The origin of low-mass white dwarfs

Rebassa‐Mansergas, A.; Schreiber, M. R.; Gänsicke, B. T.; Gómez‐Morán, A. Nebot; Girven, J.

doi:10.1063/1.3527818

Cited by 70 publications

(206 citation statements)

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“…This research has been funded by MINECO grant AYA2014-59084-P, by the AGAUR, by the European Research Council under the European Union's Seventh Framework Programme (FP/2007(FP/ -2013 , ApJ, 190, 275 Ferrario L., 2012, MNRAS, 426, 2500 Gentile Fusillo N. P., Gänsicke B. T., Greiss S., 2015, MNRAS, 448, 2260Green R. F., Richstone D. O., Schmidt M., 1978, ApJ, 224, 892 Hermes J. J. et al, 2015, MNRAS, 451, 1701 Hewett P. C., Warren S. J., Leggett S. K., Hodgkin S. T., 2006, MNRAS, 367, 454 Kepler S. O. et al, 2015, MNRAS, 446, 4078 Kepler S. O. et al, 2016 Kilic M., Brown W. R., Gianninas A., Hermes J. J., Allende Prieto C., , MNRAS, 429, 256 Parsons S. G. et al, 2014, MNRAS, 438, L91 Parsons S. G. et al, 2015, MNRAS, 449, 2194Pyrzas S. et al, 2009, MNRAS, 394, 978 Pyrzas S. et al, 2012, MNRAS, 419, 817 Raghavan D. et al, 2010 Rebassa-Mansergas A., Gänsicke B. T., Rodríguez-Gil P., Schreiber M. R., Koester D., 2007, MNRAS, 382, 1377Rebassa-Mansergas A. et al, 2008, MNRAS, 390, 1635 Rebassa-Mansergas A., Gänsicke B. T., Schreiber M. R., Koester D., Rodríguez-Gil P., 2010, MNRAS, 402, 620 Rebassa-Mansergas A., Nebot Gómez-Morán A., Schreiber M. R., Girven J., Gänsicke B. T., 2011, MNRAS, 413, 1121 Rebassa-Mansergas A., Nebot Gómez-Morán A., Schreiber M. R., Gänsicke B. T., Schwope A., Gallardo J., Koester D., 2012a, MNRAS, 419, 806 Rebassa-Mansergas A. et al, 2012b Rebassa-Mansergas A., Schreiber M. R., Gänsicke B. T. , A&A, 419, 1057Yanny B. et al, 2009, AJ, 137, 4377 York D. G. et al, 2000, AJ, 120, 1579Yuan H.-B. et al, 2015a Yuan H., Liu X., Xiang M., Huang Y., Chen B., Wu Y., Hou Y., Zhang Y., 2015b, ApJ, 799, 135 Zorotovic M., Schreiber M. R., 2013, A&A, 549, A95 Zorotovic M., Schreiber M. R., Gänsicke B. T., Nebot Gómez-Morán A., 2010, A&A, 520, A86 Zorotovic M. et al, 2011a, A&A, 536, L3 Zorotovic M., Schreiber M. R., Gänsicke B. T., 2011b, A&A, 536, A42 Zorotovic M., Schreiber M. R., García-Berro E., Camacho J., Torres S., Rebassa-Mansergas A., Gänsicke B. T., 2014, A&A, 568, A68…”

Section: Ac K N Ow L E D G E M E N T Smentioning

confidence: 99%

“…These include for example: constraining current theories of close compact binary evolution (Davis, Kolb & Willems 2010;Zorotovic et al 2010Zorotovic et al , 2011aRebassa-Mansergas et al 2012b); demonstrating in a robust way that the majority of low-mass white dwarfs are formed in binaries (Rebassa-Mansergas et al 2011); constraining the pairing properties of main-sequence stars (Ferrario 2012); providing robust observational evidence for disrupted magnetic braking ; constraining the rotationage-activity relation of low-mass main-sequence stars (RebassaMansergas, Schreiber & Gänsicke 2013a); studying the statistical properties of the PCEB population using Monte Carlo techniques (Toonen & Nelemans 2013;Camacho et al 2014;Zorotovic et al 2014); analysing why the average mass of white dwarfs in cataclysmic variables is significantly larger than the average mass of single white dwarfs (Zorotovic, Schreiber & Gänsicke 2011b;Nelemans et al 2016;Schreiber, Zorotovic & Wijnen 2016); testing hierarchical probabilistic models used to infer properties of unseen companions to low-mass white dwarfs (Andrews, Price-Whelan & Agüeros 2014); detecting new gravitational wave verification sources (Kilic et al 2014); analysing the interior structural effects of common envelope evolution on low-mass pulsating white dwarfs (Hermes et al 2015). In addition, many eclipsing SDSS PCEBs have been identified (Nebot Gómez-Morán et al 2009;Pyrzas et al 2009Pyrzas et al , 2012Parsons et al 2013Parsons et al , 2015 which are being used to test theoretical mass-radius relations of both white dwarfs and lowmass main-sequence stars (Parsons et al 2012b,a), as well as the existence of circumbinary planets (Zorotovic & Schreiber 2013;Marsh et al 2014;Parsons et al 2014).…”

Section: The Sdss Wdms Binary Cataloguementioning

confidence: 99%

See 1 more Smart Citation

The SDSS spectroscopic catalogue of white dwarf-main-sequence binaries: new identifications from DR 9–12

Rebassa‐Mansergas

Ren

Parsons

et al. 2016

Mon. Not. R. Astron. Soc.

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We present an updated version of the spectroscopic catalogue of white dwarf-main-sequence (WDMS) binaries from the Sloan Digital Sky Survey (SDSS). We identify 938 WDMS binaries within the data releases (DR) 9-12 of SDSS plus 40 objects from DR 1-8 that we missed in our previous works, 646 of which are new. The total number of spectroscopic SDSS WDMS binaries increases to 3294. This is by far the largest and most homogeneous sample of compact binaries currently available. We use a decomposition/fitting routine to derive the stellar parameters of all systems identified here (white dwarf effective temperatures, surface gravities and masses, and secondary star spectral types). The analysis of the corresponding stellar parameter distributions shows that the SDSS WDMS binary population is seriously affected by selection effects. We also measure the Na I λλ 8183.27, 8194.81 absorption doublet and H α emission radial velocities (RV) from all SDSS WDMS binary spectra identified in this work. 98 objects are found to display RV variations, 62 of which are new. The RV data are sufficient enough to estimate the orbital periods of three close binaries.Key words: binaries: close -binaries: spectroscopic -stars: low-mass -white dwarfs. I N T RO D U C T I O NA large fraction of main-sequence stars are found in binary systems (Duquennoy & Mayor 1991;Raghavan et al. 2010;Yuan et al. 2015b). It is expected that ∼25 per cent of all main-sequence binaries are close enough to begin mass transfer interactions when the more massive star becomes a red giant or an asymptotic giant star (Willems & Kolb 2004). This has been observationally verified e.g. by Farihi, Hoard & Wachter (2010) and by Nebot . Because the mass transfer rate generally exceeds the Eddington limit, the secondary star is not able to accrete the transferred material and the system evolves through a common envelope phase. That is, the core of the giant and the main-sequence companion orbit within a common envelope formed by the outer layers of the giant star. Drag forces between the two stars and the envelope lead to the shrinkage of the orbit and therefore to the release E-mail: alberto.rebassa@upc.edu of orbital energy. The orbital energy is deposited into the envelope and is eventually used to eject it (Webbink 2008). The outcome of common envelope evolution is hence a close binary formed by the core of the giant star (which later becomes a white dwarf) and a main-sequence companion, i.e. a close white dwarf-main-sequence (WDMS) binary. These are commonly referred to as post-common envelope binaries (PCEBs). The remaining ∼75 per cent of mainsequence binaries are wide enough to avoid mass transfer interactions. In these cases the more massive stars evolve like single stars until they eventually become white dwarfs. The orbital separations of such WDMS binaries are similar to those of the main-sequence binaries from which they descend.During the last years we have mined the Sloan Digital Sky Survey (SDSS; York et al. 2000) spectroscopic data base to build up th...

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Section: Ac K N Ow L E D G E M E N T Smentioning

confidence: 99%

Section: The Sdss Wdms Binary Cataloguementioning

confidence: 99%

The SDSS spectroscopic catalogue of white dwarf-main-sequence binaries: new identifications from DR 9–12

Rebassa‐Mansergas

Ren

Parsons

et al. 2016

Mon. Not. R. Astron. Soc.

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“…We were exclusively interested in the sharp Na I absorption doublet at rest wavelengths of 8183.27 and 8194.81 Å (e.g. Rebassa-Mansergas et al 2012b). Further details describing our reduction and analysis methods for the VLT data can be found in Schreiber et al (2008).…”

Section: Spectroscopic Observationsmentioning

confidence: 99%

Insights into internal effects of common-envelope evolution using the extended Kepler mission

Hermes

Gänsicke

Kim

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the binary and physical parameters of a unique pulsating white dwarf with a main-sequence companion, SDSS J1136+0409, observed for more than 77 d during the first pointing of the extended Kepler mission: K2 Campaign 1. Using new groundbased spectroscopy, we show that this post-common-envelope binary has an orbital period of 6.89760103(60) h, which is also seen in the photometry as a result of Doppler beaming and ellipsoidal variations of the secondary. We spectroscopically refine the temperature of the white dwarf to 12 330 ± 260 K and its mass to 0.601 ± 0.036 M . We detect seven independent pulsation modes in the K2 light curve. A preliminary asteroseismic solution is in reasonable agreement with the spectroscopic atmospheric parameters. Three of the pulsation modes are clearly rotationally split multiplets, which we use to demonstrate that the white dwarf is not synchronously rotating with the orbital period but has a rotation period of 2.49 ± 0.53 h. This is faster than any known isolated white dwarf, but slower than almost all white dwarfs measured in non-magnetic cataclysmic variables, the likely future state of this binary.

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“…We made use of these spectra to measure the radial velocities of our WD+FGK binaries as follows (the radial velocities are provided in Table 3). We followed the method described by Rebassa-Mansergas et al (2008) and Ren et al (2013) to fit the Na I doublet at ∼5,800Å arising from all spectra obtained from our INT, SPM, CFHT and TNT observations ( Table 2). To that end we used a combination of a second order polynomial and a double-Gaussian profile.…”

Section: Radial Velocitiesmentioning

confidence: 99%

The white dwarf binary pathways survey – II. Radial velocities of 1453 FGK stars with white dwarf companions from LAMOST DR 4

Rebassa‐Mansergas¹,

Ren²,

Irawati³

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the second paper of a series of publications aiming at obtaining a better understanding regarding the nature of type Ia supernovae (SN Ia) progenitors by studying a large sample of detached F, G and K main sequence stars in close orbits with white dwarf companions (i.e. WD+FGK binaries). We employ the LAMOST (Large Sky Area Multi-Object Fibre Spectroscopic Telescope) data release 4 spectroscopic data base together with GALEX (Galaxy Evolution Explorer) ultraviolet fluxes to identify 1,549 WD+FGK binary candidates (1,057 of which are new), thus doubling the number of known sources. We measure the radial velocities of 1,453 of these binaries from the available LAMOST spectra and/or from spectra obtained by us at a wide variety of different telescopes around the globe. The analysis of the radial velocity data allows us to identify 24 systems displaying more than 3σ radial velocity variation that we classify as close binaries. We also discuss the fraction of close binaries among WD+FGK systems, which we find to be ∼10 per cent, and demonstrate that high-resolution spectroscopy is required to efficiently identify double-degenerate SN Ia progenitor candidates.

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The origin of low-mass white dwarfs

Cited by 70 publications

References 0 publications

The SDSS spectroscopic catalogue of white dwarf-main-sequence binaries: new identifications from DR 9–12

The SDSS spectroscopic catalogue of white dwarf-main-sequence binaries: new identifications from DR 9–12

Insights into internal effects of common-envelope evolution using the extended Kepler mission

The white dwarf binary pathways survey – II. Radial velocities of 1453 FGK stars with white dwarf companions from LAMOST DR 4

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