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

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F22%3A00558363" target="_blank" >RIV/67985815:_____/22:00558363 - isvavai.cz</a>

Výsledek na webu

<a href="http://hdl.handle.net/11104/0332243" target="_blank" >http://hdl.handle.net/11104/0332243</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-4357/ac6bf5" target="_blank" >10.3847/1538-4357/ac6bf5</a>

Jazyk výsledku

angličtina

Název v původním jazyce

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

Popis výsledku v původním jazyce

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.

Název v anglickém jazyce

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

Popis výsledku anglicky

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.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

Výsledek vznikl pri realizaci vícero projektů. Více informací v záložce Projekty.

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2022

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Astrophysical Journal

ISSN

0004-637X

e-ISSN

1538-4357

Svazek periodika

932

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

12

Strana od-do

3

Kód UT WoS článku

000807766200001

EID výsledku v databázi Scopus

2-s2.0-85132739829