, Current Status, and Seasonal Trends in the Diurnal Behavior of Water Ice Clouds, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-1815, https://doi.org/10.5194/egusphere-egu23-1815, 2023.

09:45–09:55
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EGU23-15008
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ECS
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On-site presentation
Alia Almansoori, Michael Rothman, Dave Brain, Michael Wolff, Aurélien Stcherbinine, and Justin Deighan

Observations of clouds in planetary atmospheres can provide insight about atmospheric characteristics such as vertical temperature structure and dynamics. Clouds observed at the limb of a planet (from the perspective of the telescope or spacecraft observing them) can be particularly useful tools, in part because their height above the surface can be measured directly.

The Emirates Mars Mission (EMM) has been recording visible light images of the Martian disk since early 2021, using the Emirates eXploration Imager (EXI). We present an analysis of limb clouds evident in EXI images taken using its red filter (centered on 635 nm) over the course of a Martian year. We present statistics on their height, thickness, spatial extent, and geographic and local time distribution – as well as correlations between these parameters. We place our results in context with previous work, and explore reasons for observed trends.

How to cite: Almansoori, A., Rothman, M., Brain, D., Wolff, M., Stcherbinine, A., and Deighan, J.: Properties of Limb Clouds at Mars determined from the Emirates Mars Mission (EMM) eXploration Imager (EXI), EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-15008, https://doi.org/10.5194/egusphere-egu23-15008, 2023.

09:55–10:15
Results from the Emirates Mars Mission: Orals II
Coffee break
Chairpersons: Maryam Yousuf, Krishnaprasad Chirakkil
10:45–10:50
10:50–11:10
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EGU23-9807
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solicited
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On-site presentation
Christopher Edwards, Mikki Osterloo, Charles Fisher, Chris Jeppesen, Nathan Smith, Greg Holsclaw, Michael Wolff, Andrew Jonees, Justin Knavel, Emily Pilinski, Daniel Kubitschek, Thibaud Teil, Justin Deighan, Hessa Al Matroushi, Jeff Parker, Philip Christensen, Saadat Anwar, Heather Reed, Pete Withnell, and Omran Sharaf

The origins of the martian moons Phobos and Deimos remain enigmatic. Over the past decades a range of spacecraft have observed Phobos and Deimos in order to constrain their origin and evolutionary history, with proposals for their origins ranging from captured asteroids, to coalesced material from a giant impact on Mars. However, given the orbits these spacecraft and the orbits of Phobos and Deimos, Phobos has garnered the majority of the attention. Now thanks to the unique orbit of the Emirates Mars Mission (EMM) Hope spacecraft and a minor correction to its nominal science orbit, EMM has a unique opportunity to examine Deimos in great detail while fully retaining the originally designed mission to capture the variability in the martian atmosphere and exosphere.

Following a minor orbital adjustment maneuver campaign beginning in August 2022, EMM will encounter Deimos multiple times, progressively observing the martian moon at lower and lower distances beginning in early 2023. These flybys culminate in the closest approach of ~150 km, observing the mostly illuminated, far side of Deimos. All three EMM instruments, the Emirates eXploration Imager (EXI), the Emirates Mars Infrared Spectrometer (EMIRS), and the Emirates Ultraviolet Spectrometer (EMUS) have observation sequences tailored to these flybys, collecting the highest resolution multispectral visible imaging data, thermal infrared surface temperatures and emission spectra, and ultraviolet spectra.  When combined these instrument observations will provide key insights into the composition, morphology, and surface physical properties of the least studied martian moon, Deimos.

How to cite: Edwards, C., Osterloo, M., Fisher, C., Jeppesen, C., Smith, N., Holsclaw, G., Wolff, M., Jonees, A., Knavel, J., Pilinski, E., Kubitschek, D., Teil, T., Deighan, J., Al Matroushi, H., Parker, J., Christensen, P., Anwar, S., Reed, H., Withnell, P., and Sharaf, O.: The First Observations of Deimos from the Emirates Mars Mission (EMM) Flybys, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-9807, https://doi.org/10.5194/egusphere-egu23-9807, 2023.

11:10–11:20
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EGU23-3092
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On-site presentation
Khalid Badri, Michael Smith, Christopher Edwards, Eman AlTunaiji, and Philip Christensen

The Emirates Mars Mission (EMM) is on its way to achieving 1 Martian year of Scientific Observations by the end of April 2023 to explore the dynamics of the Martian atmosphere on a global scale. The Emirates Mars Infrared Spectrometer (EMIRS) instrument onboard EMM, is an interferometric thermal infrared spectrometer designed to characterize the geographic, seasonal, and diurnal variability of key characteristics of Mars such as atmospheric dust, which will be the focus of this talk, and other constituents such as water ice optical depth, water vapor abundance, surface temperature, and atmospheric temperature profiles on sub-seasonal timescales.  

EMIRS observations provide full local solar time coverage at multiple emission angles providing data on these constituents over the entire Martian disk. Here, we present initial results of the spatial, seasonal and diurnal variation of dust on a global scale with particular attention to the diurnal variations of dust and the evolution of dust storms. Preliminary results show more diurnal variations during dust storm seasons. In addition, results on the biggest storm of the year will be presented which occurred after solar longitude of 300.  These new observations will continue to enhance our understanding of the dust cycle on Mars and how dust influences the current climate and atmospheric dynamics on Mars by relating the effect of dust to other EMIRS constituents mentioned above.

How to cite: Badri, K., Smith, M., Edwards, C., AlTunaiji, E., and Christensen, P.: The Spatial and Diurnal Distribution of Lower Atmospheric Dust as Revealed by the Emirates Mars Infrared Spectrometer, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-3092, https://doi.org/10.5194/egusphere-egu23-3092, 2023.

11:20–11:30
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EGU23-2640
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ECS
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On-site presentation
Bijay Kumar Guha, Claus Gebhardt, Roland M. B. Young, and Michael J. Wolff

Abstract: The Emirates eXploration Imager (EXI) onboard EMM is a multi-wavelength double lens camera suitable for observing the Martian lower atmospheric phenomena such as dust storms [3, 5]. The spacecraft’s unique orbit allows the EXI camera a full disk view of Mars at a time step of hours or less through its visible and UV channels (at ~2-4 km per pixel resolution). Therefore, we have used these unprecedented observations to characterize the dust storms for a one Martian-year period [4, 6]. Our dust storm research is directly aligned with the EMM science objective on the lower atmosphere and also with the objective of correlating the lower and upper atmosphere [1, 2]. In this study, we have prepared a one Martian year of dust storm database from EMM-EXI images. The dust storm database includes the start and end time of dust storms, their area, and the centroid latitude and longitude. Here, we also focused on characterizing the dust storms at a sub-daily time scale (which has not been emphasized before) by tracking their evolution at multiple local times. In addition, we consider the origination region, the pathway, and the morphological characteristics of dust storms. Our presentation includes accompanying simulations by a planetary climate model.

References: [1] Almatroushi, H., et al. (2021). Space Science Reviews, 217(8), 1-31. [2] Amiri, H. E. S., et al. (2022). Space Science Reviews, 218, 4 (2022). [3] Gebhardt, C., et al. (2022). Geophysical Research Letters. 49, e2022GL099528. [4] Guha, B. K., et al. (2021). Planetary and Space Science, 209, 105357. [5] Jones, A.R., et al. (2021). Space Science Reviews, 217, 81. [6] Wang, H., & Richardson, M. I. (2015). Icarus, 251, 112-127.

How to cite: Guha, B. K., Gebhardt, C., Young, R. M. B., and Wolff, M. J.: Dust storm statistics based on the EMM camera EXI for a complete Martian Year period, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-2640, https://doi.org/10.5194/egusphere-egu23-2640, 2023.

11:30–11:40
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EGU23-2424
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Virtual presentation
Syed A. Haider, Tariq Majeed, and Siddhi Shah

Recently, Emirates Mars Mission (EMM) arrived at Mars on 9 February 2021. It carried three instruments: (1) Emirates eXploration Imager (EXI), (2) Emirates Mars Infrared Spectrometer (EMIRS), and (3) Emirates Mars Ultraviolet Spectrometer (EMUS). In this paper we have used EMIRS data. The EMIRS instrument is measuring atmospheric temperature (at 0.5 mbar) and the column abundance of dust aerosols (referenced to 9 μm), water ice clouds (referenced to 12 μm), and water vapour (pr-μm). These observations were taken between 24 May, 2021 (MY 36, Ls= ~ 50o) and 24 February, 2022 (MY36, Ls = 180o). There is a gap in these data between Ls = 100o and 120o due to the solar conjunction and the spacecraft entering into safe mode. We have studied the seasonal and diurnal variability of surface temperature and dust aerosols in the Martian atmosphere. These observations are reported at Ls= 5o interval and 2o interval in latitude. The data are averaged over longitude. Our results show that Mars was relatively cool with little dust. The growth and decay of regional dust storms were observed by EMIRS instrument. Based on our analysis we conclude that EMIRS instrument is well suited for the study of temporal and seasonal variability of atmospheric temperature and column integrated quantities of dust. Detailed analysis of these observations will improve our understanding of the underlying physical processes. It will also help to validate and tune GCM models. The EMIRS observations are always providing an exciting new information as we enter the dust perihelion season.  

How to cite: Haider, S. A., Majeed, T., and Shah, S.: EMIRS observations of temperature and dust aerosols: Seasonal and diurnal variability, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-2424, https://doi.org/10.5194/egusphere-egu23-2424, 2023.

11:40–11:50
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EGU23-15830
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On-site presentation
Roland Young, Ehouarn Millour, François Forget, Christopher Edwards, Nathan Smith, Michael Smith, Saadat Anwar, Philip Christensen, and Luca Montabone

The Emirates Mars Mission (EMM) will have spent just over one Martian Year (MY) of science operations by the time the EGU General Assembly begins in late April 2023, having begun its primary science phase in May 2021 or MY36 Ls = 49o. Over this primary phase of the mission, we have been assimilating observations from EMM into the Mars Planetary Climate Model (PCM), using the Local Ensemble Transform Kalman Filter (LETKF), to understand various aspects of Mars' climate. EMM's unique high orbit and viewing geometry make it an extremely valuable source of data for assimilation, as it can observe nearly a whole hemisphere at once, monitor synoptic-scale features for several hours, and sample the whole diurnal cycle over 10 sols. This presentation will focus on the assimilation of atmospheric temperature profiles and column dust optical depth measurements, retrieved from spectral observations made by the Emirates Mars InfraRed Spectrometer (EMIRS), a thermal infrared spectrometer sensitive to 6-50 μm wavelengths on board EMM. We may also include EMIRS surface temperature measurements, and observations from Mars Climate Sounder (MCS) on board Mars Reconnaissance Orbiter (MRO) to fill in gaps in the data record. The assimilation combines EMIRS observations with a climate model in a statistically rigorous way to produce a data product consistent with the uncertainties in both. By measuring the quality of these analyses against assimilated and independent observations, we will highlight how assimilation can be used to inform the future development of our climate simulations.

How to cite: Young, R., Millour, E., Forget, F., Edwards, C., Smith, N., Smith, M., Anwar, S., Christensen, P., and Montabone, L.: One Martian Year of data assimilation with the Emirates Mars Mission, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-15830, https://doi.org/10.5194/egusphere-egu23-15830, 2023.

11:50–12:00
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EGU23-3198
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ECS
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On-site presentation
Siteng Fan, Francois Forget, Michael Smith, Sandrine Guerlet, Khalid Badri, Samuel Atwood, Roland Young, Christopher Edwards, Philip Christensen, Justin Deighan, Hessa Al Matroushi, Antoine Bierjon, Jiandong Liu, and Ehouarn Millour

We present results of diurnal temperature variations and thermal tides in the Martian atmosphere using observations obtained by the Emirates Mars InfraRed Spectrometer (EMIRS) onboard the Emirates Mars Mission (EMM) Hope probe during its primary mission. The novel orbit design of the spacecraft allows a full geography and local time to be covered every 10 Martian days, approximately ~5° of solar longitude (LS). Diurnal temperature variations are derived for the first time on a planetary scale without any significant gaps in local time or interference from seasonal changes. Contributions of thermal tides are then analyzed. The dataset of the EMM primary mission covers one Martian Year (MY) starting from MY 36 LS=49°. Seasonal changes of the diurnal temperature variations and thermal tides are investigated. The results show good agreements with predictions provided by the Mars Planetary Climate Model (PCM), but with noticeable differences in the phases and wavelengths of the thermal tides. This work provides valuable information on understanding the diurnal climate of Mars, and inspires future advances of Mars GCMs.

How to cite: Fan, S., Forget, F., Smith, M., Guerlet, S., Badri, K., Atwood, S., Young, R., Edwards, C., Christensen, P., Deighan, J., Al Matroushi, H., Bierjon, A., Liu, J., and Millour, E.: Diurnal Temperature Variations and Thermal Tides in the Martian Atmosphere Observed by EMIRS during EMM Primary Mission, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-3198, https://doi.org/10.5194/egusphere-egu23-3198, 2023.

12:00–12:10
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EGU23-11074
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On-site presentation
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Dimitra Atri, Nour Abdelmoneim, Dattaraj Dhuri, and Mathilde Simoni
The ~55 hour orbit of the Emirates Mars Mission (EMM) or the “Hope'" orbiter enables it to achieve a near-global coverage of the planet every 4 orbits, or ~9 sols. The Emirates Mars Infrared Spectrometer (EMIRS) instrument on board EMM is used to retrieve surface temperatures. We study the geographical and temporal variation of surface temperature on diurnal and seasonal timescales. We compare these measurements with NASA’s rover measurements —  from the Rover Environmental Monitoring Station (REMS) suite on board the Mars Science Laboratory (MSL) "Curiosity" rover, and the Mars Environmental Dynamics Analyzer (MEDA) suite on board the Mars 2020 "Perseverance” rover. We also compare these measurements with the Mars Climate Database (MCD), identify anomalies in surface temperature and discuss the role of thermal inertia. We discuss other implications of these findings leading to a better understanding of temperature variation on Mars and its impact on weather and climate.  

 

How to cite: Atri, D., Abdelmoneim, N., Dhuri, D., and Simoni, M.: Surface temperature of Mars: Exploring diurnal and seasonal variations with the Emirates Mars Mission, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-11074, https://doi.org/10.5194/egusphere-egu23-11074, 2023.

12:10–12:20
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EGU23-9770
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ECS
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On-site presentation
Aurélien Stcherbinine, Christopher Edwards, Michael Wolff, Eman Altunaiji, Christopher Haberle, Michael Smith, and Philip Christensen

Condensation and sublimation of ices at the surface of the planet is a key part of both the Martian H2O and CO2 cycles, either from a seasonal or diurnal aspect. If most of the ices are located within the polar caps, surface frost is known to be formed during nighttime down to equatorial latitudes. The Emirate Mars InfraRed Spectrometer (EMIRS) instrument onboard the Emirates Mars Mission (EMM) "Hope" probe is a Fourier Transform Infrared spectrometer that is observing the Martian surface and atmosphere between 6 and 100 μm from February 2022. The unique orbit of EMM allows EMIRS to observe the entire Martian disk at each observation, covering all the surface of the planet across all local times in ~ 4 orbits, which corresponds to ~ 5° of Ls.

Here we use the surface temperature data retrieved from the EMIRS spectra (Smith et al. 2022) to detect and map the ice at the surface of the Red Planet. We compute the amplitude of the diurnal temperature variations to derive maps of the presence of ices (either H2O or CO2) at the surface of the planet over the day, which allows us to monitor the seasonal evolution of the polar caps. And, based on the methodology used in Piqueux et al. (2016), we also compute for each EMIRS pixel the corresponding freezing temperature of CO2, according to Clapeyron’s law, and we consider that CO2 ice is present at the surface if the retrieved temperature is below TCO2, ice. This allows us to monitor the timing of the formation and disappearance of the surface CO2 frost under midlatitudes over the Martian night, and its seasonal evolution.

How to cite: Stcherbinine, A., Edwards, C., Wolff, M., Altunaiji, E., Haberle, C., Smith, M., and Christensen, P.: Diurnal and Seasonal Mapping of Martian Ices with EMM/EMIRS, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-9770, https://doi.org/10.5194/egusphere-egu23-9770, 2023.

12:20–12:30

Posters on site: Tue, 25 Apr, 16:15–18:00 | Hall X4

Chairpersons: Krishnaprasad Chirakkil, Maryam Yousuf
Results from the Emirates Mars Mission: Posters (on-site)
X4.327
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EGU23-9313
Mikki Osterloo, Christopher Edwards, Charles Fisher, Chris Jeppesen, Michael Wolff, Andrew Jones, Justin Knavel, Emily Pilinski, Christopher Tomso, Ralph Shuping, Justin Deighan, and Hessa Al Matroushi

The Emirates Mars Mission (EMM) has a unique opportunity to observe the surface of Deimos, the smaller and outermost of the two moons of Mars. The origins of both Phobos and Deimos remain debated largely due to lack of available observations. The elliptical orbit of the EMM spacecraft, designed to provide comprehensive coverage of the martian atmosphere, allows for campaigns to periodically observe the moon. The slight adjustment of the orbit to move into a resonance with Deimos permits nominal science to continue. The campaign began in August of 2022 by undertaking a series of maneuvers to enable several flybys each stepping in and progressively attaining a closer distance to Deimos. Here, we will present the images collected by EXI of the targeted flyby (e.g., the flyby wherein the spacecraft achieves its closest distance to the moon). Observations for each flyby will include an initial image set at the start of the approach (red/green/blue/320 nm/260 nm), red images will be acquired at 1 min intervals during the approach, and when the spacecraft is at the closest point to Deimos a red/green/blue image set at full resolution, as well as a 320 nm image binned at 2×2 pixels, will be acquired. As the spacecraft leaves Deimos, the reverse observation strategy will be employed. These observations will help constrain the short-wavelength spectral properties and further characterize the geomorphology of this relatively understudied martian moon.

How to cite: Osterloo, M., Edwards, C., Fisher, C., Jeppesen, C., Wolff, M., Jones, A., Knavel, J., Pilinski, E., Tomso, C., Shuping, R., Deighan, J., and Al Matroushi, H.: First observations of Deimos from the Emirates eXploration Imager (EXI), EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-9313, https://doi.org/10.5194/egusphere-egu23-9313, 2023.

X4.328
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EGU23-10291
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ECS
Nathan Smith, Christopher Edwards, Mikki Osterloo, Philip Christensen, Saadat Anwar, Emily Pilinski, Paul Wren, Dale Noss, Ken Rios, Scott Dickenshied, Hessa Al Matroushi, Justin Deighan, Jeffrey Parker, and Omran Sharaf

We present the initial views of the surface of Mars’ outer moon Deimos as observed by the Emirates Mars InfraRed Spectrometer (EMIRS), a Fourier transform infrared spectrometer observing from 6-50 µm with a spectral sampling of up to 5 cm-1. The primary science goal of the Emirates Mars Mission (EMM) is to study the variability in Mars’ atmosphere. As part of a coordinated campaign, the EMM spacecraft has adjusted its orbit into a resonance with Deimos, where it will periodically fly by the moon. Beginning the spring of 2023, EMIRS will collect numerous thermal infrared spectra of Deimos’ surface with a spatial resolution ranging from ~1-10 km. These observations will be the best-resolved infrared views of Deimos to date. Our planned observations achieve nearly complete global coverage of the surface, and span a range of local solar times, enabling investigations of both compositional and thermophysical properties. We will discuss these observations and initial findings. 

How to cite: Smith, N., Edwards, C., Osterloo, M., Christensen, P., Anwar, S., Pilinski, E., Wren, P., Noss, D., Rios, K., Dickenshied, S., Al Matroushi, H., Deighan, J., Parker, J., and Sharaf, O.: The Observations of Deimos from the Emirates Mars Infrared Spectrometer (EMIRS), EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-10291, https://doi.org/10.5194/egusphere-egu23-10291, 2023.

X4.329
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EGU23-10186
Gregory Holsclaw, Justin Deighan, Michael Chaffin, Hessa Al Matroushi, Robert Lillis, Matthew Fillingim, Scott England, Sonal Jain, Fatma Lootah, Hoor Al Mazmi, Gabriel Bershenyi, Emily Pilinski, Thibaud Teil, Jeff Parker, and Omran Sharaf

The Emirates Mars Mission (EMM) Hope probe launched on 20 Jul 2020 and entered Mars orbit on 9 Feb 2021, carrying a payload of 3 complementary instruments to characterize the global atmosphere across the full range of altitudes (surface to exosphere) at diurnal and seasonal timescales.  The unique, high-altitude orbit of the Hope probe (19,970 km periapse, 42,650 km apoapse altitude, 25 deg inclination, 54.5-hour period) that enables its synoptic view of the red planet also brings the spacecraft across the orbit of Mars’ outermost moon, Deimos.  The Hope trajectory was slightly modified by two maneuvers in Aug 2022 and Jan 2023 that will allow the surface of Deimos to be observed in a series of flybys in Feb-Mar 2023.  Here we present preliminary results from the Emirates Mars Ultraviolet Spectrometer (EMUS), an imaging spectrograph with a wavelength range of 100-170 nm and a field of view of 10.75 x 0.18 deg (using the high-resolution slit position).  We will derive the absolute reflectance of the surface, search for any compositionally distinct spectral features (e.g. carbon, polycyclic aromatic hydrocarbons, water ice), and examine any spatial heterogeneity across the surface.

How to cite: Holsclaw, G., Deighan, J., Chaffin, M., Al Matroushi, H., Lillis, R., Fillingim, M., England, S., Jain, S., Lootah, F., Al Mazmi, H., Bershenyi, G., Pilinski, E., Teil, T., Parker, J., and Sharaf, O.: The First Observations of Deimos by the Emirates Mars Ultraviolet Spectrometer (EMUS), EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-10186, https://doi.org/10.5194/egusphere-egu23-10186, 2023.

X4.330
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EGU23-5359
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ECS
Maryam Yousuf, Mikki Osterloo, and Christopher Edwards

Observations of clouds on Mars have long been studied to understand activity and the Martian water cycle. The Martian volcanoes have been shown to have associated cloud formations such as the Aphelion Cloud Belt (ACB) (Wolff et al., 2022), Orographic Clouds (Benson et al., 2006), and Perihelion Cloud Trails (Clancy et al., 2021). Previous studies provide insights into how these clouds appear and contribute to the atmosphere. The objective of this study is to provide a catalog of the life cycle of clouds observed by Emirates eXploration Imager (EXI) spatially (longitude, latitude) and temporally (Solar Longitude (Ls), local time) using the following wavelength channels 635nm (red), 546nm (green), 437nm (blue) and 320nm (ultraviolet which can be used to retrieve the water ice optical depth). To undertake this study, we identified the volcanic region (Olympus Mons and Arsia Mons) as the study region due to cloud presence in the area throughout the Martian year.  EXI is a camera on board the Emirates Mars Mission (EMM) – Hope Probe. EXI acquires 12-megapixel images and has sufficient radiometric calibration for detailed scientific analysis (Jones et al., 2021). It was developed to better understand several critical constituents (e.g., dust, water ice clouds, etc) geographic and diurnal distribution in the lower atmosphere (Jones et al., 2021). We will present the results of our database for clouds for Mars year 36.

 

Benson, J., James, P., Cantor, B., & Remigio, R. (2006). Interannual variability of water ice clouds over major martian volcanoes observed by MOC. Icarus, 184(2), 365–371. https://doi.org/10.1016/j.icarus.2006.03.014

Clancy, R. T., Wolff, M. J., Heavens, N. G., James, P. B., Lee, S. W., Sandor, B. J., Cantor, B. A., Malin, M. C., Tyler, D., & Spiga, A. (2021). Mars perihelion cloud trails as revealed by MARCI: Mesoscale topographically focused updrafts and gravity wave forcing of high altitude clouds. Icarus, 362, 114411. https://doi.org/10.1016/j.icarus.2021.114411

Jones, A. R., Wolff, M., Alshamsi, M., Osterloo, M., Bay, P., Brennan, N., Bryant, K., Castleman, Z., Curtin, A., DeVito, E., Drake, V. A., Ebuen, D., Espejo, J., Farren, J., Fenton, B., Fisher, C., Fisher, M., Fortier, K., Gerwig, S., . . . Yaptengco, J. L. (2021). The Emirates Exploration Imager (EXI) Instrument on the Emirates Mars Mission (EMM) Hope Mission. Space Science Reviews, 217(8). https://doi.org/10.1007/s11214-021-00852-5

Wolff, M. J., Fernando, A., Smith, M. D., Forget, F., Millour, E., Atwood, S. A., Jones, A. R., Osterloo, M. M., Shuping, R., Al Shamsi, M., Jeppesen, C., & Fisher, C. (2022). Diurnal Variations in the Aphelion Cloud Belt as Observed by the Emirates Exploration Imager (EXI). Geophysical Research Letters, 49(18). https://doi.org/10.1029/2022gl100477

How to cite: Yousuf, M., Osterloo, M., and Edwards, C.: Diurnal and seasonal variations of clouds in the Tharsis Montes region of Mars using the Emirates eXploration Imager (EXI) observations, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-5359, https://doi.org/10.5194/egusphere-egu23-5359, 2023.

X4.331
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EGU23-10766
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ECS
Michael Rothman, Alia Almansoori, David Brain, and Michael Wolff

The Emirates Mars Mission (EMM) has returned an abundance of whole disk images of Mars at visible wavelengths. Clouds and hazes are evident at the limb of the planet in many of these images, offering an opportunity to determine the vertical distribution of clouds on Mars over the course of a Martian year. However, there are challenges in determining the height of limb clouds due to uncertainty in the location of the Martian surface in the images. This uncertainty comes primarily from small uncertainties in the pointing of the instrument, coupled with the fact that the surface can be difficult to identify in the images due to the opacity of the atmosphere at low altitudes. With a typical pixel spanning roughly 5 km on the limb, the uncertainties in cloud height can be large.

 

Here we present an algorithm for automatically detecting limb clouds and hazes in Emirates eXploration Imager (EXI) observations, while simultaneously detecting the location of the surface. The algorithm considers straight line ‘transects’ through the images that extend from space to the disk of the planet. The inflection point in the recorded intensity along the transect (i.e. from ‘space’ where the intensity is small, to ‘Mars’ where the intensity is large) is used to determine the location of the surface. The transect is also used to infer the presence of detached clouds, as well as surface hazes. The heights and thicknesses of clouds and hazes can be extracted from the transects. We will present the algorithm, as well as a comparison of how the results of the algorithm compare to manual analysis of EXI images. We will highlight where the algorithm does well and where it has difficulty, and how the algorithm might be used to analyze other planetary datasets.

How to cite: Rothman, M., Almansoori, A., Brain, D., and Wolff, M.: Automated Detection of Limb Clouds and Hazes by the Emirates Mars Mission (EMM) Emirates eXploration Imager (EXI), EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-10766, https://doi.org/10.5194/egusphere-egu23-10766, 2023.

X4.332
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EGU23-3053
Claus Gebhardt, Bijay K. Guha, Roland M. B. Young, Michael J. Wolff, and Christopher S. Edwards

Mars dust storms are an interdisciplinary field of research. They impact the entry-descent-landing operations of spacecraft, the energy production by the solar panels of Mars rovers and landers, and others. As can be foreseen, dust storms are also critical for the future human exploration of Mars. Dust storm research is directly aligned with the Emirates Mars Mission (EMM) science objective on the lower atmosphere, and with the science objective of correlating the lower and upper atmosphere [1,2]. First results of EMM dust storm research were reported in [3].

EMM has a high-altitude orbit and provides data products for studies of the Mars atmosphere and surface with a near-hemispheric view. Moreover, EMM can provide information on dust storm activity every few hours or less. EMM observed multiple dust storms during the primary mission, including a large regional dust storm in Sep. and Oct. 2022.

The focus of this presentation are unique dust storm observations by the EMM camera EXI [4]. We study a subset of dust storms, which is of particular interest to our research. The formation and growth of dust storms is followed at a (sub-)hourly time scale. This includes results on the dust storm morphology, wind direction, wind speed, surface dust lifting, etc.. Based on that, the implications for the physics and dynamics of dust storms are considered.

[1] Amiri, H.E.S., Brain, D., Sharaf, O. et al. The Emirates Mars Mission. Space Sci Rev 218, 4 (2022). https://doi.org/10.1007/s11214-021-00868-x

[2] Almatroushi, H., AlMazmi, H., AlMheiri, N. et al. Emirates Mars Mission Characterization of Mars Atmosphere Dynamics and Processes. Space Sci Rev 217, 89 (2021). https://doi.org/10.1007/s11214-021-00851-6

[3] Gebhardt, C., Guha, B. K., Young, R. M. B., & Wolff, M. J. (2022). A frontal dust storm in the northern hemisphere at solar longitude 97—An unusual observation by the Emirates Mars mission. Geophysical Research Letters, 49, e2022GL099528. https://doi.org/10.1029/2022GL099528

[4] Jones, A.R., Wolff, M., Alshamsi, M. et al. The Emirates Exploration Imager (EXI) Instrument on the Emirates Mars Mission (EMM) Hope Mission. Space Sci Rev 217, 81 (2021). https://doi.org/10.1007/s11214-021-00852-5

How to cite: Gebhardt, C., Guha, B. K., Young, R. M. B., Wolff, M. J., and Edwards, C. S.: The physics and dynamics of selected dust storms in the EMM primary mission, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-3053, https://doi.org/10.5194/egusphere-egu23-3053, 2023.

X4.333
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EGU23-10341
Luca Montabone, Armin Kleinboehl, Michael Smith, Christopher Edwards, François Forget, David Kass, Ehouarn Millour, and Aurélien Stcherbinine

Montabone et al., 2015 and 2020, [1, 2] have developed an iterative, weighted, running mean methodology to grid the available retrievals of atmospheric column dust optical depth (CDOD) from multi-annual and multi-instrument spacecraft observations at Mars. The application of this methodology has produced daily gridded maps of CDOD from Martian Year (MY) 24 through 35, using Mars Global Surveyor/Thermal Emission Spectrometer and Mars Odyssey/Thermal Emission Imaging System nadir observations, as well as the estimates of this quantity from Mars Reconnaissance Orbiter/Mars Climate sounder (MRO/MCS) limb observations. Given the lack of dust observations at certain times and locations, the daily gridded maps have missing values at some grid points. Kriging spatial interpolation has been used to produce regular maps that are useful as multiannual dust scenarios for model simulations, and for the Mars Climate Database (MCD) statistics [3].

We have now adapted this methodology to include CDOD retrievals from Emirates Mars Mission/Emirates Mars Infrared Spectrometer (EMM/EMIRS) nadir observations in MY 36 [4]. The specificity of EMIRS spatial and temporal coverage as well as the extended nature of its footprint are taken into account when carrying out the gridding. We will present a cross-comparison of maps obtained using only EMIRS retrievals and maps obtained using only MCS retrievals, in the attempt to understand what is the best approach to produce a MY 36 dust scenario that makes the best use of both instruments. We will particularly focus on the evolution of large-scale dust storms in MY 36.

References: [1] Montabone, L., et al. (2015) Icarus 251, pp. 65-95, doi: 10.1016/j.icarus.2014.12.034 ; [2] Montabone, L., et al. (2020) J. Geophys. Res. - Planets, doi: 10.1029/2019JE006111 ; [3] http://www-mars.lmd.jussieu.fr (Publicly available dust gridded maps can be currently found up to MY 35 by clicking on the “climatologies of Martian atmospheric dust” link under “Martian dust Climatology”) ; [4] Smith, M.D., et al. (2022) Geophys. Res. Lett. 49, Issue 15, doi: 10.1029/2022GL099636

How to cite: Montabone, L., Kleinboehl, A., Smith, M., Edwards, C., Forget, F., Kass, D., Millour, E., and Stcherbinine, A.: Reconstructing Martian Year 36 column dust optical depth maps using EMM/EMIRS and MRO/MCS, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-10341, https://doi.org/10.5194/egusphere-egu23-10341, 2023.

X4.334
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EGU23-11146
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ECS
George H. Cann, Roland M. B. Young, Christopher S. Edwards, Michael D. Smith, and Michael J. Wolff

Keywords: Mars, Atmosphere, EMM, Emirates Mars Infrared Spectrometer, Off-axis Detectors.

Introduction: The Emirates Mars Mission (EMM) Emirates Mars InfraRed Spectrometer (EMIRS) instrument is a Fourier Transform Infrared (FTIR) spectrometer designed to observe the Martian disk, with the primary scientific objective of determining the three-dimensional thermal state of the lower atmosphere and its diurnal variability on sub-seasonal timescales [1].

EMIRS uses a 3x3 array of deuterated L-alanine doped triglycine sulfate (DLaTGS) pyroelectric detectors [1], however, following the integration of the EMIRS electronics with the optical and mechanical hardware it was observed that the performance of the off-axis (non-central) detectors of the array were lower than expected [1]. Investigations into the performance of these off-axis detectors has so far yielded inconclusive root causes. As EMIRS could meet its primary science objective with the on-axis (central) detector and was subject to a pressing instrument schedule, a project level decision was made to forgo any additional investigation and instead rely on the on-axis detector [1][2].

Method: In this study we present a comparison of observations captured by EMIRS from the off-axis detectors against the on-axis detector. The comparison is performed via a top-down and bottom-up pathway approach using the EMM Science Team processing pipeline. The top-down pathway focuses on the effects of the pre-processing steps on the detector interferograms, whereas the bottom-up approach compares calibrated radiances derived from the pipeline with and without applying the pre-processing steps [3] [4]. Correction of these issues will expand the retrieval derived products by a factor of five.

Results: The top-down comparison shows differences in terms interferogram amplitude and phase error between on and off-axis detectors. We assess the feasibility of correction, then apply correction methods to a subset of EMIRS observations, and propose the root cause of the issues. This study is presented along with the generation of a joint dataset of near-mutual EMIRS and EXI (Emirates eXploration Imager) observations [5].

Acknowledgements: The authors would like to acknowledge support by a Joint Research Agreement between the Mohammed Bin Rashid Space Centre (MBRSC) and the National Space Science and Technology Center (NSSTC), UAE University (UAEU).

References:

[1] Edwards, C. S., et al. (2021). Space Science Reviews (2021) 217:77.

[2] Amiri, H.E. S., et al. (2022). Space Science Reviews (2022) 218:4.

[3] Forman, M. L., et al. (1966). J. Opt. Soc. Am. 56(1), 59–63.

[4] Christensen, V.E., et al. (2018). Space Science Reviews (2018), 215:87.

[5] Jones, A. R., et al. (2021). Space Science Reviews (2021) 217:81.

How to cite: Cann, G. H., Young, R. M. B., Edwards, C. S., Smith, M. D., and Wolff, M. J.: Expanding the Emirates Mars Infrared Spectrometer (EMIRS) Science Dataset using EMIRS off-axis detectors, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-11146, https://doi.org/10.5194/egusphere-egu23-11146, 2023.

X4.335
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EGU23-8656
J. Scott Evans, Michael Chaffin, Justin Deighan, Sonal Jain, John Correira, Emmaris Soto, Hessa Al Matroushi, Hoor Al Mazmi, Scott England, Matthew Fillingim, Greg Holsclaw, Rob Lillis, and Fatma Lootah and the MAVEN Team Members

The Emirates Mars Ultraviolet Spectrometer (EMUS) onboard the Emirates Mars Mission (EMM) observes the Martian dayglow at ultraviolet wavelengths (100-170 nm). EMUS disk observations show unexpected variations in atomic hydrogen, atomic oxygen, and carbon monoxide disk emissions. These variations display local time and hemispheric asymmetry and are observed in approximately 25% of the disk images. England et al. (2022; doi:10.1029/2022GL099611) suggested that the spatial structure, occurrence, and spectral characteristics of these variations are associated with changes in composition and photoelectron flux. Using a similar EMUS data set, Chaffin et al. (2022; doi:10.1029/2022GL099881) reported the first observations of neutral atmosphere auroral emission on the Martian dayside, which is not a new type of aurora but another observable form of proton aurora, and suggested that solar wind deposition is responsible for exciting the auroral emission. We further investigate these two potential drivers of the unexpected variations in EMUS disk observations using data from the Imaging Ultraviolet Spectrograph (IUVS), the Solar Wind Ion Analyzer (SWIA), the SupraThermal And Thermal Ion Composition (STATIC) instrument, and a magnetometer (MAG), all onboard NASA’s Mars Atmosphere and Volatile EvolutioN (MAVEN) mission. We use vertical profiles of densities and temperatures retrieved from limb scan observations by IUVS to identify signatures of dynamics that correlate with unexpected variations in EMUS disk observations. We use measurements from all of the instruments to categorize and characterize EMUS observations in order to determine how changes in composition and solar wind deposition produce unexpected variations in the Martian ultraviolet dayglow.

How to cite: Evans, J. S., Chaffin, M., Deighan, J., Jain, S., Correira, J., Soto, E., Al Matroushi, H., Al Mazmi, H., England, S., Fillingim, M., Holsclaw, G., Lillis, R., and Lootah, F. and the MAVEN Team Members: Dayside auroral emission induced by proton deposition observed by EMM EMUS, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-8656, https://doi.org/10.5194/egusphere-egu23-8656, 2023.

X4.336
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EGU23-13029
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ECS
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Dattaraj Dhuri, Mathilde Simoni, Dimitra Atri, and Ahmed Alhantoobi

Auroras are an important probe for characterizing the interaction of solar wind with the induced magnetosphere of Mars and understanding the evolution of Mars’s atmosphere. Since their first discovery in 2005, Mars auroras have been studied extensively, particularly using the observations from NASA’s Mars Atmosphere and Volatile Evolution (MAVEN). Electron auroras with discrete and diffuse morphology are observed on the nightside of Mars whereas proton auroras are observed mainly on the dayside of Mars. Recently the Emirates Mars UV Spectrometer (EMUS) onboard the Emirates Mars Mission (EMM) has discovered new morphologies of sinuous electron auroras and patchy proton auroras on Mars. In this work, we perform comprehensive statistical analyses of aurora observations to understand the processes responsible for the varied auroral activity on Mars. We systematically isolate electron aurora regions from the nightside EMUS observations and characterize their occurrences and emissions with respect to the crustal magnetic fields, IMF, and electron energies measured by MAVEN. We also develop a purely data-driven model of proton auroras on Mars using MAVEN in-situ observations and UV limb scans between 2014-2022 to train an artificial neural network (ANN). We show that the ANN faithfully reconstructs the observed proton aurora limb scans profiles. We use the trained ANN to analyze the influence of Mars’ crustal magnetic field and IMF on the occurrence rates of the proton auroras using gradient-based attribution maps. 

How to cite: Dhuri, D., Simoni, M., Atri, D., and Alhantoobi, A.: Comprehensive statistical analyses and data-driven modeling of electron and proton auroras on Mars using EMM and MAVEN observations, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-13029, https://doi.org/10.5194/egusphere-egu23-13029, 2023.

X4.338
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EGU23-11360
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ECS
Krishnaprasad Chirakkil, Robert Lillis, Justin Deighan, Michael Chaffin, Sonal Jain, David Brain, Matthew Fillingim, Susarla Raghuram, Scott Evans, Gregory Holsclaw, Hessa Al Matroushi, Scott England, Hoor Al Mazmi, Robin Ramstad, Jasper Halekas, Jared Espley, Shaosui Xu, Xiaohua Fang, Nick Schneider, and Shannon Curry

Discrete aurorae are produced by charged particle precipitation (mostly electrons) into the upper atmosphere. Electron impact causes electronic excitations of atoms and molecules in the atmosphere, whose deexcitation releases ultraviolet photons. Discrete aurora was first discovered as an ultraviolet glow coming from “magnetic umbrellas” in the southern hemisphere. These are strong crustal magnetic field regions on Mars, which are remnants of a global field that decayed billions of years ago. Both Mars Express (Bertaux et al., 2005) and MAVEN (Schneider et al., 2021) have observed cases of discrete aurora events using their limb viewing observations. Emirates Mars Mission (EMM) provides the first synoptic (or disk) images of discrete aurora at Mars (Lillis et al., 2022), thanks to its large orbit and high sensitivity UV spectrograph.

Using observations from Emirates Mars Ultraviolet Spectrometer (EMUS) onboard EMM, the geographic, local time and seasonal distributions of FUV discrete aurora in oxygen auroral emissions (130.4 nm and 135.6 nm) are investigated. Interesting local time asymmetry is observed in the aurora occurrence rates, brightnesses and emission line ratios. More aurora occurrence is observed during pre-midnight (dusk) as compared to post-midnight (dawn). Strong radial crustal field regions (SCFR) have aurora mostly during dusk, and not during dawn. Aurora also tend to occur more in open magnetic field regions away from SCFR. Brighter aurora is observed in the southern hemisphere during dusk, while in the northern hemisphere during dawn. Low brightness ratio [O I 130.4 nm/O I 135.6 nm] is observed in SCFR, but higher ratio in regions away from SCFR in the southern hemisphere. Also, the occurrence rate is found to be enhanced during the perihelion season as compared to the aphelion season. Statistical analysis of the dependence of discrete aurora on observation geometry, upstream solar wind and interplanetary magnetic field conditions will also be presented.

References:

[1] Bertaux, JL., Leblanc, F., Witasse, O. et al. (2005). Discovery of an aurora on Mars. Nature, 435, 790–794, https://doi.org/10.1038/nature03603.

[2] Schneider, N. M., Milby, Z., Jain, S. K., Gérard, J.-C., Soret, L., Brain, D. A., et al. (2021). Discrete aurora on Mars: Insights into their distribution and activity from MAVEN/IUVS observations. Journal of Geophysical Research: Space Physics, 126, https://doi.org/10.1029/2021JA029428.

[3] Lillis, R. J., Deighan, J., Brain, D., Fillingim, M., Jain, S., Chaffin, M., et al. (2022). First synoptic images of FUV discrete aurora and discovery of sinuous aurora at Mars by EMM EMUS. Geophysical Research Letters, 49, https://doi.org/10.1029/2022GL099820.

How to cite: Chirakkil, K., Lillis, R., Deighan, J., Chaffin, M., Jain, S., Brain, D., Fillingim, M., Raghuram, S., Evans, S., Holsclaw, G., Al Matroushi, H., England, S., Al Mazmi, H., Ramstad, R., Halekas, J., Espley, J., Xu, S., Fang, X., Schneider, N., and Curry, S.: Seasonal and Local Time Dependence of Martian FUV Discrete Aurora Observed by EMM EMUS, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-11360, https://doi.org/10.5194/egusphere-egu23-11360, 2023.

X4.339
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EGU23-4712
Justin Deighan, Michael Chaffin, Krishnaprasad Chirakkil, Hessa Al Matroushi, Robert Lillis, Matthew Fillingim, Scott England, Sonal Jain, Greg Holsclaw, Fatma Lootah, Hoor Al Mazmi, Susarla Raghuram, Frank Eparvier, Ed Thiemann, Phil Chamberlin, and Shannon Curry

One of the primary objectives of the Emirates Mars Mission (EMM) is to study the seasonal variation of the upper atmosphere of Mars and associated changes in the escape of atmosphere to space. Here we present a preliminary analysis of the oxygen population in the inner exosphere (1.06-1.6 Martian radii) with nearly-contiguous sampling across all Martian seasons from early MY 36 to early MY 37. This oxygen is thought to be a non-thermal photochemically generated population driven by solar EUV, which can produce energetic atoms with sufficient velocity to escape Mars’ gravity. The observations are made by measuring the atomic oxygen emission at 130.4 nm using the Emirates Mars Ultraviolet Spectrometer (EMUS). We compare the brightness of the exospheric oxygen population with the thermospheric population ( < 1.06 Mars radii, or < 200 km) and find that the exosphere is much more responsive to seasonal variations in solar energy input. The seasonal variations cannot be explained by modulations in solar irradiance at 130.4 nm alone, and are consistent with the expectation that the extended oxygen exosphere at Mars is generated by a photochemical source.

How to cite: Deighan, J., Chaffin, M., Chirakkil, K., Al Matroushi, H., Lillis, R., Fillingim, M., England, S., Jain, S., Holsclaw, G., Lootah, F., Al Mazmi, H., Raghuram, S., Eparvier, F., Thiemann, E., Chamberlin, P., and Curry, S.: Seasonal Variation of the Martian Inner Hot Oxygen Exosphere Observed by EMM/EMUS, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-4712, https://doi.org/10.5194/egusphere-egu23-4712, 2023.

X4.340
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EGU23-13324
Susarla Raghuram, Krishnaprasad Chirakkil, Justin Deighan, Michael Chaffin, Sonal Jain, Robert Lillis, Marko Gacesa, Matthew O. Fillingim, David Brain, Ed Thiemann, Frank Eparvier, Greg Holsclaw, Scott England, Scott Evans, Fatma Hussain Lootah, Hoor Abdelrahman Al Mazmi, Shannon Curry, and Hessa Rashid Al Matroushi

Atomic hydrogen and oxygen are the dominant species in the Martian exosphere. Atomic hydrogen is essentially produced from the dissociation of H2O, whereas, hot oxygen atoms are populated by non-thermal processes such as the dissociative recombination of O2+ with electrons in the Martian ionosphere. The study of these species helps to understand the evolution of the Martian atmosphere and more specifically the history of water on Mars.  The Emirates Mars Ultraviolet Spectrometer (EMUS), one of the primary instruments onboard the Emirates Mars Mission (EMM), has been observing atomic hydrogen and oxygen in the Martian exosphere over the Mars Year 36. We present the analysis of the cross-exospheric observations by the EMUS for hydrogen Lyman series and oxygen 130.4 nm emissions and their seasonal variability. The EMUS cross-exospheric observations cover the tangent altitude starting from 130 km to more than 35,000 km above the disk (see Fig. 1), with most of the observations below 25,000 km. The observations show that when Mars moved from perihelion to aphelion, the hydrogen emission line intensities increase by an order of magnitude or more whereas, for oxygen, it is an increment by a factor of about 2 at larger altitudes. Based on these observations, we also discuss the retrieval of densities, temperature, and the estimation of escape fluxes of hydrogen and oxygen species by applying 3D hydrogen ballistic corona and 3D Monte Carlo particle transport models, respectively.

Figure 1: The EMM-observed cross-exosphere emission intensity profiles of atomic hydrogen and oxygen during Mars Year 36

How to cite: Raghuram, S., Chirakkil, K., Deighan, J., Chaffin, M., Jain, S., Lillis, R., Gacesa, M., Fillingim, M. O., Brain, D., Thiemann, E., Eparvier, F., Holsclaw, G., England, S., Evans, S., Lootah, F. H., Al Mazmi, H. A., Curry, S., and Al Matroushi, H. R.: Seasonal variability of atomic hydrogen and oxygen in the EMM/EMUS cross-exospheric observations during Mars year 36, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-13324, https://doi.org/10.5194/egusphere-egu23-13324, 2023.

X4.341
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EGU23-15440
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Mohammad Marwan, Maryam Yousuf, Badriya Mohammad, and Huda AlHammadi

The Martian atmosphere has undergone significant decay over time, with several factors contributing to this process. It is believed that thermal (Jeans) escape is a significant contributor to hydrogen loss on Mars (Chaufray, 2021). In this research, the role of thermal (Jeans) escape in the uplifting of hydrogen molecules to the exosphere, driven by solar wind forcing, is investigated on seasonal bases. Studying hydrogen escape seasonally can provide insights into the role of solar forcing in atmospheric processes. This research utilizes observations from the Emirates Mars Ultraviolet Spectrometer (EMUS) onboard the Emirates Mars Mission (EMM) To study the atmospheric Hydrogen Lyman Alpha emission on seasonal timescales. The data for this study focuses on the perihelion (greater than Ls 225) and aphelion (between 60-90 Ls)  periods, during which variations in the escape flux due to exobase temperature changes are expected. Level 2b/2a data is specifically chosen because it includes calibrated brightness and added geometric data, a combination of different EMUS observation modes is used in the study. The Lyman Alpha brightness measurements are used to derive the density profile of hydrogen in the Martian atmosphere using the same approach described in (Chaufray, 2008). The atmospheric model is divided into two parts, below the exobase the hydrogen density is described by a diffusive model, while above it uses Chamberlain’s model without satellite particles (Chamberlain, 1963). Deriving atmospheric hydrogen density profile is done by assuming the exobase temperature and solving radiative transfer equations to compute theoretical intensities which are then fitted with observational data to determine exobase temperature and density, a reasonable fit of observations is done assuming the parameters are in ranges that are in line with photochemical models (Krasnopolsky, 2002). This approach has been used to analyze the Mariner 6, 7 exospheric Lyman-α data during the late 1960s (Anderson and Hord, 1971), and the same approach has been used to analyze SPICAM Lyman-α data on Mrs express (Chaufray, 2008), this research attempts to use the same approach to analyze EMUS Lyman-α observations. It is expected that the (Jeans) escape flux of Hydrogen will vary on seasonal timescales, with higher escape fluxes observed around the perihelion period when the exobase temperature is the highest. This is due to the fact that the (Jeans) escape mechanism is driven by the temperature of the exobase, with higher temperatures resulting in higher escape rates. On the other hand, it is expected that lower escape fluxes will be observed during the aphelion period when the exobase temperature is lower.

How to cite: Marwan, M., Yousuf, M., Mohammad, B., and AlHammadi, H.: Investigating Seasonal Variations in Mars' Hydrogen Escape Flux derived by model fitting Lyman Alpha observations from Emirates Mars Ultraviolet Spectrometer (EMUS) onboard the Emirates Mars Mission (EMM)., EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-15440, https://doi.org/10.5194/egusphere-egu23-15440, 2023.

X4.342
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EGU23-13860
Marko Gacesa, Balasubramoniam Murali Krishnan, Saheer Velluvakandi Chaluvalappil, and Mariam Alraie

We present scattering cross sections for O(3P), C(3P), and H colliding with a CO2 molecule at collision energies between 0.1 and 5 eV. The kinetics, transport, and energy relaxation associated with collisions between fast atoms and thermal background atomic and molecular species are of fundamental interest for escape processes in the Martian atmosphere. Two of three primary objectives of the Emirates Mars Mission are related to hydrogen and oxygen escape processes and the collision cross sections are used in the models needed to interpret the observations by the EMUS and EMIRS instruments.

In this work, the collision cross sections have been computed using first principles electronic potential energy surfaces constructed in reduced dimensionality for the lowest-energy asymptotes corresponding to the ground states of the interacting pairs. For the three systems, namely C(3P)-CO2, O(3P)-CO2, and H-CO2, velocity-dependent elastic, rotationally inelastic, and corresponding differential cross sections and derived quantities, including the momentum-transfer cross sections, were constructed. In all cases, the CO2 molecule was modeled using the rigid-rotor approximation, and the collisions were treated as non-reactive. The cross sections were calculated from the first principles (no external parameters) by solving quantum-mechanical coupled channel equations following the approach of Arthurs-Dalgarno, with the coupled-state approximation1,2.

We estimate the impact of the collision cross sections impact on the O, C, and H escape rates at Mars using simple 1D transport models and find significant differences compared to the values in the literature. In the transport model, we used the altitude density profiles taken from NASA’s MAVEN mission. In case of all three energetic atoms, the inelastic cross sections are found to be a significant part of the total cross sections. In case of O escape, we obtain a larger escape flux closer to the estimates based on the MAVEN measurements. We find that that O+CO flux affects the O escape more significantly than expected3, due to its effects on the available energetic O flux. We expect a similar effect to be present not only at Mars but at all CO2-rich planets due to the O-CO-CO2 photochemistry. The impact on C escape is inconclusive, suggesting that the accounted mechanisms of photochemical escape of C are not sufficient to explain the missing carbon at Mars4,5. Please insert your abstract HTML here.

How to cite: Gacesa, M., Krishnan, B. M., Chaluvalappil, S. V., and Alraie, M.: Scattering cross sections for O(3P), C(3P), and H colliding with a CO2 molecule for planetary aeronomy, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-13860, https://doi.org/10.5194/egusphere-egu23-13860, 2023.

Posters virtual: Tue, 25 Apr, 16:15–18:00 | vHall ST/PS

Chairpersons: Maryam Yousuf, Krishnaprasad Chirakkil
Results from the Emirates Mars Mission: Posters (virtual)
vSP.7
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EGU23-3932
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ECS
Anton Fernando, Mike Wolff, and Francois Forget

The formation of water ice clouds can significantly influence the Martian climate, although the Martian atmosphere contains low water vapor concentrations compared to terrestrial levels. The lower Martian atmosphere exhibits three global water ice cloud systems: Aphelion cloud belt (ACB), polar hoods (PHs), and orographic clouds. These clouds are associated with topography, solar heating, global atmospheric circulation, wave activity, and local convection. An appreciable amount of research has been conducted on the first two regimes (ACB and PHs) and very little attention has been given to the third regime (orographic clouds). In general, orographic clouds are observed in northern Spring and summer since they are associated with the major Martian volcanoes. Water ice optical depths provided by the Emirates Exploration Imager (EXI) of the Emirate Mars Mission (EMM) will be used to investigate seasonal and diurnal variations of such clouds in the Tharsis volcanic region: Ascraeus Mons, Pavonis Mons, Arsia Mons, and Olympus Mons. Additionally, context will be provided using the meteorological fields from the Mars PCM (Mars Planetary Climate Model led by Laboratoire de Meteorologie Dynamique Paris, France). This study provides a general picture of how Martian water ice clouds correlate with Mars PCM's meteorological variables: water ice optical depth, atmospheric temperature, meteorological winds, and water vapor mixing ratio. 

How to cite: Fernando, A., Wolff, M., and Forget, F.: Seasonal and Diurnal Variations of Orographic Clouds on Mars with EMM/EXI observations and the Mars Planetary Climate Model, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-3932, https://doi.org/10.5194/egusphere-egu23-3932, 2023.

vSP.8
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EGU23-3162
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Lauriane Soret, Jean-Claude Gérard, Benoît Hubert, and Sonal Jain

The presence of a weak oxygen emission at 130.4-nm resulting from the O 3P-3S transition was first detected in limb observations of the Martian aurora with SPICAM/Mars Express (Soret et al., 2016). It is mostly excited by direct impact of energetic electrons on ground-based O(3P) atoms, but the 130.4-nm radiation is affected by multiple scattering and absorption by CO2. In April 2021, the Emirates Mars Ultraviolet Spectrometer (EMUS) instrument (Holsclaw et al., 2021) on board the HOPE Emirates orbiter started collecting spectral images in the 110-180 nm range with a much increased sensitivity. The OI 135.6-nm emission corresponding to the 3P-5S forbidden transition has also been observed (Jain et al., 2022). In addition, EMUS is taking images of the discrete and sinuous aurora at 130.4 nm. We present Monte Carlo model simulations of the production of the O 3S and 5S excited states for different initial electron energies and discuss possible seasonal variations. We solve the radiative transfer equation for the 130.4-nm triplet and show that the I(130.4 nm/I(135.6 nm) nadir intensity ratio is expected to widely vary with the initial electron energy. These variations result from two effects:

  • The different shapes of the two emission cross sections since the optically thick 3P-3S resonance transition is permitted while 3P-5S is forbidden
  • the radiation entrapment of the 130.4 nm triplet by atmospheric atomic oxygen coupled with absorption by CO2.

We also discuss the sensitivity of the 130.4-nm nadir brightness to the energy distribution of the incoming auroral electrons.

 

References

Jain, S. et al. (2022), poster presented at AGU fall meeting.

Holsclaw, G. et al. (2021), Space Science Reviews217, 1-49.

Lillis, R. J. et al. (2022), Geophysical Research Letters49, e2022GL099820.

Soret, L. et al. (2016), Icarus264, 398-406.

How to cite: Soret, L., Gérard, J.-C., Hubert, B., and Jain, S.: Production and radiative transfert of the OI 130.4 and 135.6 nm emissions in the Mars aurora, EGU General Assembly 2023, Vienna, Austria, 23–28 Apr 2023, EGU23-3162, https://doi.org/10.5194/egusphere-egu23-3162, 2023.