Coronal dimming parameters and their variations in the 24th solar cycle

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Аннотация

We analyzed coronal dimming parameters and their relation to coronal mass ejections to determine the location of possible ejections sources on the solar disk in the 24th solar cycle. We used Solar Demon database that contains flares and dimmings parameters obtained from SDO/AIA image. Coronal mass ejections from the CACTus database were associated with 16% of all the dimmings for the period 2010–2018. On average, dimmings associated with coronal mass ejections are events with large absolute parameter values. Correlation coefficient between dimming position angle and associated coronal mass ejection position angle is 0.96. Correlation coefficients between the coronal mass ejection speed and dimming parameters are close to 0.5 for dimmings in the central region of the solar disk. Obtained results can be used to model coronal mass ejections propagation and to define the probability of their arrival in near-Earth space.

Толық мәтін

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Авторлар туралы

A. Vakhrusheva

Lomonosov Moscow State University (MSU)

Хат алмасуға жауапты Автор.
Email: vakhr.anna@gmail.com

Skobeltsyn Institute of Nuclear Physics (SINP), Faculty of Physics

Ресей, Moscow

Yu. Shugay

Lomonosov Moscow State University (MSU)

Email: vakhr.anna@gmail.com

Skobeltsyn Institute of Nuclear Physics (SINP)

Ресей, Moscow

K. Kaportseva

Lomonosov Moscow State University (MSU)

Email: vakhr.anna@gmail.com

Skobeltsyn Institute of Nuclear Physics (SINP), Faculty of Physics

Ресей, Moscow

V. Eremeev

Lomonosov Moscow State University (MSU)

Email: vakhr.anna@gmail.com

Skobeltsyn Institute of Nuclear Physics (SINP)

Ресей, Moscow

V. Kalegaev

Lomonosov Moscow State University (MSU)

Email: vakhr.anna@gmail.com

Skobeltsyn Institute of Nuclear Physics (SINP), Faculty of Physics

Ресей, Moscow

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2. Fig. 1. Calculation of the position angle for dimming (left) and VCR (right).

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3. Fig. 2. Histograms of the distribution of dimming parameters: (a) – maximum value of the full brightness module; (b) — maximum brightness jump; (c) — maximum area; (d) — dimming duration. On the Y axis on the left is the number of events for all dimmings (black columns), on the right is the number of events for dimmings associated with the CME (shaded columns). The curves indicate the density approximation of the lognormal distribution.

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4. Fig. 3. Variations in solar activity events over the years. On the Y axis on the left is the number of events (dimmings, flares, CMEs), on the right is the annual average number of sunspots according to WDC-SILSO data (https://www.sidc.be/silso/datafiles).

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5. Fig. 4. Dependence of the average dimming latitude on time for 2010–2018.

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6. Fig. 5. Dependence of the average CME speed in the coronagraph on the maximum dimming area for all corresponding CMEs and dimmings. The straight line denotes the linear dependence of the logarithms of the parameters.

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7. Fig. 6. Dependence of the average CME speed in the coronagraph on the maximum dimming area. The calculation was made for a sample of dimmings from the central region of the solar disk. The straight line denotes the linear dependence of the logarithms of the parameters.

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8. Fig. 7. Dependence of the VCR position angle on the dimming position angle. The straight line denotes the linear dependence of the parameters.

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