Motions and magnetic fields in filaments

  • Р.К. Жигалкин Crimean Astrophysical Observatory, Nauchny, Crimea, Ukraine, 98409
  • Г.В. Руденко Институт солнечно-земной физики СОРАН, 664033, Иркутск, а/я-291, Россия
  • Н.Н. Степанян Crimean Astrophysical Observatory, Nauchny, Crimea, Ukraine, 98409
  • В.Г. Файнштейн Институт солнечно-земной физики СОРАН, 664033, Иркутск, а/я-291, Россия
  • Н.И. Штерцер Crimean Astrophysical Observatory, Nauchny, Crimea, Ukraine, 98409

Abstract

On the basis of developed method of the joint use of data about magnetic fields and brightness of filaments and coronal holes at different altitudes in the solar atmosphere as well as about velocities in the photosphere we obtained the following results:

  • The upward motion of matter is typical for filament channels in the form of bright stripes which envelope filaments during the observation in the НеI 1083 nm line.
  • Filament channels observed simultaneously in H-alpha and in НеI 1083 nm differ in size, emission characteristics and other parameters. It was concluded that the simultaneous investigation of filament channels in two spectral ranges allows us to make progress in understanding physics of their formation and evolution.
  • Most filaments observed in the НеI 1083 nm line consist of dark nodes with different velocity distribution in them. A possible interpretation of these nodes is suggested.
  • The altitude of distribution of the small-scale magnetic field in the vicinity of individual dark nodes of filaments in the solar atmosphere varies within 3 to 20 thousand kilometers.
  • The zero surface separating the large-scale magnetic field structures in corona and calculated in potential approximation changes inclination to the solar surface with an altitude and shifts over 1-2 days.
  • Observed emergence of a filament in the coronal hole (CH) was accompanied by the significant magnetic field variation in the CH region at the altitude within 0 to 30 square kilometers up to the change of predominant sign of the field over the whole area of CH. There is an assumption that it occurs at the stage of the CH extinction.

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Published
2008-12-26
How to Cite
Жигалкин Р., Руденко Г., Степанян Н., et al., 2008. Izvestiya Krymskoi Astrofizicheskoi Observatorii, vol. 104, no. 1, pp. 93-108. Available at: https://jn.craocrimea.ru/index.php/izvcrao/article/view/594 (Accessed: 4December2020)
Section
Research articles