HD 165246: an early-type binary with a low mass ratio

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F13%3A10174137" target="_blank" >RIV/00216208:11320/13:10174137 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1051/0004-6361/201220388" target="_blank" >http://dx.doi.org/10.1051/0004-6361/201220388</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/201220388" target="_blank" >10.1051/0004-6361/201220388</a>

Jazyk výsledku

angličtina

Název v původním jazyce

HD 165246: an early-type binary with a low mass ratio

Popis výsledku v původním jazyce

Analyses of 13 FEROS spectra from the ESO archive and 617 V-band photometric observations from the ASAS3 database allowed us to demonstrate that HD 165246 is a double-lined spectroscopic binary. As an earlier finding revealed, HD 165246 is also an eclipsing system. We were able to derive consistent orbital and light-curve solutions and all basic physical properties of the system. The period of this O8V + B7V binary is 4(d).592706 and the semiamplitudes of the radial-velocity curves are K-1 = 55.5 km s(-1) and K-2 = 321 km s(-1). As the mass ratio is small (0.173), the secondary lines cannot be seen directly in the spectra; however the application of spectral disentangling allowed us to detect weak Balmer and He I lines of the secondary component. The primary component rotates with a high projected velocity of v sin i = 243 km s(-1). A combined radial-velocity and light-curve solution led to the component masses and radii expected for the young stars of the given spectral types. Due to

Název v anglickém jazyce

HD 165246: an early-type binary with a low mass ratio

Popis výsledku anglicky

Analyses of 13 FEROS spectra from the ESO archive and 617 V-band photometric observations from the ASAS3 database allowed us to demonstrate that HD 165246 is a double-lined spectroscopic binary. As an earlier finding revealed, HD 165246 is also an eclipsing system. We were able to derive consistent orbital and light-curve solutions and all basic physical properties of the system. The period of this O8V + B7V binary is 4(d).592706 and the semiamplitudes of the radial-velocity curves are K-1 = 55.5 km s(-1) and K-2 = 321 km s(-1). As the mass ratio is small (0.173), the secondary lines cannot be seen directly in the spectra; however the application of spectral disentangling allowed us to detect weak Balmer and He I lines of the secondary component. The primary component rotates with a high projected velocity of v sin i = 243 km s(-1). A combined radial-velocity and light-curve solution led to the component masses and radii expected for the young stars of the given spectral types. Due to

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/GAP209%2F10%2F0715" target="_blank" >GAP209/10/0715: Přesné fyzikální vlastnosti horkých hvězd získané studiem dvojhvězd a vícenásobných soustav</a><br>

Návaznosti

Z - Vyzkumny zamer (s odkazem do CEZ)

Rok uplatnění

2013

Kód důvěrnosti údajů

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

Název periodika

Astronomy and Astrophysics

ISSN

0004-6361

e-ISSN

—

Svazek periodika

550

Číslo periodika v rámci svazku

únor

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

7

Strana od-do

—

Kód UT WoS článku

000314879700002

EID výsledku v databázi Scopus

—