Doppler-velocity Drifts Detected in a Solar Prominence

Kód výsledku v IS VaVaI

RIV/67985815:_____/22:00559602 - isvavai.cz

Výsledek na webu

https://hdl.handle.net/11104/0333350

DOI - Digital Object Identifier

10.3847/1538-4357/ac778a

Jazyk výsledku

angličtina

Název v původním jazyce

Doppler-velocity Drifts Detected in a Solar Prominence

Popis výsledku v původním jazyce

We analyzed multiline observations of a quiescent prominence from the slit spectrograph located at the Ondrejov Observatory. Dopplergrams and integrated intensity maps of the whole prominence were obtained from observations in six spectral lines: Ca ii H, H epsilon, H beta, He i D3, H alpha, and Ca ii IR. By combining integrated intensity maps with non-LTE radiative-transfer modeling, we carefully identified areas in an optically thin regime. The comparison of the Doppler-velocity maps and scatterplots from different lines shows the existence of differences in the velocity of ions and neutrals called velocity drift. The drift is of a local nature, present mostly at prominence edges in the area with a large velocity gradient, as can be tentatively expected based on multifluid MHD models. We could not explore the time evolution of the drift, since our data set consists of a single scan only. Our paper brings another contribution to a rather controversial problem of the detection of multifluid effects in solar prominences.

Název v anglickém jazyce

Doppler-velocity Drifts Detected in a Solar Prominence

Popis výsledku anglicky

We analyzed multiline observations of a quiescent prominence from the slit spectrograph located at the Ondrejov Observatory. Dopplergrams and integrated intensity maps of the whole prominence were obtained from observations in six spectral lines: Ca ii H, H epsilon, H beta, He i D3, H alpha, and Ca ii IR. By combining integrated intensity maps with non-LTE radiative-transfer modeling, we carefully identified areas in an optically thin regime. The comparison of the Doppler-velocity maps and scatterplots from different lines shows the existence of differences in the velocity of ions and neutrals called velocity drift. The drift is of a local nature, present mostly at prominence edges in the area with a large velocity gradient, as can be tentatively expected based on multifluid MHD models. We could not explore the time evolution of the drift, since our data set consists of a single scan only. Our paper brings another contribution to a rather controversial problem of the detection of multifluid effects in solar prominences.

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

934

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

10

Strana od-do

16

Kód UT WoS článku

000828342400001

EID výsledku v databázi Scopus

2-s2.0-85135104003