Venus exospheric structure: The role of solar radiation pressure
dc.contributor.author | Bishop, James | en_US |
dc.date.accessioned | 2006-04-07T20:43:14Z | |
dc.date.available | 2006-04-07T20:43:14Z | |
dc.date.issued | 1989-09 | en_US |
dc.identifier.citation | Bishop, James (1989/09)."Venus exospheric structure: The role of solar radiation pressure." Planetary and Space Science 37(9): 1063-1077. <http://hdl.handle.net/2027.42/27796> | en_US |
dc.identifier.uri | http://www.sciencedirect.com/science/article/B6V6T-46YK032-1DR/2/d8a01688cfefa32db0608706d98185f1 | en_US |
dc.identifier.uri | https://hdl.handle.net/2027.42/27796 | |
dc.description.abstract | The existence of a "hot" population of hydrogen atoms in the Venus exosphere is well known. In the outer coronal region where it is dominant (r [gsim] 2.0RV), hydrogen atoms are also subject to a relatively strong radiation pressure exerted by resonant scattering of solar Lyman-[alpha] photons. Collisionless models illustrating the consequent structure are discussed, with the nonthermal population mimicked by a dual Maxwellian exobase kinetic distribution. In these models, a considerable fraction of the "hot" atoms outside 2.0RV belongs to the quasi-satellite component, this fraction exceeding 1/2 for 4.0RV [lsim] r [lsim] 10.0RV. Quasi-satellites also raise the kinetic temperature near 2.0Rv by ~ 150 K. Solar ionization of bound atoms occurs mainly outside the ionopause, yielding a partial escape flux [gsim] 2 x 106cm-2s-1 over the day side exobase for assumed solar conditions. The inclusion of a cold exobase prescribed by Pioneer Venus observations has little influence on the outer region (in particular, the quasi-satellite component is unaltered) except that the transition to "hot" kinetic character occurs closer to the exobase on the nightside due to the colder main exobase temperatures there. Lastly, a "tail" of bound atoms is formed as in the terrestrial situation. | en_US |
dc.format.extent | 1380537 bytes | |
dc.format.extent | 3118 bytes | |
dc.format.mimetype | application/pdf | |
dc.format.mimetype | text/plain | |
dc.language.iso | en_US | |
dc.publisher | Elsevier | en_US |
dc.title | Venus exospheric structure: The role of solar radiation pressure | en_US |
dc.type | Article | en_US |
dc.rights.robots | IndexNoFollow | en_US |
dc.subject.hlbsecondlevel | Atmospheric, Oceanic and Space Sciences | en_US |
dc.subject.hlbtoplevel | Science | en_US |
dc.description.peerreviewed | Peer Reviewed | en_US |
dc.contributor.affiliationum | Department of Atmospheric, Oceanic and Space Sciences, University of Michigan, Space Research Building, Ann Arbor, MI 48109-2143, U.S.A. | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/27796/1/0000196.pdf | en_US |
dc.identifier.doi | http://dx.doi.org/10.1016/0032-0633(89)90079-2 | en_US |
dc.identifier.source | Planetary and Space Science | en_US |
dc.owningcollname | Interdisciplinary and Peer-Reviewed |
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