Diagnosis of the high-latitude ionosphere and spatio-temporal dynamics of auroral precipitation

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Resumo

Using high-latitude observations by the Polar Geophysical Institute, the development of a typical auroral substorm on September 13, 2013, is traced. The event, according to satellite data, is linked to solar wind parameters, physical magnetospheric domains, and boundaries. The characteristics of the spatial structure of polar auroras (scaling indices, anisotropy) have been determined for typical auroral structures (quiet and rayed arcs, breakup, pulsating bands, omega structures).

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Sobre autores

B. Kozelov

Polar Geophysical Institute

Autor responsável pela correspondência
Email: boris.kozelov@gmail.com
Rússia, Apatity

V. Vorobyov

Polar Geophysical Institute

Email: boris.kozelov@gmail.com
Rússia, Apatity

E. Titova

Polar Geophysical Institute

Email: boris.kozelov@gmail.com
Rússia, Apatity

T. Popova

Polar Geophysical Institute

Email: boris.kozelov@gmail.com
Rússia, Apatity

Bibliografia

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2. Fig. 1. Observations of auroras with the all-sky camera in Apatity 12-13.09.2013: above - auroral keogram for the whole interval; below - images of the whole sky at certain moments of time. Time - UT (Universal Time)

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3. Fig. 2. Magnetic measurements 12-13.09.2013 at the Lovozero PGI Observatory: three components of the magnetic field (a); ELF pulsations in the H-component of the magnetic field (b)

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4. Fig. 3. Interplanetary field data and activity indices for 12-13.09.09. 2013: delay in ACE satellite data to the sunflower point of the magnetosphere (OMNI data) (a); z-component of the interplanetary magnetic field B in GSM-coordinates, with the gap area in the OMNI data highlighted in red (b); z-component of the interplanetary magnetic field B in GSM-coordinates at the Sunspot from OMNI data, red dashed line shows the area taken from ACE data (c); 5-minute AE-index (d); SYM/H-index (e)

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5. Fig. 4. Image processing: frame from the all-sky camera (a), red frame - selection of the area in the image with regard to orientation; determination of the slope (spectral index) by the logarithmic plot of the dispersion of detailing coefficients from the scale for the selected area using the method from [11] in the scale range of 1.5-50 km (b); dependence of the spectral index on the azimuthal direction (mask orientation) (c)

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6. Fig. 5. Results of optical data processing for the interval 20:00-21:00 UT, 12.09.2013: dependence of the spectral index a in the ‘time-direction’ coordinates, light sides are shown on the direction axis (a); dependences of max(a), min(a) and min(a)/max(a) on time (b). Individual moments are marked with points 1-5, which are discussed in the text

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7. Fig. 6. The same as in Fig. 5, but for 23:00-24:00 UT, 12.09.2013. Individual moments are marked with points 6-9

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