文章基本信息

标题：Launch of a CME-associated eruptive prominence as observed with IRIS and ancillary instruments ⋆
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作者：P. Zhang ; É. Buchlin ; J.-C. Vial 等
期刊名称：Astronomy & Astrophysics
印刷版ISSN：0004-6361
电子版ISSN：1432-0746
出版年度：2019
卷号：624
DOI：10.1051/0004-6361/201834259
语种：English
出版社：EDP Sciences
摘要：Aims. In this paper we focus on the possible observational signatures of the processes which have been put forward for explaining eruptive prominences. We also try to understand the variations in the physical conditions of eruptive prominences and estimate the masses leaving the Sun versus the masses returning to the Sun during eruptive prominences.Methods. As far as velocities are concerned, we combined an optical flow method on the Atmospheric Imaging Assembly (AIA) 304 Å and Interface Region Imaging Spectrograph (IRIS). Mg IIh&k observations in order to derive the plane-of-sky velocities in the prominence, and a Doppler technique on the IRIS Mg IIh&k profiles to compute the line-of-sight velocities. As far as densities are concerned, we compared the absolute observed intensities with values derived from non-local thermodynamic equilibrium radiative transfer computations to derive the total (hydrogen) density and consequently compute the mass flows.Results. The derived electron densities range from 1.3 × 109to 6.0 × 1010cm−3and the derived total hydrogen densities range from 1.5 × 109to 2.4 × 1011cm−3in different regions of the prominence. The mean temperature is around 1.1 × 104K, which is higher than in quiescent prominences. The ionization degree is in the range of 0.1–10. The total (hydrogen) mass is in the range of 1.3 × 1014–3.2 × 1014g. The total mass drainage from the prominence to the solar surface during the whole observation time of IRIS is about one order of magnitude smaller than the total mass of the prominence.
关键词：enSun: filaments, prominencesSun: coronal mass ejections (CMEs)techniques: spectroscopic