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Oscillations accompanying a He I 10830 Å negative flare in a solar facula  

Andrei Chelpanov   Submitted: 2018-11-07 20:07

On 21 September 21 2012, we carried out spectral observations of a solar facula in the Si I 10827 Å , He I 10830 Å, and Hα spectral lines. Later, in the process of analyzing the data, we found a small-scale flare in the middle of the time series. Due to an anomalous increase in the absorption of the He I 10830 Å line, we identified this flare as a negative flare. The aim of this article is to study the influence of the negative flare on the oscillation characteristics in the facular photosphere and chromosphere. We measured line-of-sight (LOS) velocity and intensity of all the three lines as well as the half width of the chromospheric lines. We also used Helioseismic and Magnetic Imager (HMI) magnetic field data. The flare caused a modulation of all the studied parameters. In the location of the negative flare, the amplitude of the oscillations increased four times on average. In the adjacent magnetic field local maxima, the chromospheric LOS velocity oscillations appreciably decreased during the flare. The facular region oscillated as a whole with a 5-minute period before the flare, and this synchronicity was disrupted after the flare. The flare changed the spectral composition of the LOS magnetic field oscillations, causing an increase in the low-frequency oscillation power.

Authors: Andrei Chelpanov, Nikolai Kobanov
Projects: None

Publication Status: Accepted to Solar Physics
Last Modified: 2018-11-08 11:40
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Negative flare in the He I 10830 Å line in facula  

Andrei Chelpanov   Submitted: 2018-04-23 02:19

A small-scale flare SOL2012-09-21T02:19 (B2) occurred in a spotless active region that we observed at a ground-based telescope equipped with a spectrograph. During the flare, we registered an increase in absorption in the He I 10830 Å line by 25%, while other chromospheric and coronal spectral lines demonstrated increase in brightness at the same location. This phenomenon called negative flare had rarely been observed at the Sun before. In this paper, we describe the morphology of this flare and investigate its dynamics based on our spectral observations and space imaging data. The Hα and He I 10830 Å lines reach their extreme intensities 5 and 6 minutes after the 171 Å line. The brightening first occurred in the 171 Å and 193 Å Solar Dynamics Observatory (SDO) channels followed by the 94 Å, 304 Å, and 1600 Å signals ∼2 minutes after (for the maximum phases). However, the abrupt changes in line-of-sight (LOS) velocities in the chromospheric lines occur simultaneously with the intensity changes in the 304 Å and 1600 Å lines: we observed a downward motion that was followed by two upward motions. The measured horizontal speed of the perturbation propagation was close to 70 km s-1 both in the chromospheric and coronal lines. We assume that we observed the photoionization-recombination process caused by UV radiation from the transition region during the coronal flare. With this, we point out the difficulties in interpreting the time lag between the emission maximum in the SDO UV channels and the second absorption maximum in the He I 10830 Å line.

Authors: Nikolai Kobanov, Andrei Chelpanov, Vasiliy Pulyaev
Projects: None

Publication Status: Accepted in Journal of Atmospheric and Solar-Terrestrial Physics
Last Modified: 2018-04-25 12:15
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Influence of the Magnetic Field on Oscillation Spectra in Solar Faculae  

Andrei Chelpanov   Submitted: 2016-07-19 21:54

In this work, we studied oscillation parameters in faculae above magnetic knots and in the adjacent to them areas. Using SDO data we analysed oscillations in magnetic strength, Doppler velocity, and intensity signals for the lower photosphere, and in intensity for the higher levels. We found that in the magnetic field strength oscillation spectra in magnetic knots, peaks at a frequency of about 4.8 mHz appear, while there are no such frequencies in the adjacent facular patches of a moderate field strength. On the contrary, Doppler velocity photospheric oscillation spectra are similar for these types of regions: in both cases, the significant peaks are in the 2.5-4.5 mHz range, though the oscillations in magnetic knots are 2-3 times weaker than those at the facular periphery. At the upper photosphere, the dominant frequencies in magnetic knots are 0.5-1 mHz higher than in the medium-field regions. The transition region oscillations above magnetic knots mainly concentrate in the 3-6 mHz range, and those above moderate-field patches concentrate below 3 mHz.

Authors: Andrei A. Chelpanov, Nikolai I. Kobanov, Dmitry Y. Kolobov
Projects: None

Publication Status: Accepted in Solar Physics
Last Modified: 2016-07-20 12:23
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Abstracts by Author
Oscillations accompanying a He I 10830 ? negative flare in a solar facula
Negative flare in the He I 10830 ? line in facula
Influence of the Magnetic Field on Oscillation Spectra in Solar Faculae

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