3D-modeling of Mercury's solar wind sputtered surface-exosphere environment
The efficiency of sputtered refractory elements by H+ and He++ solar wind ions from Mercury's surface and their contribution to the exosphere are studied for various solar wind conditions. A 3D solar wind–planetary interaction hybrid model is used for the evaluation of precipitation maps of the...
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| Published in: | Planetary and space science Vol. 115; pp. 90 - 101 |
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01-09-2015
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| Abstract | The efficiency of sputtered refractory elements by H+ and He++ solar wind ions from Mercury's surface and their contribution to the exosphere are studied for various solar wind conditions. A 3D solar wind–planetary interaction hybrid model is used for the evaluation of precipitation maps of the sputter agents on Mercury's surface. By assuming a global mineralogical surface composition, the related sputter yields are calculated by means of the 2013 SRIM code and are coupled with a 3D exosphere model. Because of Mercury's magnetic field, for quiet and nominal solar wind conditions the plasma can only precipitate around the polar areas, while for extreme solar events (fast solar wind, coronal mass ejections, interplanetary magnetic clouds) the solar wind plasma has access to the entire dayside. In that case the release of particles form the planet's surface can result in an exosphere density increase of more than one order of magnitude. The corresponding escape rates are also about an order of magnitude higher. Moreover, the amount of He++ ions in the precipitating solar plasma flow enhances also the release of sputtered elements from the surface in the exosphere. A comparison of our model results with MESSENGER observations of sputtered Mg and Ca elements in the exosphere shows a reasonable quantitative agreement.
•We modeled Mercury's sputtered exosphere in a self-consistent way.•Average surface composition model is consistent with MESSENGER observations.•Mg and Ca tail observations are in reasonable agreement with simulation results.•Some exospheric species may become detectable only during special SW-conditions. |
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| AbstractList | The efficiency of sputtered refractory elements by H+ and He++ solar wind ions from Mercury's surface and their contribution to the exosphere are studied for various solar wind conditions. A 3D solar wind–planetary interaction hybrid model is used for the evaluation of precipitation maps of the sputter agents on Mercury's surface. By assuming a global mineralogical surface composition, the related sputter yields are calculated by means of the 2013 SRIM code and are coupled with a 3D exosphere model. Because of Mercury's magnetic field, for quiet and nominal solar wind conditions the plasma can only precipitate around the polar areas, while for extreme solar events (fast solar wind, coronal mass ejections, interplanetary magnetic clouds) the solar wind plasma has access to the entire dayside. In that case the release of particles form the planet's surface can result in an exosphere density increase of more than one order of magnitude. The corresponding escape rates are also about an order of magnitude higher. Moreover, the amount of He++ ions in the precipitating solar plasma flow enhances also the release of sputtered elements from the surface in the exosphere. A comparison of our model results with MESSENGER observations of sputtered Mg and Ca elements in the exosphere shows a reasonable quantitative agreement.
•We modeled Mercury's sputtered exosphere in a self-consistent way.•Average surface composition model is consistent with MESSENGER observations.•Mg and Ca tail observations are in reasonable agreement with simulation results.•Some exospheric species may become detectable only during special SW-conditions. The efficiency of sputtered refractory elements by and He++ solar wind ions from Mercury's surface and their contribution to the exosphere are studied for various solar wind conditions. A 3D solar wind-planetary interaction hybrid model is used for the evaluation of precipitation maps of the sputter agents on Mercury's surface. By assuming a global mineralogical surface composition, the related sputter yields are calculated by means of the 2013 SRIM code and are coupled with a 3D exosphere model. Because of Mercury's magnetic field, for quiet and nominal solar wind conditions the plasma can only precipitate around the polar areas, while for extreme solar events (fast solar wind, coronal mass ejections, interplanetary magnetic clouds) the solar wind plasma has access to the entire dayside. In that case the release of particles form the planet's surface can result in an exosphere density increase of more than one order of magnitude. The corresponding escape rates are also about an order of magnitude higher. Moreover, the amount of He++ ions in the precipitating solar plasma flow enhances also the release of sputtered elements from the surface in the exosphere. A comparison of our model results with MESSENGER observations of sputtered Mg and Ca elements in the exosphere shows a reasonable quantitative agreement. |
| Author | McKenna-Lawlor, S. Alho, M. Lichtenegger, H.I.M. Martín-Fernández, J.A. Kallio, E. Wurz, P. Lammer, H. Pfleger, M. Mura, A. |
| Author_xml | – sequence: 1 givenname: M. surname: Pfleger fullname: Pfleger, M. organization: Space Research Institute, Austrian Academy of Sciences, Schmiedlstraße 6, A-8042 Graz, Austria – sequence: 2 givenname: H.I.M. surname: Lichtenegger fullname: Lichtenegger, H.I.M. email: herbert.lichtenegger@oeaw.ac.at organization: Space Research Institute, Austrian Academy of Sciences, Schmiedlstraße 6, A-8042 Graz, Austria – sequence: 3 givenname: P. surname: Wurz fullname: Wurz, P. organization: Physikalisches Institut, University of Bern, Sidlerstraße 5, CH-3012 Bern, Switzerland – sequence: 4 givenname: H. surname: Lammer fullname: Lammer, H. organization: Space Research Institute, Austrian Academy of Sciences, Schmiedlstraße 6, A-8042 Graz, Austria – sequence: 5 givenname: E. surname: Kallio fullname: Kallio, E. organization: Aalto University, School of Electrical Engineering, Helsinki, Finland – sequence: 6 givenname: M. surname: Alho fullname: Alho, M. organization: Aalto University, School of Electrical Engineering, Helsinki, Finland – sequence: 7 givenname: A. surname: Mura fullname: Mura, A. organization: Istituto Nazionale Di Astrofisica, Viale del Parco Mellini n°84, 00136 Roma, Italy – sequence: 8 givenname: S. surname: McKenna-Lawlor fullname: McKenna-Lawlor, S. organization: National University of Ireland, Maynooth, Ireland – sequence: 9 givenname: J.A. surname: Martín-Fernández fullname: Martín-Fernández, J.A. organization: Department for Computer Science and Applied Mathematics, University of Girona, Edifici P-IV, Campus Montilivi, E-17071 Girona, Spain |
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| Snippet | The efficiency of sputtered refractory elements by H+ and He++ solar wind ions from Mercury's surface and their contribution to the exosphere are studied for... The efficiency of sputtered refractory elements by and He++ solar wind ions from Mercury's surface and their contribution to the exosphere are studied for... |
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| SubjectTerms | BepiColombo Coronal mass ejection Density Exosphere Mercury Mercury surface Messenger Particle release Planetary magnetic fields Precipitates Precipitation Solar wind Surface sputtering |
| Title | 3D-modeling of Mercury's solar wind sputtered surface-exosphere environment |
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