Modification of auroral kilometric radiation spectra caused propagation in inhomogeneous cosmic plasma

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We have analyzed characteristics of electric components of the auroral kilometric radiation (AKR) detected onboard of two satellites, in the Earth’s inner magnetosphere (ERG) and in the solar wind (WIND). It is shown that spectra are modified as the result of AKR the propagation in plasma channels — high frequencies are suppressed. The computer simulation confirms experiments.

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作者简介

V. Kolpak

Space Research Institute of the Russian Academy of Sciences; Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation of the Russian Academy of Sciences

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Email: lera.kolpak@yandex.ru
俄罗斯联邦, Moscow; Moscow

M. Mogilevsky

Space Research Institute of the Russian Academy of Sciences

Email: lera.kolpak@yandex.ru
俄罗斯联邦, Moscow

D. Chugunin

Space Research Institute of the Russian Academy of Sciences

Email: lera.kolpak@yandex.ru
俄罗斯联邦, Moscow

A. Chernyshov

Space Research Institute of the Russian Academy of Sciences

Email: lera.kolpak@yandex.ru
俄罗斯联邦, Moscow

I. Moiseenko

Space Research Institute of the Russian Academy of Sciences

Email: lera.kolpak@yandex.ru
俄罗斯联邦, Moscow

参考

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2. Fig. 1. Simultaneous measurements of the mean radiative power (averaged over F frequencies): from 56 to 596 kHz for WIND with a 60 s step, from 54.9 to 596 kHz for ERG with an 8 s step. The measurements were performed on 02.05.2019 on two satellites: from 9:36 to 13:26, on board the WIND satellite (upper panel) and on board the ERG satellite (lower panel)

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3. Fig. 2. Schematic of the mutual location of the ACR source and the ERG and WIND satellites during the measurements on 07.03.2019 and 02.05.2019 (a). The view of the ecliptic plane from the (-ZGSE) side is presented. 07.03.2019 coordinates for the ERG satellite: X = -0.6; Y = 3.3; Z = 0.4; for the WIND satellite: X = 256; Y = -42; Z = 8.8 (in the GSE system, in RE units). 02.05.2019 coordinates for the ERG satellite: X = -3.3; Y = -1.7; Z = 0.6; for the WIND satellite: X = 205; Y = -71; Z = 1.5. Schematic of radiation capture into the plasma channel (b): 1 - force line on which the ACR source is located; 2 - plasma channel stretched along the magnetic field force line; 3 - illumination region of the channel end for frequencies f1 ≤ f ≤ f2; 4 - area of illumination for frequencies f2 ≤ f ≤ f ≤ f3; 5 - area of illumination for frequencies higher than f3; f1, f2, f3 - ACR frequencies, where f1 > f2 > f3; - solution of the ACR radiation cone; N1 - plasma density outside the channel; N2 - plasma density in the channel. The arrows show the propagation of radiation from the source and in the channel

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4. Fig. 3. ACR spectra recorded on 07.03.2019 at 17:00:30 on the WIND (upper panel) and ERG (lower panel) satellites

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5. Fig. 4. Results of calculation of the reflection coefficients from the channel wall (for the case (N1 - N2) / N1 = 0.67) for three angles: 85° (solid line), 80° (dotted line), 75° (dashed line)

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