Time-resolved UVES observations of a stellar flare on the planet host HD 189733 during primary transit

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F17%3A00482450" target="_blank" >RIV/67985815:_____/17:00482450 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201630068" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201630068</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201630068" target="_blank" >10.1051/0004-6361/201630068</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Time-resolved UVES observations of a stellar flare on the planet host HD 189733 during primary transit

Popis výsledku v původním jazyce

HD 189733 is an exoplanetary system consisting of a transiting hot Jupiter and an active K2V-type main sequence star. Rich manifestations of a stellar activity, like photometric spots or chromospheric flares were repeatedly observed in this system in optical, UV and X-rays. Aims. We aim to use VLT/UVES high resolution (R = 60 000) echelle spectra to study a stellar flare. We determine the energy released during the flare in all studied chromospheric lines combined to be about 8.7 X 10(31) erg, which puts this event at the upper end of flare energies observed on the Sun. Our analysis does not reveal any significant delay of the flare peak observed in the Balmer and Ca II H & K lines, although we find a clear difference in the temporal evolution of these lines. The He I D3 shows additional absorption possibly related to the flare event. Based on the flux released in Ca II H & K lines during the flare, we estimate the soft X-ray flux emission to be 7 X 10(30) erg.n

Název v anglickém jazyce

Time-resolved UVES observations of a stellar flare on the planet host HD 189733 during primary transit

Popis výsledku anglicky

HD 189733 is an exoplanetary system consisting of a transiting hot Jupiter and an active K2V-type main sequence star. Rich manifestations of a stellar activity, like photometric spots or chromospheric flares were repeatedly observed in this system in optical, UV and X-rays. Aims. We aim to use VLT/UVES high resolution (R = 60 000) echelle spectra to study a stellar flare. We determine the energy released during the flare in all studied chromospheric lines combined to be about 8.7 X 10(31) erg, which puts this event at the upper end of flare energies observed on the Sun. Our analysis does not reveal any significant delay of the flare peak observed in the Balmer and Ca II H & K lines, although we find a clear difference in the temporal evolution of these lines. The He I D3 shows additional absorption possibly related to the flare event. Based on the flux released in Ca II H & K lines during the flare, we estimate the soft X-ray flux emission to be 7 X 10(30) erg.n

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

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

12

Strana od-do

"A66/1"-"A66/12"

Kód UT WoS článku

000415265200003

EID výsledku v databázi Scopus

2-s2.0-85034431475