Estimating the Energy of Solar and Stellar Superflares

M. M. Katsova; V. N. Obridko; D. D. Sokoloff; I. M. Livshits

doi:10.1134/S0016793221070094

Estimating the Energy of Solar and Stellar Superflares

M. M. Katsova^*
, V. N. Obridko
, D. D. Sokoloff
, I. M. Livshits

^*Corresponding author for this work

Lomonosov Moscow State University
RAS - Pushkov Institute of Terrestrial Magnetism, Ionosphere and Radiowave Propagation
RAS - Pulkovo Astronomical Observatory
Moscow Center of Fundamental and Applied Mathematics

Research output: Contribution to journal › Article › peer-review

3 Scopus citations

Abstract

Abstract: We discuss the current observations of the most powerful non-steady phenomena on solar-like stars. While remaining within even the most extreme solar ideas, it is very problematic to get the flare energy more than (3–5) × 10³⁴ erg, which is apparently an absolute upper limit for solar-type flares. For explanation of the higher flare energy, about of 10³⁶ erg, one need to adopt that spots with the magnetic field strength of a few kG should cover more than 30% of a hemisphere. This estimate leads to a mean magnetic field around 1 kG. New observational evidences for a presence of the strong magnetic fields on solar-like stars appeared recently. We discuss to what extent it is necessary to change the mechanisms of convection and dynamo with a corresponding change in the models of the atmosphere. We consider possible ways of solving the problem of the energy of superflares.

Original language	English
Pages (from-to)	1063-1068
Number of pages	6
Journal	Geomagnetism and Aeronomy
Volume	61
Issue number	7
DOIs	https://doi.org/10.1134/S0016793221070094
State	Published - Dec 2021
Externally published	Yes

Funding

Funders	Funder number
Basis Foundation	21-1-1-4-1
Russian Foundation for Basic Research	19-02-00191
Ministry of Education and Science of the Russian Federation	075-15-2020-780

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10.1134/S0016793221070094

Cite this

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title = "Estimating the Energy of Solar and Stellar Superflares",

abstract = "Abstract: We discuss the current observations of the most powerful non-steady phenomena on solar-like stars. While remaining within even the most extreme solar ideas, it is very problematic to get the flare energy more than (3–5) × 1034 erg, which is apparently an absolute upper limit for solar-type flares. For explanation of the higher flare energy, about of 1036 erg, one need to adopt that spots with the magnetic field strength of a few kG should cover more than 30\% of a hemisphere. This estimate leads to a mean magnetic field around 1 kG. New observational evidences for a presence of the strong magnetic fields on solar-like stars appeared recently. We discuss to what extent it is necessary to change the mechanisms of convection and dynamo with a corresponding change in the models of the atmosphere. We consider possible ways of solving the problem of the energy of superflares.",

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year = "2021",

month = dec,

doi = "10.1134/S0016793221070094",

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T1 - Estimating the Energy of Solar and Stellar Superflares

AU - Katsova, M. M.

AU - Obridko, V. N.

AU - Sokoloff, D. D.

AU - Livshits, I. M.

PY - 2021/12

Y1 - 2021/12

N2 - Abstract: We discuss the current observations of the most powerful non-steady phenomena on solar-like stars. While remaining within even the most extreme solar ideas, it is very problematic to get the flare energy more than (3–5) × 1034 erg, which is apparently an absolute upper limit for solar-type flares. For explanation of the higher flare energy, about of 1036 erg, one need to adopt that spots with the magnetic field strength of a few kG should cover more than 30% of a hemisphere. This estimate leads to a mean magnetic field around 1 kG. New observational evidences for a presence of the strong magnetic fields on solar-like stars appeared recently. We discuss to what extent it is necessary to change the mechanisms of convection and dynamo with a corresponding change in the models of the atmosphere. We consider possible ways of solving the problem of the energy of superflares.

AB - Abstract: We discuss the current observations of the most powerful non-steady phenomena on solar-like stars. While remaining within even the most extreme solar ideas, it is very problematic to get the flare energy more than (3–5) × 1034 erg, which is apparently an absolute upper limit for solar-type flares. For explanation of the higher flare energy, about of 1036 erg, one need to adopt that spots with the magnetic field strength of a few kG should cover more than 30% of a hemisphere. This estimate leads to a mean magnetic field around 1 kG. New observational evidences for a presence of the strong magnetic fields on solar-like stars appeared recently. We discuss to what extent it is necessary to change the mechanisms of convection and dynamo with a corresponding change in the models of the atmosphere. We consider possible ways of solving the problem of the energy of superflares.

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Estimating the Energy of Solar and Stellar Superflares

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