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The solar wind flow along the subsolar line in the magnetic barrier and reconnection at the magnetopause. / Erkaev, N. V.; Mezentsev, A. V.; Biernat, H. K.; Besser, B. P.; Bachmaier, G. A.; Semenov, V. S.; Rijnbeek, R. P.; Farrugia, C. J.

в: Advances in Space Research, Том 14, № 7, 07.1994, стр. 81-86.

Результаты исследований: Научные публикации в периодических изданиях › статья › Рецензирование

Harvard

Erkaev, NV, Mezentsev, AV, Biernat, HK, Besser, BP, Bachmaier, GA, Semenov, VS, Rijnbeek, RP & Farrugia, CJ 1994, 'The solar wind flow along the subsolar line in the magnetic barrier and reconnection at the magnetopause', Advances in Space Research, Том. 14, № 7, стр. 81-86. https://doi.org/10.1016/0273-1177(94)90051-5

APA

Erkaev, N. V., Mezentsev, A. V., Biernat, H. K., Besser, B. P., Bachmaier, G. A., Semenov, V. S., Rijnbeek, R. P., & Farrugia, C. J. (1994). The solar wind flow along the subsolar line in the magnetic barrier and reconnection at the magnetopause. Advances in Space Research, 14(7), 81-86. https://doi.org/10.1016/0273-1177(94)90051-5

Vancouver

Erkaev NV, Mezentsev AV, Biernat HK, Besser BP, Bachmaier GA, Semenov VS и пр. The solar wind flow along the subsolar line in the magnetic barrier and reconnection at the magnetopause. Advances in Space Research. 1994 Июль;14(7):81-86. https://doi.org/10.1016/0273-1177(94)90051-5

Author

Erkaev, N. V. ; Mezentsev, A. V. ; Biernat, H. K. ; Besser, B. P. ; Bachmaier, G. A. ; Semenov, V. S. ; Rijnbeek, R. P. ; Farrugia, C. J. / The solar wind flow along the subsolar line in the magnetic barrier and reconnection at the magnetopause. в: Advances in Space Research. 1994 ; Том 14, № 7. стр. 81-86.

BibTeX

@article{345bea35e0f44c3284025571b92bd06c,
title = "The solar wind flow along the subsolar line in the magnetic barrier and reconnection at the magnetopause",
abstract = "The magnetic barrier is a significant fraction of the magnetosheath region where magnetic forces react back on the plasma flow. We use a magnetohydrodynamic approach to calculate the solar wind flow around the magnetosphere. The use of so-called frozen-in coordinates, where the flow lines and the magnetic field are coordinate axes, is found to be most appropriate. Numerical solutions are presented for the problem of the flow around a blunt body. The results near the magnetopause are used as input parameters for a model of the reconnection of magnetic field lines based on shock-type structures.",
author = "Erkaev, {N. V.} and Mezentsev, {A. V.} and Biernat, {H. K.} and Besser, {B. P.} and Bachmaier, {G. A.} and Semenov, {V. S.} and Rijnbeek, {R. P.} and Farrugia, {C. J.}",
year = "1994",
month = jul,
doi = "10.1016/0273-1177(94)90051-5",
language = "English",
volume = "14",
pages = "81--86",
journal = "Advances in Space Research",
issn = "0273-1177",
publisher = "Elsevier",
number = "7",

}

RIS

TY - JOUR

T1 - The solar wind flow along the subsolar line in the magnetic barrier and reconnection at the magnetopause

AU - Erkaev, N. V.

AU - Mezentsev, A. V.

AU - Biernat, H. K.

AU - Besser, B. P.

AU - Bachmaier, G. A.

AU - Semenov, V. S.

AU - Rijnbeek, R. P.

AU - Farrugia, C. J.

PY - 1994/7

Y1 - 1994/7

N2 - The magnetic barrier is a significant fraction of the magnetosheath region where magnetic forces react back on the plasma flow. We use a magnetohydrodynamic approach to calculate the solar wind flow around the magnetosphere. The use of so-called frozen-in coordinates, where the flow lines and the magnetic field are coordinate axes, is found to be most appropriate. Numerical solutions are presented for the problem of the flow around a blunt body. The results near the magnetopause are used as input parameters for a model of the reconnection of magnetic field lines based on shock-type structures.

AB - The magnetic barrier is a significant fraction of the magnetosheath region where magnetic forces react back on the plasma flow. We use a magnetohydrodynamic approach to calculate the solar wind flow around the magnetosphere. The use of so-called frozen-in coordinates, where the flow lines and the magnetic field are coordinate axes, is found to be most appropriate. Numerical solutions are presented for the problem of the flow around a blunt body. The results near the magnetopause are used as input parameters for a model of the reconnection of magnetic field lines based on shock-type structures.

UR - http://www.scopus.com/inward/record.url?scp=43949161706&partnerID=8YFLogxK

U2 - 10.1016/0273-1177(94)90051-5

DO - 10.1016/0273-1177(94)90051-5

M3 - Article

AN - SCOPUS:43949161706

VL - 14

SP - 81

EP - 86

JO - Advances in Space Research

JF - Advances in Space Research

SN - 0273-1177

IS - 7

ER -

ID: 53092837