Fundamental Parameters of the Eclipsing Binary DD CMa and Evidence for Mass Exchange

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00549021" target="_blank" >RIV/67985815:_____/21:00549021 - isvavai.cz</a>

Výsledek na webu

<a href="https://doi.org/10.3847/1538-3881/abded0" target="_blank" >https://doi.org/10.3847/1538-3881/abded0</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/1538-3881/abded0" target="_blank" >10.3847/1538-3881/abded0</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Fundamental Parameters of the Eclipsing Binary DD CMa and Evidence for Mass Exchange

Popis výsledku v původním jazyce

We present a detailed photometric and spectroscopic analysis of DD CMa, based on published survey photometry and new spectroscopic data. We find an improved orbital period of P-o = 2.0084530(6) days. Our spectra reveal H beta and H alpha absorptions with weak emission shoulders, and we also find a color excess in the Wide-field Infrared Survey Explorer multiband photometry, interpreted as signatures of circumstellar matter. We model the V-band orbital light curve derived from the ASAS and ASAS-SN surveys, assuming a semidetached configuration and using the mass ratio and temperature of the hotter star derived from our spectroscopic analysis. Our model indicates that the system consists of a B2.5 dwarf and a B9 giant of radii 3.2 and 3.7 R, respectively, orbiting in a circular orbit of radius 6.75 R. We also found M-c = 1.7 0.1 M, T-c = 11,350 100 K, and M-h = 6.4 0.1 M, T-h = 20,000 500 K, for the cooler and hotter star, respectively. We find broad single emission peaks in H alpha and H beta after subtracting the synthetic stellar spectra. Our results are consistent with mass exchange between the stars and suggest the existence of a stream of gas being accreted onto the early B-type star.

Název v anglickém jazyce

Fundamental Parameters of the Eclipsing Binary DD CMa and Evidence for Mass Exchange

Popis výsledku anglicky

We present a detailed photometric and spectroscopic analysis of DD CMa, based on published survey photometry and new spectroscopic data. We find an improved orbital period of P-o = 2.0084530(6) days. Our spectra reveal H beta and H alpha absorptions with weak emission shoulders, and we also find a color excess in the Wide-field Infrared Survey Explorer multiband photometry, interpreted as signatures of circumstellar matter. We model the V-band orbital light curve derived from the ASAS and ASAS-SN surveys, assuming a semidetached configuration and using the mass ratio and temperature of the hotter star derived from our spectroscopic analysis. Our model indicates that the system consists of a B2.5 dwarf and a B9 giant of radii 3.2 and 3.7 R, respectively, orbiting in a circular orbit of radius 6.75 R. We also found M-c = 1.7 0.1 M, T-c = 11,350 100 K, and M-h = 6.4 0.1 M, T-h = 20,000 500 K, for the cooler and hotter star, respectively. We find broad single emission peaks in H alpha and H beta after subtracting the synthetic stellar spectra. Our results are consistent with mass exchange between the stars and suggest the existence of a stream of gas being accreted onto the early B-type star.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

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

Astronomical Journal

ISSN

0004-6256

e-ISSN

1538-3881

Svazek periodika

161

Číslo periodika v rámci svazku

4

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

12

Strana od-do

165

Kód UT WoS článku

000626615600001

EID výsledku v databázi Scopus

2-s2.0-85102471548