The low-mass interacting binary system OO Aql revisited: a new quadruple system

Abstract

In this study we present photometric and spectroscopic variation analysis and orbital period study of a low-mass interacting system OO Aql. Simultaneous solution of the light and radial velocity curves provide us a determination of new set of stellar physical parameters for the primary and the secondary companion as M${}_1$ = 1.05(2) M${}_{\odot }$, M${}_2$ = 0.89(2) M${}_{\odot }$, R${}_1$ = 1.38(2) R${}_{\odot }$, R${}_2$ = 1.28(2) R${}_{\odot }$, $\log (L_1/L_{\odot })=0.258$ and $\log (L_2/L_{\odot })=0.117$ and the separation of the components were determined a = 3.333(16) R${}_{\odot }$. Newly obtained parameters yield the distance of the system as 136(8) pc. Analyses of the mid-eclipse times indicate a period increase of $\frac{P}{\dot{P}}=4\times 10^7$ yr that can be interpreted in terms of the mass transfer $\frac{dM}{dt}=5\times 10^{-8}$ M${}_{\odot }$/yr from the less massive component to the more massive component. Our new solution confirmed that OO Aql is a multiple system in the form of AB + C + D. We found initial astrophysical parameters for the component of the system and its current age to be 8.6 Gyr using nonconservative stellar evolution model (EV-TWIN code).

Accepted for publication in the Astronomical Journal (10 pages, including 3 figures and 4 tables)

References in corpus (2)

• Radial Velocity Studies of Close Binary Stars. XII
• Absolute properties of the binary system BB Pegasi

Cited by in corpus (3)

• Physical parameters of close binary systems: VIII
• The First Photometric and Spectroscopic Study of Contact Binary V2840 Cygni
• The multiple nature of CC Com: one of the ultra-short orbital period late-type contact binary systems