Preflare X-Ray Pulsations with Sources Outside
the Main Flare Active Region

I. V. Zimovets; Зимовец И. В.; I. N. Sharykin; Шарыкин И. Н.; T. I. Kaltman; Кальтман Т. И.; A. G. Stupishin; Ступишин А. Г.; B. A. Nizamov; Низамов Б. А.

doi:10.31857/S0016794023600345

Preflare X-Ray Pulsations with Sources Outside the Main Flare Active Region

Authors: Zimovets I.V.¹, Sharykin I.N.¹, Kaltman T.I.², Stupishin A.G.³, Nizamov B.A.⁴
Affiliations:
1. Space Research Institute, Russian Academy of Sciences (IKI RAN)
2. Special Astrophysical Observatory, Russian Academy of Sciences (SAO RAN)
3. St. Petersburg State University (SPBU)
4. Sternberg Astronomical Institute, Moscow State University (GAISh MGU)
Issue: Vol 63, No 5 (2023)
Pages: 547-560
Section: Articles
URL: https://journals.rcsi.science/0016-7940/article/view/134745
DOI: https://doi.org/10.31857/S0016794023600345
EDN: https://elibrary.ru/DLHDSR
ID: 134745

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Abstract
About the authors
References
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Abstract

Earlier, we showed that according to the nature of the location of sources of preflare X-ray pulsations
relative to the main solar flare, events are divided into at least two types: in type I events, the sources of
pulsations and the main flare are in the same active region (AR) and in type II events they are in different
regions. This paper presents an analysis of a type II event in which, according to data from the Ramaty High-
Energy Solar Spectroscopic Imager (RHESSI) space observatory, X-ray sources of preflare quasi-periodic
pulsations (with a period P = 1.5 ± 0.1 min), which began at ~1802 UT, were located in AR 11884 in the Western
Hemisphere, and the sources of the main flare M1.0 SOL2013-11-05T18:08 were located in AR 11890 in
the Eastern Hemisphere. The pulsations were also observed with the Gamma-Ray Burst Monitor (GBM)
aboard the Fermi space observatory and the X-Ray Sensor (XRS) aboard the Geostationary Operational
Environmental Satellite (GOES), excluding the possibility of their artificial origin. According to the data of
the Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory (SDO) in the extreme
ultraviolet range, it was found that the sources of pulsations were located at the base of coronal jets that flowed
out at velocities of ~100–1500 km/s. The distance between AR 11884 and AR 11890 was ~1.4 RS. It would
take ~17–250 min for the jet plasma to reach AR 11890, which is much longer than the time interval between
the onset of pulsations (jets) and the flare (~6 min). No loops connecting AR 11884 and AR 11890 were
observed in the corona. Moreover, no connection of these regions by magnetic field lines extrapolated from
the photosphere to the corona in the potential approximation was found. These arguments indicate that the
jets (and associated pulsations) could not be the trigger for the flare. Thus, a vivid example of an event is presented
in which there was no physical connection between preflare X-ray pulsations (and jets) and the flare
that followed them. This event demonstrates the importance of spatially resolved observations in the study of
pulsations on the Sun and stars.

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