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13 results on '"Jakosky, B.M."'

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

Author

Jakosky, B.M., Brain, D., Chaffin, M., Curry, S., Deighan, J., Grebowsky, J., Halekas, J., Leblanc, F., Lillis, R., Luhmann, J.G., Andersson, L., Andre, N., Andrews, D., Baird, D., Baker, D., Bell, J., Benna, M., Bhattacharyya, D., Bougher, S., Bowers, C., Chamberlin, P., Chaufray, J.-Y., Clarke, J., Collinson, G., Combi, M., Connerney, J., Connour, K., Correira, J., Crabb, K., Crary, F., Cravens, T., Crismani, M., Delory, G., Dewey, R., DiBraccio, G., Dong, C., Dong, Y., Dunn, P., Egan, H., Elrod, M., England, S., Eparvier, F., Ergun, R., Eriksson, A., Esman, T., Espley, J., Evans, S., Fallows, K., Fang, X., Fillingim, M., Flynn, C., Fogle, A., Fowler, C., Fox, J., Fujimoto, M., Garnier, P., Girazian, Z., Groeller, H., Gruesbeck, J., Hamil, O., Hanley, K.G., Hara, T., Harada, Y., Hermann, J., Holmberg, M., Holsclaw, G., Houston, S., Inui, S., Jain, S., Jolitz, R., Kotova, A., Kuroda, T., Larson, D., Lee, Y., Lee, C., Lefevre, F., Lentz, C., Lo, D., Lugo, R., Ma, Y.-J., Mahaffy, P., Marquette, M.L., Matsumoto, Y., Mayyasi, M., Mazelle, C., McClintock, W., McFadden, J., Medvedev, A., Mendillo, M., Meziane, K., Milby, Z., Mitchell, D., Modolo, R., Montmessin, F., Nagy, A., Nakagawa, H., Narvaez, C., Olsen, K., Pawlowski, D., Peterson, W., Rahmati, A., Roeten, K., Romanelli, N., Ruhunusiri, S., Russell, C., Sakai, S., Schneider, N., Seki, K., Sharrar, R., Shaver, S., Siskind, D.E., Slipski, M., Soobiah, Y., Steckiewicz, M., Stevens, M.H., Stewart, I., Stiepen, A., Stone, S., Tenishev, V., Terada, N., Terada, K., Thiemann, E., Tolson, R., Toth, G., Trovato, J., Vogt, M., Weber, T., Withers, P., Xu, S., Yelle, R., Yiğit, E., and Zurek, R.

Published
2018
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5. Mars Exploration Rover candidate landing sites as viewed by THEMIS

Author

Christensen, P.R., Ruff, S.W., Fergason, R., Gorelick, N., Jakosky, B.M., Lane, M.D., McEwen, A.S., McSween, H.Y., Mehall, G.L., Milam, K., Moersch, J.E., Pelkey, S.M., Rogers, A.D., and Wyatt, M.B.

Subjects
Infrared imaging -- Observations, Mars probes -- Observations, Astronomy, Earth sciences
Abstract

The analysis of six landing sites that were candidates for the two NASA Mars Exploration Rovers (MER) benefited from recently available image data from the Thermal Emission Imaging Spectrometer (THEMIS) onboard the 2001 Mars Odyssey spacecraft. The combination of daytime and nighttime thermal infrared images from THEMIS supplemented by additional data sets has lead to new or expanded insights into the nature of each landing site. In Meridiani Planum, a layer of lighter-toned, higher thermal inertia material is observable just below the hematite-bearing layer. Gusev Crater displays a more complex stratigraphy than previously observed, including an upper layer with lobate margins. The highest inertia unit of southern Isidis Planitia is confined to topographic lows in the rim/basin margin and does not appear to be due to highland material transported onto the basin floor. The enigmatic, ovoid, blocky terrain on the floor of Melas Chasma displays higher thermal inertia than its surroundings, an indication that it contains coarser or more indurated material than the adjacent aeolian bedforms. The myriad channels of Athabasca Valles display distinctive thermal signatures despite the presence of a bright layer of dust covering the region. The presence of alluvial fans produced from spur-and-gulley erosion of the walls of Eos Chasma demonstrates that mass movements have occurred following the canyon scouring floods. Keywords: Mars, surface, Infrared observations

Published
2005

6. The Clementine mission to the moon: scientific overview

Author

Nozette, Stewart, Rustan, P., Pleasance, L.P., Horan, D.M., Regeon, P., Shoemaker, E.M., Spudis, P.D., Acton, C.H., Baker, D.N., Blamont, J.E., Buratti, B.J., Corson, M.P., Davies, M.E., Duxbury, T.C., Eliason, E.M., Jakosky, B.M., Kordas, J.F., Lewis, I.T., Lichtenberg, C.L., Lucey, P.G., Malaret, E., Massie, M.A., Resnick, J.H., Rollins, C.J., Park, H.S., McEwen, A.S., Priest, R.E., Pieters, C.M., Reisse, P.A., Robinson, M.S., Simpson, R.A., Smith, D.E., Sorenson, T.C., Vorder Breugge, R.W., and Zuber, M.T.

Subjects
Clementine (Space probe) -- Observations, Observations, Research, Natural history, Moon -- Natural history -- Research, Lunar flights -- Research, Space flight to the moon -- Research
Abstract

In early 1992, after a 4-month effort by the National Aeronautics and Space Administration (NASA), the U.S. Department of Defense, and industry, it was concluded that a mission to a [...], In the course of 71 days in lunar orbit, from 19 February to 3 May 1994, the Clementine spacecraft acquired just under two million digital images of the moon at visible and infrared wavelengths. These data are enabling the global mapping of the rock types of the lunar crust and the first detailed investigation of the geology of the lunar polar regions and the lunar far side. In addition, laser-ranging measurements provided the first view of the global topographic figure of the moon. The topography of many ancient impact basins has been measured, and a global map of the thickness of the lunar crust has been derived from the topography and gravity.

Published
1994

7. Fractionation of nitrogen isotopes on Mars: the role of the regolith as a buffer

Author

Zent, A.P., Quinn, R.C., and Jakosky, B.M.

Subjects
Mars (Planet) -- Atmosphere, Nitrogen -- Isotopes, Astronomy, Earth sciences
Abstract

Measurement of the adsorption of molecular nitrogen on palagonite in Mars provides information on nitrogen throughout the history of the planet. The measurement also involves modeling of the adsorbed nitrogen inventory on Martian regoliths. Investigation of the adsorption process reveals that the atmospheric isotopic composition of the planet cannot be buffered by the regolith reservoir of adsorbed nitrogen alone, indicating the presence of other buffering mechanisms.

Published
1994

9. Discovery of Diffuse Aurora on Mars

Author

Stiepen, Arnaud, Schneider, N.M., Jain, S.K., Deighan, Justin, Stewart, A.I.F., Evans, J.S, Stevens, M.H., Larson, D., Mitchell, D., Montmessin, Franck, Chaffin, M.H., McClintock, W.E., Clarke, J.T., Holsclaw, G.M., Jakosky, B.M., Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Computational Physics, Inc., Naval Research Laboratory (NRL), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), 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), Center for Space Physics [Boston] (CSP), Boston University [Boston] (BU), University of California [Berkeley], and University of California-University of California

Subjects
[SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; The Imaging Ultraviolet Spectrograph (IUVS, McClintock et al., 2014) onboard the MAVEN spacecraft has discovered diffuse aurora in Mars’ northern hemisphere spanning a wide range of geographic latitudes and longitudes (Figure 1). This widespread aurora differs from the small auroral patches discovered by the SPICAM instrument onboard the Mars Express spacecraft (Bertaux et al., 2005; Leblanc et al., 2008; Gérard et al., submitted; Soret et al., submitted) restricted to regions of crustal magnetic fields in the southern hemisphere. Furthermore, the northern diffuse aurora appears to peak at altitudes below 100 km, while the crustal field aurora peaked around 120 km.

Published
2015

11. Variability of carbon monoxide in the mars atmosphere

Author

Clancy, R.T., Muhleman, D.O., and Jakosky, B.M.

Abstract

In January of 1982 we measured a microwave spectrum of CO in the Martian atmosphere utilizing the rotational J= 1 → 2 transition of CO. We have analyzed data and reanalyzed the microwave spectra of R. K. Kakar, J. W. Waters, and W. J. Wilson, (Science196, 1090–1091, 1977, measured in 1975) and J. C. Good and F. P. Schloerb, (Icarus47, 166–172, 1981measured in 1980) in order to constrain estimates of the temporal variability of CO abundance in the Martian atmosphere. Our values of CO column density from the data of Karar et al., Good and Schloerb, and our own are 1.7 ± 0.9 × 1020, 3.0 ± 1.0 × 1020, and 4.6 ± 2.0 × 1020cm−2, respectively. The most recent estimate of CO column density from the 1967 infrared spectra of J. Connes, P. Connes, and J.P. Maillard, (Atlas de Spectres Infarouges de Venus, Mars, Jupiter, et Saturne, Editions due Centre National de la Recherche Scientifique, Paris, 1969), is 2.0 ± 0.8 × 1020cm−2(L.D.G. Young and A.T. Young, Icarus30, 75–79, 1977). The large uncertainties given for the microwave measurements are due primarily to uncertainty in the difference between the continuum brightness temperature and atmospheric temperatures of Mars. We have accurately calculated the variation among the observations of the continuum (surface) brightness temperature of Mars, which is primaroly a function of the observed aspect of Mars. A more difficult problem to consider is variability of global atmospheric temperatures among the observations, particularly the effects of global dust storms and the ellipticity of the orbit of Mars. The large bars accompanying our estimates of CO column density from the three sets of microwave measurements are primarily caused by an assumed uncertainty of ±10°K in our atmospheric temperature model due to possible dust in the atmosphere. A qualitative consideration of seasonal variability of global atmospheric temperatures among the measurements suggests that there is not strong evidence for variability of the column abundance of CO on Mars, although variability of 0–100% over a time scale of several years is allowed by the data set. The implication for the variability of Mars O2is, crudely, a factor of two less. We found that the altitude distribution of CO in the atmosphere of Mars was not well constrained by any of the spectra, although our spectrum was marginally better fitted by an altitude increasing profile of CO mixing ratios.

Published
1983
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