SIMBAD references

2017MNRAS.467.1414M - Mon. Not. R. Astron. Soc., 467, 1414-1425 (2017/May-2)

The binary fraction, separation distribution and merger rate of white dwarfs from SPY.

MAOZ D. and HALLAKOUN N.

Abstract (from CDS):

From a sample of spectra of 439 white dwarfs (WDs) from the ESO-VLT Supernova-Ia Progenitor Survey (SPY), we measure the maximal changes in radial velocity (ΔRVmax) between epochs (generally two epochs, separated by up to 470 d), and model the observed ΔRVmax statistics via Monte Carlo simulations, to constrain the population characteristics of double WDs (DWDs). The DWD fraction among WDs is fbin = 0.10 ± 0.02 (1σ, random) +0.02 (systematic), in the separation range <=4 au within which the data are sensitive to binarity. Assuming the distribution of binary separation, a, is a power law, dN/da ∝ aα, at the end of the last common-envelope phase and the start of solely gravitational-wave-driven binary evolution, the constraint by the data is α = -1.3 ± 0.2 (1σ) ±0.2 (systematic). If these parameters extend to small separations, the implied Galactic WD merger rate per unit stellar mass is Rmerge = (1-80) x 10–13 yr–1 M–1 (2σ), with a likelihood-weighted mean of Rmerge = (7 ± 2) x 10–13 yr–1 M–1 (1σ). The Milky Way's specific Type Ia supernova (SN Ia) rate is likely RIa ≃ 1.1 x 10–13 yr–1 M–1 and therefore, in terms of rates, a possibly small fraction of all merging DWDs (e.g. those with massive-enough primary WDs) could suffice to produce most or all SNe Ia.

Abstract Copyright: © 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): binaries: close - binaries: spectroscopic - supernovae: general - white dwarfs - white dwarfs

VizieR on-line data: <Available at CDS (J/MNRAS/467/1414): tablea1.dat>

Simbad objects: 439

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2021.04.23-06:52:26

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