Wray 15-906: a candidate luminous blue variable discovered with WISE, Herschel, and SALT

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F20%3A00538328" target="_blank" >RIV/67985815:_____/20:00538328 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.1093/mnras/staa2659" target="_blank" >https://doi.org/10.1093/mnras/staa2659</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/staa2659" target="_blank" >10.1093/mnras/staa2659</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Wray 15-906: a candidate luminous blue variable discovered with WISE, Herschel, and SALT

Popis výsledku v původním jazyce

We present the results of study of the Galactic candidate luminous blue variable Wray 15-906, revealed via detection of its infrared circumstellar shell (of approximate to 2 pc in diameter) with the Wide-field Infrared Survey Explorer and the Herschel Space Observatory. Using the stellar atmosphere code CMFGEN and the Gaia parallax, we found that Wray 15-906 is a relatively low-luminosity, log(L/L-circle dot) approximate to 5.4, star of temperature of 25 +/- 2 kK, with a mass-loss rate of approximate to 3 x 10(-5) M-circle dot yr(-1), a wind velocity of 280 +/- 50 km s(-1), and a surface helium abundance of 65 +/- 2 per cent (by mass). In the framework of single-star evolution, the obtained results suggest that Wray 15-906 is a post-red supergiant star with initial mass of approximate to 25 M-circle dot and that before exploding as a supernova it could transform for a short time into a WN11h star. Our spectroscopic monitoring with the Southern African Large Telescope does not reveal significant changes in the spectrum of Wray 15-906 during the last 8 yr, while the V-band light curve of this star over years 1999-2019 shows quasi-periodic variability with a period of approximate to 1700 d and an amplitude of approximate to 0.2 mag. We estimated the mass of the shell to be 2.9 +/- 0.5 M-circle dot assuming the gas-to-dust mass ratio of 200. The presence of such a shell indicates that Wray 15-906 has suffered substantial mass-loss in the recent past. We found that the open star cluster C1128-631 could be the birth place of Wray 15-906 provided that this star is a rejuvenated product of binary evolution (a blue straggler).

Název v anglickém jazyce

Wray 15-906: a candidate luminous blue variable discovered with WISE, Herschel, and SALT

Popis výsledku anglicky

We present the results of study of the Galactic candidate luminous blue variable Wray 15-906, revealed via detection of its infrared circumstellar shell (of approximate to 2 pc in diameter) with the Wide-field Infrared Survey Explorer and the Herschel Space Observatory. Using the stellar atmosphere code CMFGEN and the Gaia parallax, we found that Wray 15-906 is a relatively low-luminosity, log(L/L-circle dot) approximate to 5.4, star of temperature of 25 +/- 2 kK, with a mass-loss rate of approximate to 3 x 10(-5) M-circle dot yr(-1), a wind velocity of 280 +/- 50 km s(-1), and a surface helium abundance of 65 +/- 2 per cent (by mass). In the framework of single-star evolution, the obtained results suggest that Wray 15-906 is a post-red supergiant star with initial mass of approximate to 25 M-circle dot and that before exploding as a supernova it could transform for a short time into a WN11h star. Our spectroscopic monitoring with the Southern African Large Telescope does not reveal significant changes in the spectrum of Wray 15-906 during the last 8 yr, while the V-band light curve of this star over years 1999-2019 shows quasi-periodic variability with a period of approximate to 1700 d and an amplitude of approximate to 0.2 mag. We estimated the mass of the shell to be 2.9 +/- 0.5 M-circle dot assuming the gas-to-dust mass ratio of 200. The presence of such a shell indicates that Wray 15-906 has suffered substantial mass-loss in the recent past. We found that the open star cluster C1128-631 could be the birth place of Wray 15-906 provided that this star is a rejuvenated product of binary evolution (a blue straggler).

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

2020

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

1365-2966

e-ISSN

—

Svazek periodika

498

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

16

Strana od-do

5093-5108

Kód UT WoS článku

000587755500034

EID výsledku v databázi Scopus

2-s2.0-85097157391