Non-LTE Inversion of Prominence Spectroscopic Observations in H alpha and Mg ii h&k lines

0558363 - ASÚ 2023 RIV GB eng J - Článek v odborném periodiku
Jejčič, S. - Heinzel, Petr - Schmieder, B. - Gunár, Stanislav - Menin, P. - Mein, N. - Ruan, G.
Non-LTE Inversion of Prominence Spectroscopic Observations in H alpha and Mg ii h&k lines.
Astrophysical Journal. Roč. 932, č. 1 (2022), č. článku 3. ISSN 0004-637X. E-ISSN 1538-4357
Grant CEP: GA ČR(CZ) GA19-17102S; GA ČR GA19-16890S
Institucionální podpora: RVO:67985815
Klíčová slova: energy-balance * quiet-sun * solar spectrograph
Obor OECD: Astronomy (including astrophysics,space science)
Impakt faktor: 4.9, rok: 2022
Způsob publikování: Open access

We continued our investigation of the plasma characteristics of a quiescent prominence that occurred on 2017 March 30. The prominence was observed simultaneously by several instruments, including the Interface Region Imaging Spectrograph (IRIS) and the Multichannel Subtractive Double Pass (MSDP) spectrograph operating at the Meudon solar tower. We focused on IRIS Mg ii h&k and MSDP H alpha spectra, selecting 55 well-coaligned points within the prominence. We computed an extensive grid of 63,000 isothermal and isobaric 1D-slab prominence models with a non-LTE (i.e., departures from the local thermodynamic equilibrium) radiative transfer code. We then performed a 1.5D spectral inversion searching for an optimal model that best fits five parameters of the observed profiles (observables), namely, the integrated intensity of the H alpha and Mg ii k lines, the FWHM of both lines, and the ratio of intensities of the Mg ii k and Mg ii h lines. The latter is sensitive to temperature. Our results show that the prominence is a low-temperature structure, mostly below 10,000 K, with some excursions to higher values (up to 18,000 K) but also rather low temperatures (around 5000 K). The microturbulent velocity is typically low, peaking around 8 km s(-1), and electron density values are of the order of 10(10) cm(-3). The peak effective thickness is 500 km, although the values range up to 5000 km. The studied prominence is rather optically thin in the H alpha line and optically thick in the Mg ii h&k lines.
Trvalý link: http://hdl.handle.net/11104/0332243