Simultaneous observations of very low frequency auroral hiss, aurora, and irregular geomagnetic pulsations at the Lovozero observatory

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We presented the results of the analysis of the auroral hiss bursts and geomagnetic pulsations recorded at the Lovozero Observatory. The dynamics of the location of the region on the Earth’s surface, illuminated by the auroral hiss, is compared with the dynamics of the aurora accompanying the occurrence of the hiss. We found events when hiss bursts and pulsations occur simultaneously with the appearance of aurora or with an increase in their brightness. Based on the analysis, we proposed a mechanism of possible connection between the observed phenomena.

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作者简介

A. Nikitenko

Polar Geophysical Institute

编辑信件的主要联系方式.
Email: alex.nikitenko91@gmail.com
俄罗斯联邦, Apatity

Yu. Fedorenko

Polar Geophysical Institute

Email: alex.nikitenko91@gmail.com
俄罗斯联邦, Apatity

N. Kleymenova

Schmidt Institute of Physics of Earth of the Russian Academy of Sciences

Email: alex.nikitenko91@gmail.com
俄罗斯联邦, Moscow

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2. Fig. 1. The event on 19 December 2018 at 22:06-22:09 UT. Spectrograms of the X-component of the geomagnetic field Pi1B-pulsation geomagnetic field in the range 0.03-1 Hz (a) and the horizontal component of the VLF magnetic field in the range 2-14 kHz (b), distributions of the azimuthal angle of the vector inverse to the Poynting vector (c), all-sky camera images from observations at the Verkhnetulomsky Observatory (d)

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3. Fig. 2. Event on 1 February 2019 at 19:20-19:55 UT. Keogram of polar auroras from observations at the Lovozero Observatory and all-sky camera images during the observation intervals of auroral hiss bursts (19:26:30 UT, 19:38:40 UT and 19:50:50 UT) and in the breaks between their appearance (19:32:40 UT and 19:45:10 UT) (a), spectrograms of the X-component of the geomagnetic field of Pi1B pulsations in the range of 0. 03-0.5 Hz (b) and the horizontal component of the VLF magnetic field in the range 2-14 kHz (c)

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4. Fig. 3. Event on 28 February 2019 at 19:11-19:14 UT. Spectrograms of the X-component of the geomagnetic field of Pi1B pulsations in the range 0. 03-1 Hz (a) and the horizontal component of the VLF magnetic field in the range 2-14 kHz (b); maxima of the distributions of the azimuthal angle of the inverse Poynting vector (c) and circular polarisation index (d); the keogram of polar auroras constructed from the observations at the Lovozero Observatory for the interval 19: 05-19:20 UT, red line means the time of auroral hiss observation (e); all-sky camera images based on observations at Lovozero Observatory (f)

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