Search

Your search keyword '"Connour, Kyle"' showing total 8 results
Start Over Author "Connour, Kyle"
8 results on '"Connour, Kyle"'

3. Bridge to the stars: A mission concept to an interstellar object

Author

Moore, Kimberly, Courville, Samuel, Ferguson, Sierra, Schoenfeld, Ashley, Llera, Kristie, Agrawal, Rachana, Brack, Daniel, Buhler, Peter, Connour, Kyle, Czaplinski, Ellen, DeLuca, Michael, Deutsch, Ariel, Hammond, Noah, Kuettel, Donald, Marusiak, Angela, Nerozzi, Stefano, Stuart, Jeffrey, Tarnas, Jesse, Thelen, Alexander, Castillo-Rogez, Julie, Smythe, William, Landau, Damon, Mitchell, Karl, and Budney, Charles

Published
2021
Full Text
View/download PDF

4. Water-ice and Dust Retrieved from MAVEN/IUVS Data

Author

Connour, Kyle, Wolff, Michael, Mccord Schneider, Nicholas, Deighan, Justin, Lefèvre, Franck, Jain, Sonal, Kahre, Melinda, Wilson, R. John, Millour, Ehouarn, and Cardon, Catherine

Subjects
[SDU] Sciences of the Universe [physics]
Abstract

The Imaging Ultraviolet Spectrograph (IUVS) instrument on the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft takes mid-UV spectral images of the Martian surface and atmosphere. We can retrieve information about aerosols using this nadir imaging. Measuring local time variability of large-scale recurring features is made possible with MAVEN’s nearly-global imaging combined with its ~4.5-hour elliptical orbit, something not possible with sun-synchronous orbits.In this study we performed retrievals of water ice and dust from MAVEN/IUVS data to investigate their local time variability. To do this we employed the DIScrete Ordinates Radiative Transfer (DISORT) code as the core radiative transfer algorithm. We used dust radiative properties derived from the Mars year 34 global dust storm (see Connour et al, 2022) and water-ice radiative properties derived from droxtal-shaped particles. We selected the shortest wavelengths (205--220 nm) and the longest wavelengths (290--305 nm) for these retrievals as they provide the best opportunity to isolate the effect of dust and water ice while avoiding ozone in the spectrum. These retrievals allowed us to build a dust and water-ice climatology, and to understand these aerosols' diurnal evolution, spatial extent, and optical thickness. We also compared these retrievals to global circulation model (GCMs) simulations. These aerosols are important to the radiative balance in the models, yet there have been few datasets that can provide constraints to aerosols produced by the simulations---particularly at local times away from 3pm. We discuss the parameter adjustments needed to more accurately produce the aerosols seen in this dataset and the implications of these changes.

Published
2022

5. Dynamics of the extremely elongated cloud on Mars Arsia Mons volcano

Author

Hernandez Bernal, Jorge, primary, Sánchez-Lavega, Agustín, additional, del Río-Gaztelurrutia, Teresa, additional, Hueso, Ricardo, additional, Ordóñez-Etxeberria, Iñaki, additional, Cardesín-Moinelo, Alejandro, additional, Ravanis, Eleni, additional, Wood, Simon, additional, Titov, Dmitrij, additional, Connour, Kyle, additional, Schneider, Nick, additional, Tirsch, Daniela, additional, Jaumann, Ralf, additional, Hauber, Ernst, additional, and Gondet, Brigitte, additional

Published
2020
Full Text
View/download PDF

7. Loss of the Martian atmosphere to space: Present-day loss rates determined from MAVEN observations and integrated loss through time

Author

Jakosky , Bruce, Brain , David, Chaffin , Michael, Curry , Shannon M., Deighan , Justin, Grebowsky , Joseph, Halekas , Jasper, Leblanc , François, Lillis , Robert, Luhmann , Janet, Andersson , Laila, André , Nicolas, Andrews , David, Baird , Darren, Baker , Daniel, Bell , Jared, Benna , Mehdi, Bhattacharyya , Dolon, Bougher , Stephen, Bowers , Charlie, Chamberlin , Phillip, Chaufray , Jean-Yves, Clarke , John, Collinson , Glyn, Combi , Michael, Connerney , Jack, Connour , Kyle, Correira , J., Crabb , Kyle, Crary , Frank, Cravens , Thomas, Crismani , Matteo, Delory , Greg, Dewey , Ryan, DiBraccio , Gina, Dong , Chuanfei, Dong , Yaxue, Dunn , Patrick, Egan , Hilary, Elrod , Meredith K., England , Scott, Eparvier , Frank, Ergun , Robert, Eriksson , Anders, Esman , Teresa, Espley , Jared, Evans , S., Fallows , Kathryn, Fang , Xiaohua, Fillingim , Matthew, Flynn , C., Fogle , A., Fowler , Christopher M., Fox , Jane L., Fujimoto , Masaki, Garnier , Philippe, Girazian , Zachary, Groeller , Hannes, Gruesbeck , Jacob, Hamil , O., Hanley , K., Hara , Takuya, Harada , Yuki, Hermann , Jacob, Holmberg , Mika, Holsclaw , Greg, Houston , S., Inui , S., Jain , Sonal, Jolitz , Rebecca, Kotova , Anna, Kuroda , Takeshi, Larson , Davin, Lee , Yuni, Lee , C., Lefèvre , Franck, Lentz , Christy, Lo , D., Lugo , Rafael, Ma , Yingjuan, Mahaffy , Paul R., Marquette , Melissa, Matsumoto , Y., Mayyasi , Majd, Mazelle , Christian, Mcclintock , William, McFadden , Jim, Medvedev , A., Mendillo , Michael, Meziane , K., Milby , Zachariah, Mitchell , D., Modolo , Ronan, Montmessin , Franck, Nagy , Andrew, Nakagawa , H., Narvaez , Clara, Olsen , Kirk, Pawlowski , D., Peterson , William, Rahmati , Ali, Roeten , Kali, Romanelli , Norberto, Ruhunusiri , Suranga, Russell , Christopher T., Sakai , Shotaro, Schneider , Nicholas, Seki , K., Sharrar , R., Shaver , S., Siskind , David E., Slipski , Marek, Soobiah , Yasir, Steckiewicz , Morgane, Stevens , Michael, Stewart , Ian, Laboratory for Atmospheric and Space Physics [Boulder] ( LASP ), University of Colorado Boulder [Boulder], Space Sciences Laboratory [Berkeley] ( SSL ), University of California [Berkeley], NASA Goddard Space Flight Center ( GSFC ), Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa], HEPPI - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de recherche en astrophysique et planétologie ( IRAP ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Swedish Institute of Space Physics [Uppsala] ( IRF ), NASA Johnson Space Center ( JSC ), NASA, National Institute of Aerospace [Hampton] ( NIA ), Center for Space Physics [Boston] ( CSP ), Boston University [Boston] ( BU ), Department of Climate and Space Sciences and Engineering ( CLaSP ), University of Michigan [Ann Arbor], Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), Communications and Power Industries ( CPI ), Department of Physics and Astronomy [Lawrence], University of Kansas [Lawrence] ( KU ), Princeton University, University of Arizona, Wright State University [Dayton], Institute of Space and Astronautical Science ( ISAS ), University of Kansas, Department of Physics and Astronomy [Ames, Iowa], Iowa State University ( ISU ), The University of Tokyo, National Institute of Information and Communications Technology ( NICT ), IMPEC - LATMOS, Analytical Mechanics Associates, Inc., University of California at Los Angeles [Los Angeles] ( UCLA ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), Tohoku University [Sendai], Eastern Michigan University, Institute of Geophysics and Planetary Physics [Los Angeles] ( IGPP ), Department of Earth and Planetary Science [Tokyo], and Naval Research Laboratory ( NRL )

Subjects
Mars atmosphere, [ PHYS.PHYS.PHYS-AO-PH ] Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], Atmosphere, Magnetospheres, Solar wind, Mars, Mars climate
Abstract

International audience; Observations of the Mars upper atmosphere made from the Mars Atmosphere and Volatile Evolution (MAVEN) spacecraft have been used to determine the loss rates of gas from the upper atmosphere to space for a complete Mars year (16 Nov 2014 – 3 Oct 2016). Loss rates for H and O are sufficient to remove ∼2-3 kg/s to space. By itself, this loss would be significant over the history of the planet. In addition, loss rates would have been greater early in history due to the enhanced solar EUV and more-active Sun. Integrated loss, based on current processes whose escape rates in the past are adjusted according to expected solar evolution, would have been as much as 0.8 bar CO2 or 23 m global equivalent layer of H2O; these losses are likely to be lower limits due to the nature of the extrapolation of loss rates to the earliest times. Combined with the lack of surface or subsurface reservoirs for CO2 that could hold remnants of an early, thick atmosphere, these results suggest that loss of gas to space has been the dominant process responsible for changing the climate of Mars from an early, warmer environment to the cold, dry one that we see today.

Published
2018

8. Mars topographic clouds: MAVEN/IUVS observations and LMD MGCM predictions

Author

Schneider, Nicholas M., Connour, Kyle, Forget, François, Deighan, Justin, Jain, Sonal, Vals, Margaux, Wolff, Michael J., Chaffin, Michael S., Crismani, Matteo, Stewart, A. Ian F., Mcclintock, William E., Holsclaw, Greg, Lefèvre, Franck, Montmessin, Franck, Stiepen, Arnaud, Stevens, Michael H., Evans, J. Scott, Yelle, Roger, Lo, Daniel, Clarke, John T., Jakosky, Bruce, Cardon, Catherine, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Space Science Institute [Boulder] (SSI), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Naval Research Laboratory (NRL), Computational Physics, Inc., Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)

Subjects
[SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics]
Abstract

International audience; The Imaging Ultraviolet Spectrograph (IUVS) instrument on the Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft takes mid-UV spectral images of the Martian atmosphere. From these apoapse disk images, information about clouds and aerosols can be retrieved and comprise the only MAVEN observations of topographic clouds and cloud morphologies. Measuring local time variability of large-scale recurring cloud features is made possible with MAVEN’s ~4.5-hour elliptical orbit, something not possible with sun-synchronous orbits. We have run the LMD MGCM (Mars global circulation model) at 1° x 1° resolution to simulate water ice cloud formation with inputs consistent with observing parameters and Mars seasons. Topographic clouds are observed to form daily during the late mornings of northern hemisphere spring and this phenomenon recurs until late summer (Ls = 160°), after which topographic clouds wane in thickness. By northern fall, most topographic clouds cease to form except over Arsia Mons and Pavonis Mons, where clouds can still be observed. Our data show moderate cloud formation over these regions as late as Ls = 220°, something difficult for the model to replicate. Previous studies have shown that models have trouble simulating equatorial cloud thickness in combination with a realistic amount of water vapor and not-too-thick polar water ice clouds, implying aspects of the water cycle are not fully understood. We present data/model comparisons as well as further refinements on parameter inputs based on IUVS observations.

Published
2017

Catalog

Books, media, physical & digital resources
See catalog results