Bulletin of Taras Shevchenko National University of Kyiv. Astronomy, no. 52, p. 7-11 (2015)

Estimations of local magnrtic fields in prominences which have great optical thickness in emissive elements

V. Lozitsky, Dr. Sci,
V. Masliukh, Ph. D.,
O. Botygina, eng,
Taras Shevchenko National University of Kyiv, Kyiv

According to observations, shape of bisectors of I ± V of profiles of Нα and D3 lines in prominences, as rule, do not correspond toapproximation of weak mono-component magnetic field. This follows from non-parallelism of bisectors, with maximum of their splitting around topof observed emissive profiles. These peculiarities can be explained in frame of two-component models of magnetic field. In some cases, the non-Gaussian shape of line prifiles are needed for this purpose that could be caused by great optical thickness in subtelescopic emissive elements of aprominence. According to simulations, in this case the direct measurements of maximum observed splitting of bisectors on intensity level 0.9(named as parameter В0.9) present very lowered values of true local magnetic fields in prominences – approximately 3–5 times.

Sun, prominences, optical thickness, local magnetic fields

Botygina, O.O., Lozyczkyj,V.G. 2012, Visn. Astronom. shk.,8,1–2, 159
Kurochka, L.N., Ostapenko,V.A. 1975, Soln. dannye, 7, 96
Lozyczkyj, V., Botygina,O., Maslyux,V.2014, Visn. Kyiv. nacz. un-tu imeni Tarasa Shevchenka. Astronomiya, 51, 31
Casini,R., Lopez Ariste,A., Tomczyk,S., Lites,W.B. 2003, Ap. J. Let.,598, 67
Gordovskyy, M., Lozitsky,V.G. 2014, SolarPhysics,289, 10, 3681
Kuckein,C., Centeno,R., Martinez Pillet,V.2009, Astronomy and Astrophyss,501, 3, 1113
Lozitsky, V.G., Botygina,O.A., 2012, AstronomyLetters,38, 6, 380
Trujillo Bueno,J., Merenda,L., Centeno,R.2005, Ap. J. Let.,619, 191

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