Understanding the Mg II and Halpha Spectra in a Highly Dynamical Solar Prominence

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F15%3A00444953" target="_blank" >RIV/67985815:_____/15:00444953 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1088/2041-8205/800/1/L13" target="_blank" >http://dx.doi.org/10.1088/2041-8205/800/1/L13</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/2041-8205/800/1/L13" target="_blank" >10.1088/2041-8205/800/1/L13</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Understanding the Mg II and Halpha Spectra in a Highly Dynamical Solar Prominence

Popis výsledku v původním jazyce

We discuss the possibility to interpret the unreversed single profiles by using a two-dimensional (2D) model of the entire prominence body with specific radiative boundary conditions. We have performed new 2D isothermal-isobaric modeling of both H alphaand Mg II lines and show the ability of such models to account for the line profile variations as observed. However, the Mg II line-center intensities require the model with a temperature increase toward the prominence boundary. We show that even simpleone-dimensional (1D) models with a prominence-to-corona transition region (PCTR) fit the observed Mg II and H alpha lines quite well, while the isothermal-isobaric models (1D or 2D) are inconsistent with simultaneous observations in the Mg II h and k andH alpha lines, meaning that the H alpha line provides a strong additional constraint on the modeling. IRIS far-UV detection of the C II lines in this prominence seems to provide a direct constraint on the PCTR part of the model.

Název v anglickém jazyce

Understanding the Mg II and Halpha Spectra in a Highly Dynamical Solar Prominence

Popis výsledku anglicky

We discuss the possibility to interpret the unreversed single profiles by using a two-dimensional (2D) model of the entire prominence body with specific radiative boundary conditions. We have performed new 2D isothermal-isobaric modeling of both H alphaand Mg II lines and show the ability of such models to account for the line profile variations as observed. However, the Mg II line-center intensities require the model with a temperature increase toward the prominence boundary. We show that even simpleone-dimensional (1D) models with a prominence-to-corona transition region (PCTR) fit the observed Mg II and H alpha lines quite well, while the isothermal-isobaric models (1D or 2D) are inconsistent with simultaneous observations in the Mg II h and k andH alpha lines, meaning that the H alpha line provides a strong additional constraint on the modeling. IRIS far-UV detection of the C II lines in this prominence seems to provide a direct constraint on the PCTR part of the model.

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

<a href="/cs/project/GAP209%2F12%2F0906" target="_blank" >GAP209/12/0906: Realistické modely slunečních protuberancí kombinující modelování přenosu záření a MHD simulace</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2015

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal Letters

ISSN

2041-8205

e-ISSN

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Svazek periodika

800

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

5

Strana od-do

"L13/1"-"L13/5"

Kód UT WoS článku

000349316000013

EID výsledku v databázi Scopus

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