Hot prominence detected in the core of a coronal mass ejection II. Analysis of the C III line detected by SOHO/UVCS

0482411 - ASÚ 2018 RIV FR eng J - Článek v odborném periodiku
Jejčič, S. - Susino, R. - Heinzel, Petr - Dzifčáková, Elena - Bemporad, A. - Anzer, U.
Hot prominence detected in the core of a coronal mass ejection II. Analysis of the C III line detected by SOHO/UVCS.
Astronomy & Astrophysics. Roč. 607, November (2017), A80/1-A80/10. ISSN 0004-6361. E-ISSN 1432-0746
Grant CEP: GA ČR(CZ) GA16-18495S
Institucionální podpora: RVO:67985815
Klíčová slova: line formation * radiative transfer * coronal mass ejections
Obor OECD: Astronomy (including astrophysics,space science)
Impakt faktor: 5.565, rok: 2017

We study the physics of erupting prominences in the core of coronal mass ejections (CMEs) and present a continuation of a previous analysis. We analyzed 39 observational points along the whole erupting prominence because for these points we found a solution for the kinetic temperature and microturbulent velocity. For these points we ran the non-LTE code to determine best-fit models. All models with tau(0)(L alpha) <= 0.3 and tau(0)(C III) <= 0.3 were analyzed further, for which we computed the integrated intensity of the C III line using a two-level atom. The best agreement between computed and observed integrated intensity led to 30 optically thin points along the prominence. The results are presented as histograms of the kinetic temperature, microturbulent velocity, effective thickness, radial flow velocity, electron density, and gas pressure. We also show the relation between the microturbulence and kinetic temperature together with a scatter plot of computed versus observed C III integrated intensities and the ratio of the computed to observed C III integrated intensities versus kinetic temperature.

Trvalý link: http://hdl.handle.net/11104/0277819