Quantitative magnetotail characteristics of different magnetospheric states

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Quantitative magnetotail characteristics of different magnetospheric states. / Shukhtina, M. A.; Dmitrieva, N. P.; Sergeev, V. A.

In: Annales Geophysicae, Vol. 22, No. 3, 2004, p. 1019-1032.

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

BibTeX

@article{9626b728b3074ce3a07e89f867affcc8,

title = "Quantitative magnetotail characteristics of different magnetospheric states",

abstract = "Quantitative relationships allowing one to compute the lobe magnetic field, flaring angle and tail radius, and to evaluate magnetic flux based on solar wind/IMF parameters and spacecraft position are obtained for the middle magnetotail, X=(-15, -35) R-E, using 3.5 years of simultaneous Geotail and Wind spacecraft observations. For the first time it was done separately for different states of magnetotail including the substorm onset (SO) epoch, the steady magnetospheric convection (SMC) and quiet periods (Q). In the explored distance range the magnetotail parameters appeared to be similar (within the error bar) for Q and SMC states, whereas at SO their values are considerably larger. In particular, the tail radius is larger by 1-3 R-E at substorm onset than during Q and SMC states, for which the radius value is close to previous magnetopause model values. The calculated lobe magnetic flux value at substorm onset is similar to1 GWb, exceeding that at Q (SMC) states by similar to50%. The model magnetic flux values at substorm onset and SMC show little dependence on the solar wind dynamic pressure and distance in the tail, so the magnetic flux value can serve as an important discriminator of the state of the middle magnetotail.",

keywords = "magnetospheric physics, solar wind-magnetosphere-interactions, magnetotail, storms and substorms, SOLAR-WIND CONTROL, LOBE MAGNETIC-FIELD, PLASMA SHEET, GEOMAGNETIC TAIL, MAGNETOPAUSE SHAPE, GROWTH-PHASE, SUBSTORMS, PRESSURE, SPACECRAFT, LOCATION",

author = "Shukhtina, {M. A.} and Dmitrieva, {N. P.} and Sergeev, {V. A.}",

year = "2004",

doi = "10.5194/angeo-22-1019-2004",

language = "Английский",

volume = "22",

pages = "1019--1032",

journal = "Annales Geophysicae",

issn = "0992-7689",

publisher = "Copernicus GmbH ",

number = "3",

}

RIS

TY - JOUR

T1 - Quantitative magnetotail characteristics of different magnetospheric states

AU - Shukhtina, M. A.

AU - Dmitrieva, N. P.

AU - Sergeev, V. A.

PY - 2004

Y1 - 2004

N2 - Quantitative relationships allowing one to compute the lobe magnetic field, flaring angle and tail radius, and to evaluate magnetic flux based on solar wind/IMF parameters and spacecraft position are obtained for the middle magnetotail, X=(-15, -35) R-E, using 3.5 years of simultaneous Geotail and Wind spacecraft observations. For the first time it was done separately for different states of magnetotail including the substorm onset (SO) epoch, the steady magnetospheric convection (SMC) and quiet periods (Q). In the explored distance range the magnetotail parameters appeared to be similar (within the error bar) for Q and SMC states, whereas at SO their values are considerably larger. In particular, the tail radius is larger by 1-3 R-E at substorm onset than during Q and SMC states, for which the radius value is close to previous magnetopause model values. The calculated lobe magnetic flux value at substorm onset is similar to1 GWb, exceeding that at Q (SMC) states by similar to50%. The model magnetic flux values at substorm onset and SMC show little dependence on the solar wind dynamic pressure and distance in the tail, so the magnetic flux value can serve as an important discriminator of the state of the middle magnetotail.

AB - Quantitative relationships allowing one to compute the lobe magnetic field, flaring angle and tail radius, and to evaluate magnetic flux based on solar wind/IMF parameters and spacecraft position are obtained for the middle magnetotail, X=(-15, -35) R-E, using 3.5 years of simultaneous Geotail and Wind spacecraft observations. For the first time it was done separately for different states of magnetotail including the substorm onset (SO) epoch, the steady magnetospheric convection (SMC) and quiet periods (Q). In the explored distance range the magnetotail parameters appeared to be similar (within the error bar) for Q and SMC states, whereas at SO their values are considerably larger. In particular, the tail radius is larger by 1-3 R-E at substorm onset than during Q and SMC states, for which the radius value is close to previous magnetopause model values. The calculated lobe magnetic flux value at substorm onset is similar to1 GWb, exceeding that at Q (SMC) states by similar to50%. The model magnetic flux values at substorm onset and SMC show little dependence on the solar wind dynamic pressure and distance in the tail, so the magnetic flux value can serve as an important discriminator of the state of the middle magnetotail.

KW - magnetospheric physics

KW - solar wind-magnetosphere-interactions

KW - magnetotail

KW - storms and substorms

KW - SOLAR-WIND CONTROL

KW - LOBE MAGNETIC-FIELD

KW - PLASMA SHEET

KW - GEOMAGNETIC TAIL

KW - MAGNETOPAUSE SHAPE

KW - GROWTH-PHASE

KW - SUBSTORMS

KW - PRESSURE

KW - SPACECRAFT

KW - LOCATION

UR - http://www.scopus.com/inward/record.url?scp=1942536098&partnerID=8YFLogxK

U2 - 10.5194/angeo-22-1019-2004

DO - 10.5194/angeo-22-1019-2004

M3 - статья

AN - SCOPUS:1942536098

VL - 22

SP - 1019

EP - 1032

JO - Annales Geophysicae

JF - Annales Geophysicae

SN - 0992-7689

IS - 3

ER -

ID: 36725342