Abstract
We present the result of a comparison between magnetic field parameters and the intensity of X-ray emission for solar microflares with Geosynchronous Operational Environmental Satellites (GOES) classes from A0.02 to B5.1. For our study, we used the monochromatic MgXII Imaging Spectroheliometer (MISH), the Full-disk EUV Telescope (FET), and the Solar PHotometer in X-rays (SphinX) instruments onboard the Complex Orbital Observations Near-Earth of Activity of the Sun-Photon CORONAS-Photon spacecraft because of their high sensitivity in soft X-rays. The peak flare flux (PFF) for solar microflares was found to depend on the strength of the magnetic field and on the total unsigned magnetic flux as a power-law function. In the spectral range 2.8 – 36.6 Å, which shows very little increase related to microflares, the power-law index of the relation between the X-ray flux and magnetic flux for active regions is \(1.48 \pm0.86\), which is close to the value obtained previously by Pevtsov et al. (Astrophys. J. 598, 1387, 2003) for different types of solar and stellar objects. In the spectral range 1 – 8 Å, the power-law indices for \(\mathrm{PFF}(B)\) and \(\mathrm{PFF}(\Phi)\) for microflares are \(3.87 \pm2.16\) and \(3 \pm1.6\), respectively. We also make suggestions on the heating mechanisms in active regions and microflares under the assumption of loops with constant pressure and heating using the Rosner–Tucker–Vaiana scaling laws.
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This work was supported by the Russian Science Foundation (RSF) grant No. 17-12-01567. We also thank the anonymous referee for a careful revision of the work and very useful comments that significantly improved the manuscript.
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Kirichenko, A.S., Bogachev, S.A. The Relation Between Magnetic Fields and X-ray Emission for Solar Microflares and Active Regions. Sol Phys 292, 120 (2017). https://doi.org/10.1007/s11207-017-1146-8
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DOI: https://doi.org/10.1007/s11207-017-1146-8