Multiwavelength spectroscopic observations of a quiescent prominence

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F25%3A00643350" target="_blank" >RIV/67985815:_____/25:00643350 - isvavai.cz</a>

Výsledek na webu

<a href="https://hdl.handle.net/11104/0373291" target="_blank" >https://hdl.handle.net/11104/0373291</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202348830" target="_blank" >10.1051/0004-6361/202348830</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Multiwavelength spectroscopic observations of a quiescent prominence

Popis výsledku v původním jazyce

Aims. In this paper we focus on the analysis of the multiwavelength spectroscopic observations of a quiescent prominence. The spectral and geometrical parameters in the prominence were derived and used to constrain the nonlocal thermodynamic equilibrium (NLTE) radiative transfer models of the prominence. Applying this method with multiwavelength observations provides a good opportunity to reduce the large range of thermodynamic parameters in solar prominences. Methods. As far as velocities are concerned, we used time-slice and optical flow methods in order to derive the plane-of-sky (POS) velocities in the prominence, and used gravity center and peak position methods on Mg II h&k and H I Ly alpha profiles to compute the line-of-sight (LOS) velocities. As far as densities and temperatures are concerned, we used the integrated intensities and full width at half maximum (FWHM) values of the H alpha and the CaII H together with Mg II h&k lines to compare with values derived from the NLTE radiative transfer computations. Ionization degree and thickness of the prominence plasma could be further derived. Results. Opposite flows are observed along two strands between prominence barbs. The POS velocity can reach 20 km s(-1) and the largest LOS velocity is > 90 km s(-1). The derived electron densities range from 6.5 x 10(9) to 2.7 x 10(10) cm(-3) and the derived total hydrogen densities range from 7.4 x 10(9) to 6.6 x 10(10) cm(-3) in different regions of the studied prominence. The temperature ranges from 7000 to 14000 K. The ionization degree of hydrogen is in the range of 0.40 to 0.91. The comparison between averaged and modeled profiles of Mg II and Ly alpha lines shows that macro-velocities of 15 and 20 km s(-1) are required, respectively. Conclusions. The bulk motions among prominence barbs indicate that the prominence plasma is not confined within magnetic dips but exhibits a large-scale behavior. The presence of high-speed cool plasma flows, along with a wide range of plasma densities and temperatures, suggests that the prominence plasma is far from thermodynamic equilibrium and is inherently dynamic in nature.

Název v anglickém jazyce

Multiwavelength spectroscopic observations of a quiescent prominence

Popis výsledku anglicky

Aims. In this paper we focus on the analysis of the multiwavelength spectroscopic observations of a quiescent prominence. The spectral and geometrical parameters in the prominence were derived and used to constrain the nonlocal thermodynamic equilibrium (NLTE) radiative transfer models of the prominence. Applying this method with multiwavelength observations provides a good opportunity to reduce the large range of thermodynamic parameters in solar prominences. Methods. As far as velocities are concerned, we used time-slice and optical flow methods in order to derive the plane-of-sky (POS) velocities in the prominence, and used gravity center and peak position methods on Mg II h&k and H I Ly alpha profiles to compute the line-of-sight (LOS) velocities. As far as densities and temperatures are concerned, we used the integrated intensities and full width at half maximum (FWHM) values of the H alpha and the CaII H together with Mg II h&k lines to compare with values derived from the NLTE radiative transfer computations. Ionization degree and thickness of the prominence plasma could be further derived. Results. Opposite flows are observed along two strands between prominence barbs. The POS velocity can reach 20 km s(-1) and the largest LOS velocity is > 90 km s(-1). The derived electron densities range from 6.5 x 10(9) to 2.7 x 10(10) cm(-3) and the derived total hydrogen densities range from 7.4 x 10(9) to 6.6 x 10(10) cm(-3) in different regions of the studied prominence. The temperature ranges from 7000 to 14000 K. The ionization degree of hydrogen is in the range of 0.40 to 0.91. The comparison between averaged and modeled profiles of Mg II and Ly alpha lines shows that macro-velocities of 15 and 20 km s(-1) are required, respectively. Conclusions. The bulk motions among prominence barbs indicate that the prominence plasma is not confined within magnetic dips but exhibits a large-scale behavior. The presence of high-speed cool plasma flows, along with a wide range of plasma densities and temperatures, suggests that the prominence plasma is far from thermodynamic equilibrium and is inherently dynamic in nature.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2025

Kód důvěrnosti údajů

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

Název periodika

Astronomy & Astrophysics

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

703

Číslo periodika v rámci svazku

Nov.

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

14

Strana od-do

A145

Kód UT WoS článku

001616252400007

EID výsledku v databázi Scopus

2-s2.0-105021991971