Flare stars in nearby Galactic open clusters based on TESS data

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00548624" target="_blank" >RIV/67985815:_____/21:00548624 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/00216224:14310/21:00121490

Výsledek na webu

<a href="http://hdl.handle.net/11104/0324662" target="_blank" >http://hdl.handle.net/11104/0324662</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.31577/caosp.2021.51.1.78" target="_blank" >10.31577/caosp.2021.51.1.78</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Flare stars in nearby Galactic open clusters based on TESS data

Popis výsledku v původním jazyce

The study is devoted to search for flare stars among confirmed members of Galactic open clusters using high-cadence photometry from TESS mission. We analyzed 957 high-cadence light curves of members from 136 open clusters. As a result, 56 flare stars were found, among them 8 hot B-A type objects. Of all flares, 63 % were detected in sample of cool stars (Teff<5000 K), and 29 % -- in stars of spectral type G, while 23 % in K-type stars and approximately 34% of all detected flares are in M-type stars. Using the FLATW'RM (FLAre deTection With Ransac Method) flare finding algorithm, we estimated parameters of flares and rotation period of detected flare stars. The flare with the largest amplitude appears on the M3 type EQ Cha star. Statistical analysis did not reveal any direct correlation between ages, rotation periods and flaring activity.

Název v anglickém jazyce

Flare stars in nearby Galactic open clusters based on TESS data

Popis výsledku anglicky

The study is devoted to search for flare stars among confirmed members of Galactic open clusters using high-cadence photometry from TESS mission. We analyzed 957 high-cadence light curves of members from 136 open clusters. As a result, 56 flare stars were found, among them 8 hot B-A type objects. Of all flares, 63 % were detected in sample of cool stars (Teff<5000 K), and 29 % -- in stars of spectral type G, while 23 % in K-type stars and approximately 34% of all detected flares are in M-type stars. Using the FLATW'RM (FLAre deTection With Ransac Method) flare finding algorithm, we estimated parameters of flares and rotation period of detected flare stars. The flare with the largest amplitude appears on the M3 type EQ Cha star. Statistical analysis did not reveal any direct correlation between ages, rotation periods and flaring activity.

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/GA18-05665S" target="_blank" >GA18-05665S: Ztráta hmoty v pozdních fázích vývoje hmotných hvězd</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

Contributions of the Astronomical Observatory Skalnaté Pleso

ISSN

1335-1842

e-ISSN

1336-0337

Svazek periodika

51

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

SK - Slovenská republika

Počet stran výsledku

12

Strana od-do

78-97

Kód UT WoS článku

000614521100007

EID výsledku v databázi Scopus

2-s2.0-85101118756