Estimations of Local Magnetic Fields in Solar Flares: Basic Methods and Some Results
Abstract
We consider three methods for estimations of local magnetic fields in solar flares: (1) analysis of bisectors of I ± V profiles (Lozitsky, 2015); (2) search for Zeeman-like effects in cores of spectral lines with very low Lande factors, geff ≈ 0.01 (Lozitsky, 1993, 1998); (3) semi-empirical modeling using many spectral lines and two-component models (see, e.g., Lozitsky et al., 2000). We illustrate the application of named methods to different observational data and to different spectral lines. Our main conclusions are following: (a) upper limit of local magnetic fields in solar flares is, at least, ∼104 G, (b) such extremely strong fields can occur in very small, spatially unresolved scales, (c) lifetime of such fields is, at least, a few minutes.
- Publication:
-
Odessa Astronomical Publications
- Pub Date:
- 2017
- DOI:
- 10.18524/1810-4215.2017.30.114690
- Bibcode:
- 2017OAP....30..232L
- Keywords:
-
- Sun;
- solar activity;
- solar flares;
- magnetic Fields;
- spectral lines;
- the Zeeman effect;
- diagnostics of spatially unresolved structures;
- extremely strong fields