The Relation Between Magnetic Fields and X-ray Emission for Solar Microflares and Active Regions
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 ±0.86 , 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 PFF (B ) and PFF (Φ ) for microflares are 3.87 ±2.16 and 3 ±1.6 , 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.
- Publication:
-
Solar Physics
- Pub Date:
- September 2017
- DOI:
- 10.1007/s11207-017-1146-8
- arXiv:
- arXiv:1707.09144
- Bibcode:
- 2017SoPh..292..120K
- Keywords:
-
- Flares;
- Microflares and nanoflares;
- Magnetic fields;
- Photosphere;
- Astrophysics - Solar and Stellar Astrophysics;
- 85-05
- E-Print:
- 17 pages, 12 figures