Hot prominence detected in the core of a coronal mass ejection III. Plasma filling factor from UVCS Lyman-alpha and Lyman-beta observations

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F18%3A00495470" target="_blank" >RIV/67985815:_____/18:00495470 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201832792" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201832792</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201832792" target="_blank" >10.1051/0004-6361/201832792</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Hot prominence detected in the core of a coronal mass ejection III. Plasma filling factor from UVCS Lyman-alpha and Lyman-beta observations

Popis výsledku v původním jazyce

We explore two methods for measuring this factor along the line of sight. They are based on a combination of visible-light and ultraviolet spectroscopic observations. The resulting filling factors are consistent with the model in both prominence points when the radiative and collisional components of the total intensity of the hydrogen lines are separated using the Ly alpha and Ly beta line intensities, which is required to estimate the filling factor. The exploration of the parameter space shows that the results are weakly sensitive to the plasma flow velocity, but depend more strongly on the assumed kinetic temperatures. The combination of visible-light and ultraviolet Ly alpha and Ly beta data can be used to approximately estimate the line-of-sight geometrical filling factor in erupting prominences, but the proposed technique, which is model dependent, is reliable only for emission that is optically thin in the lines considered, a condition that is not in general representative of prominence plasma.

Název v anglickém jazyce

Hot prominence detected in the core of a coronal mass ejection III. Plasma filling factor from UVCS Lyman-alpha and Lyman-beta observations

Popis výsledku anglicky

We explore two methods for measuring this factor along the line of sight. They are based on a combination of visible-light and ultraviolet spectroscopic observations. The resulting filling factors are consistent with the model in both prominence points when the radiative and collisional components of the total intensity of the hydrogen lines are separated using the Ly alpha and Ly beta line intensities, which is required to estimate the filling factor. The exploration of the parameter space shows that the results are weakly sensitive to the plasma flow velocity, but depend more strongly on the assumed kinetic temperatures. The combination of visible-light and ultraviolet Ly alpha and Ly beta data can be used to approximately estimate the line-of-sight geometrical filling factor in erupting prominences, but the proposed technique, which is model dependent, is reliable only for emission that is optically thin in the lines considered, a condition that is not in general representative of prominence plasma.

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

2018

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

617

Číslo periodika v rámci svazku

September

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

9

Strana od-do

—

Kód UT WoS článku

000444605000001

EID výsledku v databázi Scopus

2-s2.0-85053543946