Standard

Implications of the Stagnation Line Model for energy input through the dayside magnetopause. / Pudovkin, Mikhail I.; Semenov, Vladimir S.; Heyn, Martin F.; Biernat, Helfried K.

In: Geophysical Research Letters, Vol. 13, No. 3, 03.1986, p. 213-216.

Research output: Contribution to journal › Article › peer-review

Harvard

Pudovkin, MI, Semenov, VS, Heyn, MF & Biernat, HK 1986, 'Implications of the Stagnation Line Model for energy input through the dayside magnetopause', Geophysical Research Letters, vol. 13, no. 3, pp. 213-216. https://doi.org/10.1029/GL013i003p00213

APA

Pudovkin, M. I., Semenov, V. S., Heyn, M. F., & Biernat, H. K. (1986). Implications of the Stagnation Line Model for energy input through the dayside magnetopause. Geophysical Research Letters, 13(3), 213-216. https://doi.org/10.1029/GL013i003p00213

Vancouver

Pudovkin MI, Semenov VS, Heyn MF, Biernat HK. Implications of the Stagnation Line Model for energy input through the dayside magnetopause. Geophysical Research Letters. 1986 Mar;13(3):213-216. https://doi.org/10.1029/GL013i003p00213

Author

Pudovkin, Mikhail I. ; Semenov, Vladimir S. ; Heyn, Martin F. ; Biernat, Helfried K. / Implications of the Stagnation Line Model for energy input through the dayside magnetopause. In: Geophysical Research Letters. 1986 ; Vol. 13, No. 3. pp. 213-216.

BibTeX

@article{e6578d3d7a1b4800b8087356f89318c7,
title = "Implications of the Stagnation Line Model for energy input through the dayside magnetopause",
abstract = "Based on the formation of a stagnation line at the magnetopause the electromagnetic energy transport from the solar wind into the dayside magnetosphere is analyzed. The resulting energy flux is proportional to v∞B∞² sin² (θ∞ ‐ ϕ∞), where v∞ and B∞ are the solar wind speed and magnetic field and θ∞ ‐ ϕ∞ is the angle between the IMF and the stagnation line projected into the interplanetary space. A stagnation line parallel to the separator gives approximately the sin4(θ∞/2) energy flux dependence of Akasofu's ε‐index.",
author = "Pudovkin, {Mikhail I.} and Semenov, {Vladimir S.} and Heyn, {Martin F.} and Biernat, {Helfried K.}",
year = "1986",
month = mar,
doi = "10.1029/GL013i003p00213",
language = "English",
volume = "13",
pages = "213--216",
journal = "Geophysical Research Letters",
issn = "0094-8276",
publisher = "American Geophysical Union",
number = "3",

}

RIS

TY - JOUR

T1 - Implications of the Stagnation Line Model for energy input through the dayside magnetopause

AU - Pudovkin, Mikhail I.

AU - Semenov, Vladimir S.

AU - Heyn, Martin F.

AU - Biernat, Helfried K.

PY - 1986/3

Y1 - 1986/3

N2 - Based on the formation of a stagnation line at the magnetopause the electromagnetic energy transport from the solar wind into the dayside magnetosphere is analyzed. The resulting energy flux is proportional to v∞B∞² sin² (θ∞ ‐ ϕ∞), where v∞ and B∞ are the solar wind speed and magnetic field and θ∞ ‐ ϕ∞ is the angle between the IMF and the stagnation line projected into the interplanetary space. A stagnation line parallel to the separator gives approximately the sin4(θ∞/2) energy flux dependence of Akasofu's ε‐index.

AB - Based on the formation of a stagnation line at the magnetopause the electromagnetic energy transport from the solar wind into the dayside magnetosphere is analyzed. The resulting energy flux is proportional to v∞B∞² sin² (θ∞ ‐ ϕ∞), where v∞ and B∞ are the solar wind speed and magnetic field and θ∞ ‐ ϕ∞ is the angle between the IMF and the stagnation line projected into the interplanetary space. A stagnation line parallel to the separator gives approximately the sin4(θ∞/2) energy flux dependence of Akasofu's ε‐index.

UR - http://www.scopus.com/inward/record.url?scp=0022672749&partnerID=8YFLogxK

U2 - 10.1029/GL013i003p00213

DO - 10.1029/GL013i003p00213

M3 - Article

AN - SCOPUS:0022672749

VL - 13

SP - 213

EP - 216

JO - Geophysical Research Letters

JF - Geophysical Research Letters

SN - 0094-8276

IS - 3

ER -

ID: 53096821