Balmer continuum enhancement detected in a mini flare observed with IRIS

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00548090" target="_blank" >RIV/67985815:_____/21:00548090 - isvavai.cz</a>

Výsledek na webu

<a href="http://hdl.handle.net/11104/0324205" target="_blank" >http://hdl.handle.net/11104/0324205</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202141172" target="_blank" >10.1051/0004-6361/202141172</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Balmer continuum enhancement detected in a mini flare observed with IRIS

Popis výsledku v původním jazyce

The aim of the paper is to distinguish between these two mechanisms for the excess of the Balmer continuum observed in a flare. The favorable argument of a relation between the Balmer continuum excess and the HXR emission is that there is a good time coincidence between them. In addition, the shape of the maximum brightness in the 2832 SJIs, which is mainly due to this Balmer continuum excess, is similar to that of the Fermi/GBM light curve. The electron-beam flux estimated from Fermi/GBM between 10(9) and 10(10) erg s(-1) cm(-2) is consistent with the beam flux required in non-LTE radiative transfer models to obtain the excess of Balmer continuum emission observed in this IRIS spectra. Conclusions. The low-energy input by nonthermal electrons above 20 keV is sufficient to produce the enhancement in the Balmer continuum emission. This could be explained by the topology of the reconnection site. The reconnection starts in a tiny bald-patch region, which is transformed dynamically into an X-point current sheet. The size of the interacting region would be below the spatial resolution of the instrument.

Název v anglickém jazyce

Balmer continuum enhancement detected in a mini flare observed with IRIS

Popis výsledku anglicky

The aim of the paper is to distinguish between these two mechanisms for the excess of the Balmer continuum observed in a flare. The favorable argument of a relation between the Balmer continuum excess and the HXR emission is that there is a good time coincidence between them. In addition, the shape of the maximum brightness in the 2832 SJIs, which is mainly due to this Balmer continuum excess, is similar to that of the Fermi/GBM light curve. The electron-beam flux estimated from Fermi/GBM between 10(9) and 10(10) erg s(-1) cm(-2) is consistent with the beam flux required in non-LTE radiative transfer models to obtain the excess of Balmer continuum emission observed in this IRIS spectra. Conclusions. The low-energy input by nonthermal electrons above 20 keV is sufficient to produce the enhancement in the Balmer continuum emission. This could be explained by the topology of the reconnection site. The reconnection starts in a tiny bald-patch region, which is transformed dynamically into an X-point current sheet. The size of the interacting region would be below the spatial resolution of the instrument.

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/GA19-09489S" target="_blank" >GA19-09489S: Pokročilé modelování procesů ve slunečních erupcích a jejich chromosférické emise</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2021

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

654

Číslo periodika v rámci svazku

October

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

10

Strana od-do

A31

Kód UT WoS článku

000704438300009

EID výsledku v databázi Scopus

2-s2.0-85117155620