ESTIMATIONS OF LOCAL MAGNETIC FIELDS IN SOLAR FLARES: BASIC METHODS AND SOME RESULTS

Автор(и)

  • V. G. Lozitsky Astronomical Observatory of the Taras Shevchenko National University of Kyiv, Україна
  • E. A. Baranovsky Crimea Astrophysical Observatory, Nauchny, Crimea,
  • N. I. Lozitska Astronomical Observatory of the Taras Shevchenko National University of Kyiv, Україна
  • V. P. Tarashchuk Crimea Astrophysical Observatory, Nauchny, Crimea,

DOI:

https://doi.org/10.18524/1810-4215.2017.30.114690

Ключові слова:

Sun, solar activity, solar flares, magnetic Fields, spectral lines, the Zeeman effect, diagnostics of spatially unresolved structures, extremely strong fields

Анотація

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. 

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Опубліковано

2017-11-10

Номер

Том 30 (2017)

Розділ

Сонце та Сонячна система

Ліцензія

Авторське право (c) 2017 Odessa Astronomical Publications

Creative Commons License

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Відповідно Закону України про авторське право і суміжні права N 3792-XII від 23 грудня 1993 року