Results 31 to 40 of about 31,802 (281)
Are extreme AGB stars post-common envelope binaries?
, 2020 Accepted for publication in MNRAS ...
Dell'Agli, F. +8 more
openaire +2 more sources
The post-common-envelope binary central star of the planetary nebula PN G283.7-05.1 [PDF]
Astronomy & Astrophysics, 2020 We present the discovery and characterisation of the post-common-envelope central star system in the planetary nebula PN G283.7−05.1. Deep images taken as part of the POPIPlaN survey indicate that the nebula may possess a bipolar morphology similar to other post-common-envelope planetary nebulae.
Jones, D +10 more
openaire +4 more sources
On the Detectability of Post-common-envelope Binary Central Stars of Planetary Nebulae
Research Notes of the AAS, 2022 Abstract Common envelope evolution is widely accepted as the principal shaping agent in the formation of aspherical planetary nebulae. However, only some 20% of planetary nebulae are found to host post-common-envelope binary central stars.
George Hume, Paige Yarker, David Jones
openaire +1 more source
Criteria for Dynamical Timescale Mass Transfer of Metal-poor Intermediate-mass Stars
The Astrophysical Journal, 2023 The stability criteria of rapid mass transfer and common-envelope evolution are fundamental in binary star evolution. They determine the mass, mass ratio, and orbital distribution of many important systems, such as X-ray binaries, type Ia supernovae, and
Hongwei Ge +5 more
doaj +1 more source
Planetary Nebulae Embryo after a Common Envelope Event
Galaxies, 2018 In the centers of some planetary nebulae are found close binary stars. The formation of those planetary nebulae was likely through a common envelope event, which transformed an initially-wide progenitor binary into the currently observed close binary ...
Natalia Ivanova, Jose L. A. Nandez
doaj +1 more source
Post–Common-Envelope Binary Stars and the Precataclysmic Binary PG 1114+187
The Astronomical Journal, 2000 We present orbit-resolved spectroscopy and orbit-sampled photometry of the binary system PG 1114+187. Both photometry and radial velocity studies reveal a period P = 1.75992 days, which is taken to be the orbital period of the binary. Strong modulation of emission-line strength with the same period is also present. A preliminary mass ratio, M2/M1 ≈ 0.7,
Todd C. Hillwig +2 more
openaire +1 more source
Masses and envelope binding energies of primary stars at the onset of a common envelope [PDF]
, 2010 We present basic properties of primary stars that initiate a common envelope (CE) in a binary, while on the giant branch. We use the population-synthesis code described in Politano et al. (2010) and follow the evolution of a population of binary stars up
Politano, Michael +2 more
core +2 more sources
The Astrophysical Journal, 2023 Abstract The formation histories of compact binary mergers, especially stellar-mass binary black hole mergers, have recently come under increased scrutiny and revision. We revisit the question of the dominant formation channel and efficiency of forming binary neutron star (BNS) mergers.
Monica Gallegos-Garcia +2 more
openaire +3 more sources
Cataclysmic Variables and a New Class of Faint UV Stars in the Globular Cluster NGC 6397 [PDF]
, 1998 We present evidence that the globular cluster NGC 6397 contains two distinct classes of centrally-concentrated UV-bright stars. Color-magnitude diagrams constructed from U, B, V, and I data obtained with the HST/WFPC2 reveal seven UV-bright stars fainter
Adrienne M. Cool +8 more
core +3 more sources
The Evolution of Population III and Extremely Metal-poor Binary Stars
The Astrophysical Journal, 2023 Numerical simulations have now shown that Population III (Pop III) stars can form in binaries and small clusters and that these stars can be in close proximity to each other.
Sung-Han Tsai +4 more
doaj +1 more source