The Eclipses of the Close Binary Star BE UMa [PDF]
International Astronomical Union Colloquium, 1996 BE UMa is a close binary star, not transferring mass, with an extremely hot primary star irradiating the inner face of the cool secondary star. The light curve shows a large-amplitude, sinusoidal variation with a period of 2.29 d, and an eclipse that is centered on the minimum of the variation [1], [3].
E. Zhang +2 more
openaire +2 more sources
Adiabatic Mass Loss in Binary Stars. III. From the Base of the Red Giant Branch to the Tip of the Asymptotic Giant Branch [PDF]
Astrophysical Journal, 2020 The distinguishing feature of the evolution of close binary stars is the role played by the mass exchange between the component stars. Whether or not the mass transfer is dynamically stable is one of the essential questions in binary evolution.
H. Ge +3 more
semanticscholar +1 more source
Merger Conditions of Population III Protostar Binaries
The Astrophysical Journal, 2023 Massive close binary stars with extremely small separations have been observed, and they are possible progenitors of gravitational-wave sources. The evolution of massive binaries in the protostellar accretion stage is key to understanding their formation
Takanobu Kirihara +3 more
doaj +1 more source
A radial velocity survey for post-common-envelope Wolf–Rayet central stars of planetary nebulae: first results and discovery of the close binary nucleus of NGC 5189 [PDF]
, 2015 The formation of Wolf-Rayet central stars of planetary nebulae ([WR] CSPNe) whose spectroscopic appearance mimics massive WR stars remains poorly understood. Least understood is the nature and frequency of binary companions to [WR] CSPNe that may explain
R. Manick, B. Miszalski, V. McBride
semanticscholar +1 more source
Tidally trapped pulsations in binary stars [PDF]
Monthly notices of the Royal Astronomical Society, 2020 A new class of pulsating binary stars was recently discovered, whose pulsation amplitudes are strongly modulated with orbital phase. Stars in close binaries are tidally distorted, so we examine how a star’s tidally induced asphericity affects its ...
J. Fuller +4 more
semanticscholar +1 more source
Orbital Decay in an Accreting and Eclipsing 13.7 Minute Orbital Period Binary with a Luminous Donor
The Astrophysical Journal Letters, 2023 We report the discovery of ZTF J0127+5258, a compact mass-transferring binary with an orbital period of 13.7 minutes. The system contains a white dwarf accretor, which likely originated as a post–common envelope carbon–oxygen (CO) white dwarf, and a warm
Kevin B. Burdge +26 more
doaj +1 more source
Hypervelocity stars from young stellar clusters in the Galactic Centre [PDF]
, 2017 The enormous velocities of the so called hypervelocity stars (HVSs) derive, likely, from close interactions with massive black holes, binary stars encounters or supernova explosions.
Capuzzo-Dolcetta, Roberto +2 more
core +2 more sources
The fate of close encounters between binary stars and binary supermassive black holes [PDF]
, 2017 The evolution of main sequence binaries that reside in the Galactic Centre can be heavily influenced by the central supermassive black hole (SMBH). Due to these perturbative effects, the stellar binaries in dense environments are likely to experience ...
Yihan Wang +3 more
semanticscholar +1 more source
Most EL CVn systems are inner binaries of hierarchical triples [PDF]
, 2020 In spite of their importance for modern astronomy, we do not fully understand how close binary stars containing at least one white dwarf form from main sequence binary stars. The discovery of EL CVn binaries, close pre-white dwarfs with A/F main sequence star companions, offers now the unique possibility to test models of close compact binary star ...
arxiv +1 more source
Identifying close binary central stars of PN with Kepler [PDF]
, 2015 Six planetary nebulae (PN) are known in the Kepler space telescope field of view, three newly identified. Of the 5 central stars of PN with useful Kepler data, one, J193110888+4324577, is a short-period, post common envelope binary exhibiting ...
O. Marco +7 more
semanticscholar +1 more source