o Puppis: another Be plus sdO binary?

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216224%3A14310%2F12%3A00107091" target="_blank" >RIV/00216224:14310/12:00107091 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/67985815:_____/12:00388412

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201219679" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201219679</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201219679" target="_blank" >10.1051/0004-6361/201219679</a>

Jazyk výsledku

angličtina

Název v původním jazyce

o Puppis: another Be plus sdO binary?

Popis výsledku v původním jazyce

The spectrum of the Be star o Pup is shown to vary periodically with a period of 28.9 days. A radial-velocity variable He I 6678 angstrom emission component suggests that the star is the same type as phi Per, 59 Cyg, and FY CMa, i.e. binaries consisting of a Be star and a hot companion that illuminates the Be star disk (also called phi Per-type binaries or Be+sdO binaries). The range of radial-velocity variations of the stronger emission component in the helium line observed in o Pup is about 270 km s(-1), a value in good agreement with the range derived for phi Per-type binaries. The radial velocity curves defined by the prominent emission peak in He I 6678 angstrom line and H alpha + Paschen emission move in anti-phase. We suggest that o Pup is generically similar to phi Per-type systems and may represent the fourth case of a Be star with a hot subdwarf companion.

Název v anglickém jazyce

o Puppis: another Be plus sdO binary?

Popis výsledku anglicky

The spectrum of the Be star o Pup is shown to vary periodically with a period of 28.9 days. A radial-velocity variable He I 6678 angstrom emission component suggests that the star is the same type as phi Per, 59 Cyg, and FY CMa, i.e. binaries consisting of a Be star and a hot companion that illuminates the Be star disk (also called phi Per-type binaries or Be+sdO binaries). The range of radial-velocity variations of the stronger emission component in the helium line observed in o Pup is about 270 km s(-1), a value in good agreement with the range derived for phi Per-type binaries. The radial velocity curves defined by the prominent emission peak in He I 6678 angstrom line and H alpha + Paschen emission move in anti-phase. We suggest that o Pup is generically similar to phi Per-type systems and may represent the fourth case of a Be star with a hot subdwarf companion.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

S - Specificky vyzkum na vysokych skolach

Rok uplatnění

2012

Kód důvěrnosti údajů

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

Název periodika

ASTRONOMY & ASTROPHYSICS

ISSN

0004-6361

e-ISSN

—

Svazek periodika

545

Číslo periodika v rámci svazku

A121

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

4

Strana od-do

1-4

Kód UT WoS článku

000309254900121

EID výsledku v databázi Scopus

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