Population synthesis for double white dwarfs

Nelemans, G.; Yungelson, L. R.; Zwart, Simon F. Portegies; Verbunt, F.

doi:10.1051/0004-6361:20000147

Cited by 524 publications

(898 citation statements)

References 62 publications

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“…On one hand, synthetic binary models (Nelemans et al 2001;Hurley et al 2002;Izzard et al 2006;Belczynski et al 2008) merge the results of detailed single-star modelling, but fitted to formulae or tabulated for fast evaluation, with binaryevolution algorithms. While these are excellent tools to explore the binary-star parameter space in statistical studies, they still assume each star in the binary evolves like an isolated, single star.…”

Section: Introductionmentioning

confidence: 99%

BINSTAR: a new binary stellar evolution code

Siess

Izzard

Davis

et al. 2013

A&A

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We provide a detailed description of a new stellar evolution code, BINSTAR, which has been developed to study interacting binaries. Based on the stellar evolution code STAREVOL, it is specifically designed to study low-and intermediate-mass binaries. We describe the state-of-the-art input physics, which includes treatments of tidal interactions, mass transfer and angular momentum exchange within the system. A generalised Henyey method is used to solve simultaneously the stellar structure equations of each component as well as the separation and eccentricity of the orbit. Test simulations for cases A and B mass transfer are presented and compared with available models. The results of the evolution of Algol systems are in remarkable agreement with the calculations of the Vrije Universiteit Brussel (VUB) group, thus validating our code. We also computed a large grid of models for various masses (2 ≤ M/M ≤ 20) and seven metallicities (Z = 0.0001, 0.001, 0.004, 0.008, 0.01, 0.02, 0.03) to provide a useful analytical parameterisation of the tidal torque constant E 2 , which allows the determination of the circularisation and synchronisation timescales for stars with a radiative envelope and convective core. The evolution of E 2 during the main sequence shows noticeable differences compared to available models. In particular, our new calculations indicate that the circularisation timescale is constant during core hydrogen burning. We also show that E 2 weakly depends on core overshooting but is substantially increased when the metallicity becomes lower.

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Section: Introductionmentioning

confidence: 99%

BINSTAR: a new binary stellar evolution code

Siess

Izzard

Davis

et al. 2013

A&A

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“…The sdB binaries formed through stable RLOF have orbital periods ranging from 10 to 500 days, and MS companions. An alternative stable RLOF channel based on the γ-formalism is described by Nelemans et al (2000Nelemans et al ( , 2001; Nelemans (2010) and can produce sdB binaries with periods on the order of 1 − 2 years. Finally, The WD merger channel can lead to sdB stars with a higher mass, up to 0.65 M ⊙ .…”

Section: Introductionmentioning

confidence: 99%

The orbits of subdwarf-B + main-sequence binaries

Vos

Østensen

Németh

et al. 2013

A&A

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Context. The predicted orbital-period distribution of the subdwarf-B (sdB) population is bi-modal with a peak at short ( < 10 days) and long ( > 250 days) periods. Observationally, many short-period sdB systems are known, but the predicted long period peak is missing as orbits have only been determined for a few long-period systems. As these predictions are based on poorly understood binary-interaction processes, it is of prime importance to confront the predictions with reliable observational data. We therefore initiated a monitoring program to find and characterize long-period sdB stars. Aims. In this paper we aim to determine the orbital parameters of the three long-period sdB+MS binaries BD+29 • 3070, BD+34 • 1543 and Feige 87, to constrain their absolute dimensions and the physical parameters of the components. Methods. High-resolution spectroscopic time series were obtained with HERMES at the Mercator telescope on La Palma, and analyzed to determine the radial velocities of both the sdB and MS components. Photometry from the literature was used to construct the spectral-energy distribution (SED) of the binaries. Atmosphere models were used to fit these SEDs and to determine the surface gravities and temperatures of both components of all systems. Spectral analysis was used to check the results of the SEDs.Results. An orbital period of 1283 ± 63 d, a mass ratio of q = 0.39 ± 0.04 and a significant non-zero eccentricity of e = 0.15 ± 0.01 were found for BD+29 • 3070. For BD+34 • 1543 we determined P orb = 972 ± 2 d, q = 0.57 ± 0.01 and again a clear non-zero eccentricity of e = 0.16 ± 0.01. Last, for Feige 87 we found P orb = 936 ± 2 d, q = 0.55 ± 0.01 and e = 0.11 ± 0.01. Conclusions. BD+29 • 3070, BD+34 • 1543 and Feige 87 are long period sdB + MS binaries on clearly eccentric orbits. These results are in conflict with the predictions of stable Roche-lobe overflow models.

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“…Due to the quality of the data and the wavelength coverage of our spectra, we cannot rule out the presence of unseen, close white dwarf companions, suggested to be ≈25 per cent of the field population (Nelemans et al 2001), or more in old open clusters . Existing near-infrared data seem to exclude the presence of low-mass late-type companions (see next section for further discussion).…”

Section: S P E C T R a L A Na Ly S I Smentioning

confidence: 95%

A search for white dwarfs in the Galactic plane: the field and the open cluster population

Raddi¹,

Catalán²,

Gänsicke³

et al. 2016

Mon. Not. R. Astron. Soc.

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We investigated the prospects for systematic searches of white dwarfs at low Galactic latitudes, using the VLT Survey Telescope H α Photometric Survey of the Galactic plane and Bulge (VPHAS+). We targeted 17 white dwarf candidates along sightlines of known open clusters, aiming to identify potential cluster members. We confirmed all the 17 white dwarf candidates from blue/optical spectroscopy, and we suggest five of them to be likely cluster members. We estimated progenitor ages and masses for the candidate cluster members, and compare our findings to those for other cluster white dwarfs. A white dwarf in NGC 3532 is the most massive known cluster member (1.13 M ), likely with an oxygen-neon core, for which we estimate an 8.8 +1.2 −4.3 M progenitor, close to the mass-divide between white dwarf and neutron star progenitors. A cluster member in Ruprecht 131 is a magnetic white dwarf, whose progenitor mass exceeded 2-3 M . We stress that wider searches, and improved cluster distances and ages derived from data of the ESA Gaia mission, will advance the understanding of the mass-loss processes for low-to intermediate-mass stars.

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Population synthesis for double white dwarfs

Cited by 524 publications

References 62 publications

BINSTAR: a new binary stellar evolution code

BINSTAR: a new binary stellar evolution code

The orbits of subdwarf-B + main-sequence binaries

A search for white dwarfs in the Galactic plane: the field and the open cluster population

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