Latitudinal distribution of nighttime auroral precipitation during magnetic calm and near the time of substorm onset

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The unresolved problems of the physics of auroral substorms include the issue of localization and the mechanism of the start of the substorm expansion phase. The new information needed to solve this problem can be obtained by comparing the results of observations from low-altitude spacecraft with observations in the equatorial plane of the magnetosphere. For this purpose, the morphological projection method was used, which does not require knowledge about the configuration of the magnetic field. This paper considers the latitudinal profiles of the auroral precipitation characteristics at ionospheric altitudes obtained from DMSP F7 spacecraft observations and the radial distribution of ion pressure in the equatorial plane according to the THEMIS mission during periods of magnetic calm and at time intervals close to the auroral breakup. Special attention was paid to the position of the maximum energy flux of the precipitation of ions with energy larger than 3 keV and ion pressure profiles. The average ion pressure latitudinal profiles at low altitudes were determined and compared with the average pressure distributions in the equatorial plane of the magnetosphere under similar to averaged values of solar wind and geomagnetic activity parameters. It is shown that, if under geomagnetic calm the pressure maximum at low altitudes is mapped to geocentric distances of ~7−8 Re, before the substorm onset it is mapped to a distance of ~5−6 Re. The averaged values of the pressure maxima during the magnetic calm, as well as before and after substorm onset were obtained. The brightness of the auroral luminosity in the 557.7 nm emission was estimated from DMSP F7 observations of the average energy and energy flux of the precipitated electrons.

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作者简介

V. Vorobjev

Polar Geophysical Institute

编辑信件的主要联系方式.
Email: vorobjev@pgia.ru
俄罗斯联邦, Apatity, Murmansk Region

O. Yagodkina

Polar Geophysical Institute

Email: oksana41@mail.ru
俄罗斯联邦, Apatity, Murmansk Region

Е. Antonova

Moscow State University; Space Research Institute, Russian Academy of Sciences

Email: elizaveta.antonova@gmail.com

Skobeltsyn Institute of Nuclear Physics

俄罗斯联邦, Moscow; Moscow

I. Kirpichev

Space Research Institute, Russian Academy of Sciences

Email: ikir@iki.rssi.ru
俄罗斯联邦, Moscow

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2. Fig. 1. Variations of the interplanetary medium parameters and geomagnetic activity levels on October 08, 1986 in the interval 01:00-05:00 UT. From top to bottom are shown: variations of the Bz-component of the MMP and the dynamic pressure of the solar wind, variations of the AL-, SYM/H- and PC-indices of magnetic activity. The MMP and solar wind data are given in terms of the frontal point of the shock front. The transit time of the F7 satellite is indicated by the vertical dashed line.

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3. Fig. 2. Integral characteristics of the ejected particles from the F7 satellite observations on October 08, 1986 at 03:09-03:10 UT: (a)-the mean energies (Ei, keV) and energy fluxes (Fi, erg/cm2 s) of the ejected ions, (b)-the mean energies (Ee, keV) and energy fluxes (Fe, erg/cm2 s) of the ejected electrons. The corrected geomagnetic latitude (CGL) is plotted along the horizontal axis. Vertical dashed lines are the position of the b2i boundary.

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4. Fig. 3. Latitudinal profiles of ion pressure (a) and 557.7 nm emission luminosity (b) calculated from the data of Figs. 2a and 2b, respectively. Vertical dashed lines are the position of the b2i boundary.

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5. Fig. 4. Latitudinal mean ion pressure profiles, Pi (nPa): (a) - magnetically calm period, (b) - final stage of the substorm nucleation phase, (c) - initial stage of the substorm development phase. Vertical dashed lines are the average position of b2i.

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6. Fig. 5.Latitudinal mean profiles of the luminosity intensity of the 557.7 nm, I5577 (kR) emission. Panels (a-b) correspond to panels (a-c) in Fig.4.Vertical dashed lines are the average position of b2i.

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7. Fig. 6.Radial distribution of ion pressure in the pre-midnight sector of the Earth's magnetosphere during magnetically quiet periods at positive (a) and negative (b) polarity of the vertical component of the MMP.

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8. Fig. 7.Projection of the latitudinal ion pressure profile in the ionosphere into the equatorial plane of the magnetosphere (thin curve) and its comparison with observations in the equatorial plane (curve with dots). The upper panel is the magnetically quiet period; the lower panel is the final stage of the substorm nucleation phase.

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