IMF Bx and By dependencies of the polar cap auroral distribution for northward IMF orientation inferred from observations at Vostok station

Трошичев, О. А.; Gusev, M.G.

doi:10.1016/0021-9169(94)90033-7

Cited by 8 publications

(4 citation statements)

References 20 publications

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“…For example, a possible solution for D = B x at auroral zone latitudes in the LT range of [23, 3] is which is expected from studies of AL ‐ v x B s IMF coupling because most of the contribution to AL is from the north‐south component of the field, B x , in the local time range [2300, 0300] [ Allen and Kroehl , 1975]. At higher latitudes, the B z IMF dependence of f LT should take on a piecewise linear form [ Troshichev and Gusev , 1994], which can be written in terms of two slope parameters, s + and s − , Because the “hard‐rectifier” B z IMF dependence of is the case of s + = 0, a gradual increase in s + from auroral zone to high‐latitude locations is expected.…”

Section: Methodsmentioning

confidence: 97%

“…which is expected from studies of AL-v x B s IMF coupling because most of the contribution to AL is from the northsouth component of the field, B x , in the local time range [2300, 0300] [Allen and Kroehl, 1975]. At higher latitudes, the B z IMF dependence of f LT should take on a piecewise linear form [Troshichev and Gusev, 1994], which can be written in terms of two slope parameters, s + and s À ,…”

Section: Methodsmentioning

confidence: 99%

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Solar wind coupling to and predictability of ground magnetic fields and their time derivatives

2003

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[1] A spatial and dynamic study of solar wind driving of high-latitude ground magnetic fields and their time derivatives is given. Nonlinear, data-derived basis functions are used to determine the optimal solar wind driven dynamic coupling function at high-latitude locations. The method does not assume a solar wind driving function a priori so that an unbiased determination of the relative influence of different driving processes can be made. Using this method, the locations where high-latitude models capture signatures of different driving processes, such as reconnection and the Kelvin-Helmholtz instability, are revealed for both the amplitude of the field and its time derivative. The time rate of change of the field is a disturbance measure related to geomagnetically induced currents. For the amplitude of the ground magnetic field the primary driver is reconnection; the time rate of change of the field has signatures of both reconnection driving in the nightside sector and Kelvin-Helmholtz driving in the prenoon sector. The independent influence of the solar wind ion density and azimuthal component of the magnetic field in driving magnetic field fluctuations is found to be small at auroral-zone latitudes. The data-derived coupling functions are also used to estimate the expected prediction error of a general class of models that specify the ground magnetic field or its time derivative given solar wind plasma measurements. Prediction efficiencies as small as zero and as large as 0.7 for both the amplitude of the field and its time derivative are possible. The prediction efficiency is highly dependent on spatial location and the direction of field being predicted.

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Section: Methodsmentioning

confidence: 97%

Section: Methodsmentioning

confidence: 99%

Solar wind coupling to and predictability of ground magnetic fields and their time derivatives

2003

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“…Rodrigues et al (1992) components' signs on the PCA behaviour were discussed in numerous papers (e.g. Lassen and Danielsen, 1978;Sergeev, 1979, 1981;Gussenhoven, 1982;Troshichev and Gusev, 1994). Lassen and Danielsen (1978) showed with data from stations in Greenland that in the Northern Hemisphere PCAs occur more often for B IMF y > 0 and B IMF x < 0.…”

Section: Discrete Auroras In the Polar Capmentioning

confidence: 98%

Investigations of the auroral luminosity distribution and the dynamics of discrete auroral forms in a historical retrospective

Feldstein

Vorobjev

Zverev

et al. 2014

Hist. Geo Space. Sci.

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“…Particularly, IMF B y was strong and negative, with a maximum magnitude of ∼−15 nT. Note that the IMF B y polarity affects dayside and nightside auroral particle precipitation (Holappa et al., 2020; Makita et al., 1991; Reistad et al., 2020; Shen et al., 2022; Troshichev & Gusev, 1994) and the circulation of neutral winds (Mccormac et al., 1985, 1991). On the one hand, the analysis by Liou et al.…”

Section: Discussionmentioning

confidence: 99%

A Numerical Investigation on the Formation of the Stalling of the Cross‐Polar Jet in Midnight Thermospheric Winds

Tan,

Dang,

Lei

et al. 2023

JGR Space Physics

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Thermospheric winds usually flow from noon to the midnight inside the polar cap and spill further equatorward around midnight, due to the combined effects of solar radiation‐driven pressure gradient and ion drag. Recent observations from the Scanning Doppler Imager at Poker Flat indicated a distinct feature that the cross‐polar jet stalls over short horizontal distances around the magnetic midnight. However, the mechanisms responsible for the occurrence of stalling have not been well understood. In this study, we investigated the physical mechanisms of the stalling of the cross‐polar jet based on the Thermosphere Ionosphere Electrodynamics General Circulation Model simulations. The model reproduced the general stalling features at midnight over a short horizontal distance. The occurrence of stalling is mainly associated with Joule heating, which enhances the neutral temperature and then turns winds poleward by the pressure gradient force, and ion‐neutral coupling, which drags neutral winds westward in the pre magnetic local time midnight sector and contributes to the poleward turning of the meridional winds by the poleward Coriolis force. Meanwhile, the stalling region has a large latitudinal range and depends on the interplanetary magnetic field (IMF). Under southward IMF Bz, thermospheric winds are likely to stall at lower latitudes associated with strong ionospheric convection. The stalling of the cross‐polar jet in the midnight thermospheric winds has UT/longitude dependence, which could be associated with the orientation of the alignment of geomagnetic and geographic poles with respect to ionospheric convection.

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IMF Bx and By dependencies of the polar cap auroral distribution for northward IMF orientation inferred from observations at Vostok station

Cited by 8 publications

References 20 publications

Solar wind coupling to and predictability of ground magnetic fields and their time derivatives

Solar wind coupling to and predictability of ground magnetic fields and their time derivatives

Investigations of the auroral luminosity distribution and the dynamics of discrete auroral forms in a historical retrospective

A Numerical Investigation on the Formation of the Stalling of the Cross‐Polar Jet in Midnight Thermospheric Winds

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