Early optical follow-up of the nearby active star DG CVn during its 2014 superflare

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F68378271%3A_____%2F15%3A00449052" target="_blank" >RIV/68378271:_____/15:00449052 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/67985815:_____/15:00449052 RIV/68407700:21230/15:00231681

Výsledek na webu

<a href="http://dx.doi.org/10.1093/mnras/stv1565" target="_blank" >http://dx.doi.org/10.1093/mnras/stv1565</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stv1565" target="_blank" >10.1093/mnras/stv1565</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Early optical follow-up of the nearby active star DG CVn during its 2014 superflare

Popis výsledku v původním jazyce

DG Canum Venaticorum (DG CVn) is a binary system in which one of the components is an M-type dwarf ultrafast rotator, only three of which are known in the solar neighbourhood. Observations of DG CVn by the Swift satellite and several ground-based observatories during its superflare event on 2014 allowed us to perform a complete hard X-ray-optical follow-up of a superflare from the red-dwarf star. The observations support the fact that the superflare can be explained by the presence of (a) large active region(s) on the surface of the star. Such activity is similar to the most extreme solar flaring events. This points towards a plausible extrapolation between the behaviour from the most active red-dwarf stars and the processes occurring in the Sun.

Název v anglickém jazyce

Early optical follow-up of the nearby active star DG CVn during its 2014 superflare

Popis výsledku anglicky

DG Canum Venaticorum (DG CVn) is a binary system in which one of the components is an M-type dwarf ultrafast rotator, only three of which are known in the solar neighbourhood. Observations of DG CVn by the Swift satellite and several ground-based observatories during its superflare event on 2014 allowed us to perform a complete hard X-ray-optical follow-up of a superflare from the red-dwarf star. The observations support the fact that the superflare can be explained by the presence of (a) large active region(s) on the surface of the star. Such activity is similar to the most extreme solar flaring events. This points towards a plausible extrapolation between the behaviour from the most active red-dwarf stars and the processes occurring in the Sun.

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

<a href="/cs/project/GA13-33324S" target="_blank" >GA13-33324S: Rentgenový monitor račí oko</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2015

Kód důvěrnosti údajů

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

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

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Svazek periodika

452

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

8

Strana od-do

4195-4202

Kód UT WoS článku

000360862100063

EID výsledku v databázi Scopus

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