Study of Geomagnetic Disturbances from Satellite Data in Magnetic Storm on 8–9 March 1970

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Resumo

In this study, we consider historical geomagnetic satellite data obtained during a strong magnetic storm on March 8−9, 1970. In addition to the data of the Soviet satellite Kosmos-321, data from the American satellite OGO-6, which performed geomagnetic measurements at the same time, were used. We analyzed time variations of external magnetic fields recorded in satellite and ground-based observations of the magnetic field. The research also gave impetus to the creation of the improved software implementation of the auroral oval model APM, which enables reconstruction of its position and precipitation intensity in both the past and near real time. The magnetic variations originating in the near-Earth space from various sources were identified. In particular, we revealed the signatures of the storm-time ring current and equatorial and auroral electrojects. The paper highlights the enduring value of historical data of magnetic field observations stored in data centers and continuously digitized by their staff.

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Sobre autores

A. Soloviev

Geophysical Center RAS; Schmidt Institute of Physics of the Earth RAS

Autor responsável pela correspondência
Email: a.soloviev@gcras.ru
Rússia, Moscow; Moscow

I. Belov

Geophysical Center RAS

Email: i.belov@gcras.ru
Rússia, Moscow

A. Vorobev

Geophysical Center RAS; Ufa University of Science and Technology

Email: geomagnet@list.ru
Rússia, Moscow; Ufa

V. Sergeyev

Geophysical Center RAS

Email: v.sergeev@gcras.ru
Rússia, Moscow

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2. Fig 1. Dst-index values from January 20 to March 13, 1970 (https://omniweb.gsfc.nasa.gov).

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3. Fig. 2. Parameters of the interplanetary magnetic field and solar wind for March 6-10, 1970: (a) - components Bz and By in the GSE coordinate system, velocity V and density n; (b) - geomagnetic activity indices Kp, AE and Dst. The circles on the Dst plot indicate the time marks of rotations 744, 745-746 and 760 of the Cosmos-321 satellite.

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4. Fig. 3. Turns of the Cosmos-321 satellite, the data for which are given in the catalog [Dolginov et al., 1976], with their numbers indicated.

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5. Fig. 4. Flight of Cosmos-321 satellite over the polar cap of the southern hemisphere at turn 760 in the coordinates “corrected geomagnetic latitude”-“local magnetic time”. The satellite trajectory with UT counts, the perturbed field component δT along the trajectory, and the position of the auroral oval are shown [Dolginov et al., 1972].

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6. Fig. 5. Variability of the perturbed component of the dF field for the period from 00:00 UT on March 8 to 23:59 UT on March 9, 1970. Black indicates overflights on the night side, gray - on the day side.

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7. Fig. 6. Character of changes in the perturbed component of the field dF per revolution q1 according to the OGO-6 satellite data with additional parameters: (a) - the diamond marks the values of the AE index (time resolution of the original data - 1 hour), the circle marks the Kp index (resolution of the original data - 3 hours), the cross marks the Dst index (resolution of the original data - 1 hour); (b) - the diamond marks the values of the solar wind speed, the circle marks the plasma temperature, the cross marks the proton density (resolution of all these data - 1 hour). The legend and the scale for additional parameters are on the right side of the graph. Vertical dashed lines mark the place of crossing of the conditional terminator (change of day side to night side and vice versa).

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8. Fig. 7. Character of changes in the perturbed component of the field dF per revolution q2 from the data of the OGO-6 satellite. The notations are similar to Fig. 6а.

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9. Fig. 8. Character of changes in the perturbed component of the field dF from the data of the OGO-6 satellite: (a) - for a spiral d1

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10. Fig. 8 (continued). Character of changes in the perturbed component of the dF field according to the OGO-6 satellite data: (b) - for the d2 spiral, (c) - for the d3 spiral, (d) - for the d4 spiral. The designations are similar to Fig. 6.

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11. Fig. 9. Areas of diffuse rashes (A), auroral oval (B), and soft diffuse rashes (C): (a) at 06:00 UT on March 6, 1970 (~roll q1), (b) at 23:00 UT on March 9, 1970 (~roll d4), (c) at 12:00 UT on March 10, 1970 (~roll q2). The dotted line shows fragments of the satellite trajectories when crossing the polar region and indicates the UT time marks at their ends. The maps are given in “geographic latitude”-“local time” coordinates. The maps are constructed according to the improved software implementation of the APM auroral precipitation model.

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