Spectroscopic survey of emission-line stars - I. B[e] stars

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F16%3A00461656" target="_blank" >RIV/67985815:_____/16:00461656 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1093/mnras/stv2758" target="_blank" >http://dx.doi.org/10.1093/mnras/stv2758</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stv2758" target="_blank" >10.1093/mnras/stv2758</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Spectroscopic survey of emission-line stars - I. B[e] stars

Popis výsledku v původním jazyce

Here, we focus on a sample of nine B[e] stars in different evolutionary phases. Emission of the [OI] lines is one of the characteristics of B[e] stars. We find that four of the objects display [Ca II] line emission: for the B[e] supergiants V1478 Cyg and 3 Pup, the kinematics obtained from the [O I] and [Ca II] line profiles agrees with a Keplerian rotating disc scenario; the forbidden lines of the compact planetary nebula OY Gem display no kinematical broadening beyond spectral resolution; the luminous blue variable candidate V1429 Aql shows no [O I] lines, but the profile of its [Ca II] lines suggests that the emission originates in its hot, ionized circumbinary disc. As none of the B[e] stars of lower mass displays [Ca II] line emission, we conclude that these lines are more likely observable in massive stars with dense discs, supporting and strengthening the suggestion that their appearance requires high-density environments.

Název v anglickém jazyce

Spectroscopic survey of emission-line stars - I. B[e] stars

Popis výsledku anglicky

Here, we focus on a sample of nine B[e] stars in different evolutionary phases. Emission of the [OI] lines is one of the characteristics of B[e] stars. We find that four of the objects display [Ca II] line emission: for the B[e] supergiants V1478 Cyg and 3 Pup, the kinematics obtained from the [O I] and [Ca II] line profiles agrees with a Keplerian rotating disc scenario; the forbidden lines of the compact planetary nebula OY Gem display no kinematical broadening beyond spectral resolution; the luminous blue variable candidate V1429 Aql shows no [O I] lines, but the profile of its [Ca II] lines suggests that the emission originates in its hot, ionized circumbinary disc. As none of the B[e] stars of lower mass displays [Ca II] line emission, we conclude that these lines are more likely observable in massive stars with dense discs, supporting and strengthening the suggestion that their appearance requires high-density environments.

Druh

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

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

—

Projekt

<a href="/cs/project/GA14-21373S" target="_blank" >GA14-21373S: Odhalení historie ztráty hmoty vyvinutých masivních hvězd</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2016

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

—

Svazek periodika

456

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

14

Strana od-do

1424-1437

Kód UT WoS článku

000372264200020

EID výsledku v databázi Scopus

2-s2.0-84960830789