The spatial distribution of planetary ion fluxes near Mars observed by MAVEN

We present the results of an initial effort to statistically map the fluxes of planetary ions on a closed surface around Mars. Choosing a spherical shell ~1000 km above the planet, we map both outgoing and incoming ion fluxes (with energies >25 eV) over a 4 month period. The results show net esca...

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Published in:	Geophysical research letters Vol. 42; no. 21; pp. 9142 - 9148
Main Authors:	Brain, D. A., McFadden, J. P., Halekas, J. S., Connerney, J. E. P., Bougher, S. W., Curry, S., Dong, C. F., Dong, Y., Eparvier, F., Fang, X., Fortier, K., Hara, T., Harada, Y., Jakosky, B. M., Lillis, R. J., Livi, R., Luhmann, J. G., Ma, Y., Modolo, R., Seki, K.
Format:	Journal Article
Language:	English
Published:	Washington Blackwell Publishing Ltd 16.11.2015 John Wiley & Sons, Inc American Geophysical Union
Subjects:	Astrophysics Atmosphere atmospheric escape Convection Earth and Planetary Astrophysics Electric field Electric fields Evolution Fluxes Geographical distribution Geophysics Ion flux Ion fluxes Ions Mars Mars (planet) Mars atmosphere Mars missions Mars surface Northern Hemisphere Planetary evolution Planets Sciences of the Universe Solar and Stellar Astrophysics Solar wind solar wind interaction Spatial distribution Spherical shells Travel Wind power generation solar wind interaction atmospheric escape
ISSN:	0094-8276, 1944-8007
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Abstract	We present the results of an initial effort to statistically map the fluxes of planetary ions on a closed surface around Mars. Choosing a spherical shell ~1000 km above the planet, we map both outgoing and incoming ion fluxes (with energies >25 eV) over a 4 month period. The results show net escape of planetary ions behind Mars and strong fluxes of escaping ions from the northern hemisphere with respect to the solar wind convection electric field. Planetary ions also travel toward the planet, and return fluxes are particularly strong in the southern electric field hemisphere. We obtain a lower bound estimate for planetary ion escape of ~3 × 1024 s−1, accounting for the ~10% of ions that return toward the planet and assuming that the ~70% of the surface covered so far is representative of the regions not yet visited by Mars Atmosphere and Volatile EvolutioN (MAVEN). Key Points MAVEN ion measurements are mapped to a spherical surface around Mars Planetary ion fluxes are organized in four spatial regions on the shell Heavy ion escape rates exceed 2 × 1024 s−1 for energies >25 eV
AbstractList	We present the results of an initial effort to statistically map the fluxes of planetary ions on a closed surface around Mars. Choosing a spherical shell ~1000km above the planet, we map both outgoing and incoming ion fluxes (with energies >25eV) over a 4month period. The results show net escape of planetary ions behind Mars and strong fluxes of escaping ions from the northern hemisphere with respect to the solar wind convection electric field. Planetary ions also travel toward the planet, and return fluxes are particularly strong in the southern electric field hemisphere. We obtain a lower bound estimate for planetary ion escape of ~310 super(24)s super(-1), accounting for the ~10% of ions that return toward the planet and assuming that the ~70% of the surface covered so far is representative of the regions not yet visited by Mars Atmosphere and Volatile EvolutioN (MAVEN). Key Points * MAVEN ion measurements are mapped to a spherical surface around Mars * Planetary ion fluxes are organized in four spatial regions on the shell * Heavy ion escape rates exceed 210 super(24)s super(-1) for energies >25eV We present the results of an initial effort to statistically map the fluxes of planetary ions on a closed surface around Mars. Choosing a spherical shell ~1000 km above the planet, we map both outgoing and incoming ion fluxes (with energies >25 eV) over a 4 month period. The results show net escape of planetary ions behind Mars and strong fluxes of escaping ions from the northern hemisphere with respect to the solar wind convection electric field. Planetary ions also travel toward the planet, and return fluxes are particularly strong in the southern electric field hemisphere. We obtain a lower bound estimate for planetary ion escape of ~3 × 1024 s−1, accounting for the ~10% of ions that return toward the planet and assuming that the ~70% of the surface covered so far is representative of the regions not yet visited by Mars Atmosphere and Volatile EvolutioN (MAVEN). We present the results of an initial effort to statistically map the fluxes of planetary ions on a closed surface around Mars. Choosing a spherical shell ~1000km above the planet, we map both outgoing and incoming ion fluxes (with energies >25eV) over a 4month period. The results show net escape of planetary ions behind Mars and strong fluxes of escaping ions from the northern hemisphere with respect to the solar wind convection electric field. Planetary ions also travel toward the planet, and return fluxes are particularly strong in the southern electric field hemisphere. We obtain a lower bound estimate for planetary ion escape of ~3×1024s-1, accounting for the ~10% of ions that return toward the planet and assuming that the ~70% of the surface covered so far is representative of the regions not yet visited by Mars Atmosphere and Volatile EvolutioN (MAVEN). We present the results of an initial effort to statistically map the fluxes of planetary ions on a closed surface around Mars. Choosing a spherical shell ~1000 km above the planet, we map both outgoing and incoming ion fluxes (with energies >25 eV) over a 4 month period. The results show net escape of planetary ions behind Mars and strong fluxes of escaping ions from the northern hemisphere with respect to the solar wind convection electric field. Planetary ions also travel toward the planet, and return fluxes are particularly strong in the southern electric field hemisphere. We obtain a lower bound estimate for planetary ion escape of ~3 × 1024 s−1, accounting for the ~10% of ions that return toward the planet and assuming that the ~70% of the surface covered so far is representative of the regions not yet visited by Mars Atmosphere and Volatile EvolutioN (MAVEN). Key Points MAVEN ion measurements are mapped to a spherical surface around Mars Planetary ion fluxes are organized in four spatial regions on the shell Heavy ion escape rates exceed 2 × 1024 s−1 for energies >25 eV We present the results of an initial effort to statistically map the fluxes of planetary ions on a closed surface around Mars. Choosing a spherical shell ~1000 km above the planet, we map both outgoing and incoming ion fluxes (with energies >25 eV) over a 4 month period. The results show net escape of planetary ions behind Mars and strong fluxes of escaping ions from the northern hemisphere with respect to the solar wind convection electric field. Planetary ions also travel toward the planet, and return fluxes are particularly strong in the southern electric field hemisphere. We obtain a lower bound estimate for planetary ion escape of ~3 × 10 24 s −1 , accounting for the ~10% of ions that return toward the planet and assuming that the ~70% of the surface covered so far is representative of the regions not yet visited by Mars Atmosphere and Volatile EvolutioN (MAVEN). MAVEN ion measurements are mapped to a spherical surface around Mars Planetary ion fluxes are organized in four spatial regions on the shell Heavy ion escape rates exceed 2 × 10 24 s −1 for energies >25 eV
Author	Connerney, J. E. P. Harada, Y. Fortier, K. Modolo, R. Curry, S. Luhmann, J. G. Jakosky, B. M. Ma, Y. Dong, C. F. Seki, K. McFadden, J. P. Bougher, S. W. Brain, D. A. Eparvier, F. Hara, T. Dong, Y. Lillis, R. J. Halekas, J. S. Fang, X. Livi, R.
Author_xml	– sequence: 1 givenname: D. A. surname: Brain fullname: Brain, D. A. email: david.brain@lasp.colorado.edu organization: Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Colorado, Boulder, USA – sequence: 2 givenname: J. P. surname: McFadden fullname: McFadden, J. P. organization: Space Sciences Laboratory, University of California, Berkeley, California, USA – sequence: 3 givenname: J. S. surname: Halekas fullname: Halekas, J. S. organization: Department of Physics and Astronomy, University of Iowa, Iowa, Iowa City, USA – sequence: 4 givenname: J. E. P. surname: Connerney fullname: Connerney, J. E. P. organization: NASA Goddard Space Flight Center, Maryland, Greenbelt, USA – sequence: 5 givenname: S. W. surname: Bougher fullname: Bougher, S. W. organization: Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, Michigan, Ann Arbor, USA – sequence: 6 givenname: S. surname: Curry fullname: Curry, S. organization: Space Sciences Laboratory, University of California, Berkeley, California, USA – sequence: 7 givenname: C. F. surname: Dong fullname: Dong, C. F. organization: Department of Atmospheric, Oceanic, and Space Sciences, University of Michigan, Michigan, Ann Arbor, USA – sequence: 8 givenname: Y. surname: Dong fullname: Dong, Y. organization: Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Colorado, Boulder, USA – sequence: 9 givenname: F. surname: Eparvier fullname: Eparvier, F. organization: Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Colorado, Boulder, USA – sequence: 10 givenname: X. surname: Fang fullname: Fang, X. organization: Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Colorado, Boulder, USA – sequence: 11 givenname: K. surname: Fortier fullname: Fortier, K. organization: Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Colorado, Boulder, USA – sequence: 12 givenname: T. surname: Hara fullname: Hara, T. organization: Space Sciences Laboratory, University of California, Berkeley, California, USA – sequence: 13 givenname: Y. surname: Harada fullname: Harada, Y. organization: Space Sciences Laboratory, University of California, Berkeley, California, USA – sequence: 14 givenname: B. M. surname: Jakosky fullname: Jakosky, B. M. organization: Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Colorado, Boulder, USA – sequence: 15 givenname: R. J. surname: Lillis fullname: Lillis, R. J. organization: Space Sciences Laboratory, University of California, Berkeley, California, USA – sequence: 16 givenname: R. surname: Livi fullname: Livi, R. organization: Space Sciences Laboratory, University of California, Berkeley, California, USA – sequence: 17 givenname: J. G. surname: Luhmann fullname: Luhmann, J. G. organization: Space Sciences Laboratory, University of California, Berkeley, California, USA – sequence: 18 givenname: Y. surname: Ma fullname: Ma, Y. organization: Institute of Geophysics and Planetary Physics, University of California, California, Los Angeles, USA – sequence: 19 givenname: R. surname: Modolo fullname: Modolo, R. organization: UVSQ/LATMOS-IPSL/CNRS-INSU, Guyancourt, France – sequence: 20 givenname: K. surname: Seki fullname: Seki, K. organization: Solar-Terrestrial Environment Laboratory, Nagoya University, Nagoya, Japan
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Snippet	We present the results of an initial effort to statistically map the fluxes of planetary ions on a closed surface around Mars. Choosing a spherical shell ~1000... We present the results of an initial effort to statistically map the fluxes of planetary ions on a closed surface around Mars. Choosing a spherical shell...
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SubjectTerms	Astrophysics Atmosphere atmospheric escape Convection Earth and Planetary Astrophysics Electric field Electric fields Evolution Fluxes Geographical distribution Geophysics Ion flux Ion fluxes Ions Mars Mars (planet) Mars atmosphere Mars missions Mars surface Northern Hemisphere Planetary evolution Planets Sciences of the Universe Solar and Stellar Astrophysics Solar wind solar wind interaction Spatial distribution Spherical shells Travel Wind power generation
Title	The spatial distribution of planetary ion fluxes near Mars observed by MAVEN
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