Hot prominence detected in the core of a coronal mass ejection II. Analysis of the C III line detected by SOHO/UVCS

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F17%3A00482411" target="_blank" >RIV/67985815:_____/17:00482411 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201731364" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201731364</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201731364" target="_blank" >10.1051/0004-6361/201731364</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Hot prominence detected in the core of a coronal mass ejection II. Analysis of the C III line detected by SOHO/UVCS

Popis výsledku v původním jazyce

We study the physics of erupting prominences in the core of coronal mass ejections (CMEs) and present a continuation of a previous analysis. We analyzed 39 observational points along the whole erupting prominence because for these points we found a solution for the kinetic temperature and microturbulent velocity. For these points we ran the non-LTE code to determine best-fit models. All models with tau(0)(L alpha) <= 0.3 and tau(0)(C III) <= 0.3 were analyzed further, for which we computed the integrated intensity of the C III line using a two-level atom. The best agreement between computed and observed integrated intensity led to 30 optically thin points along the prominence. The results are presented as histograms of the kinetic temperature, microturbulent velocity, effective thickness, radial flow velocity, electron density, and gas pressure. We also show the relation between the microturbulence and kinetic temperature together with a scatter plot of computed versus observed C III integrated intensities and the ratio of the computed to observed C III integrated intensities versus kinetic temperature.n

Název v anglickém jazyce

Hot prominence detected in the core of a coronal mass ejection II. Analysis of the C III line detected by SOHO/UVCS

Popis výsledku anglicky

We study the physics of erupting prominences in the core of coronal mass ejections (CMEs) and present a continuation of a previous analysis. We analyzed 39 observational points along the whole erupting prominence because for these points we found a solution for the kinetic temperature and microturbulent velocity. For these points we ran the non-LTE code to determine best-fit models. All models with tau(0)(L alpha) <= 0.3 and tau(0)(C III) <= 0.3 were analyzed further, for which we computed the integrated intensity of the C III line using a two-level atom. The best agreement between computed and observed integrated intensity led to 30 optically thin points along the prominence. The results are presented as histograms of the kinetic temperature, microturbulent velocity, effective thickness, radial flow velocity, electron density, and gas pressure. We also show the relation between the microturbulence and kinetic temperature together with a scatter plot of computed versus observed C III integrated intensities and the ratio of the computed to observed C III integrated intensities versus kinetic temperature.n

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA16-18495S" target="_blank" >GA16-18495S: Pokročilý výzkum Slunce se satelitem IRIS</a><br>

Návaznosti

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Rok uplatnění

2017

Kód důvěrnosti údajů

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

Název periodika

Astronomy & Astrophysics

ISSN

1432-0746

e-ISSN

—

Svazek periodika

607

Číslo periodika v rámci svazku

November

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

10

Strana od-do

"A80/1"-"A80/10"

Kód UT WoS článku

000415762800001

EID výsledku v databázi Scopus

2-s2.0-85034787071