Testing the Initial–Final Mass Relationship of White Dwarfs

Catalán, S.; Isern, J.; Garcı́a–Berro, E.; Ribas, I.

doi:10.1007/978-3-642-11250-8_92

Cited by 113 publications

(193 citation statements)

References 92 publications

(346 reference statements)

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“…We have chosen a value of Z = 0.027 taken from Catalán et al (2008a) but our mass and age determinations do only weakly depend on the choice of metallicity: If we instead use the lowest recent value for the metallicity of Praesepe (Z = 0.019, Claver et al 2001;Casewell et al 2009) the progenitor age becomes only 1% longer, which implies the progenitor mass estimates would be 0.03 M smaller, consistent with the estimates from Casewell et al (2009).…”

Section: Wd 0836+201mentioning

confidence: 89%

“…Using their values, Catalán et al (2008a) re-estimated the mass and the progenitor mass of this object to discuss the effect of the magnetic field on IFMR. Casewell et al (2009) mentioned that the analysis with non-magnetic model spectra may lead to uncertainties in the temperature determination.…”

Section: Wd 0836+201mentioning

confidence: 99%

“…Magnetic fields, alongside angular momentum, were also proposed to be an effective factor of the mass-loss, after the discovery of a magnetic white dwarf (MWD) WD 0836+201 as a probable member of the Praesepe cluster (EG59, Claver et al 2001;Catalán et al 2008a). Note that it was mislabeled in both works as explained in Casewell et al (2009).…”

Section: Introductionmentioning

confidence: 99%

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The progenitors of magnetic white dwarfs in open clusters

Külebi

Kalirai

Jordan

et al. 2013

A&A

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Context. White dwarfs are the final stages of stellar evolution for most stars in the galaxy and magnetic white dwarfs (MWDs) represent at least ten percent of the whole sample. According to the fossil-field hypothesis magnetic fields are remnants of the previous stages of evolution. However, population synthesis calculations are unable to reproduce the MWD sample without binary interaction or inclusion of a population of progenitor with unobservable small-scale fields. Aims. One necessary ingredient in population synthesis is the initial-to-final-mass relation (IFMR) which describes the mass-loss processes during the stellar evolution. When white dwarfs are members of open clusters, their evolutionary histories can be assessed through the use of cluster properties. This enables an independent way of determining the mass of their progenitors. The discovery of the magnetic WD 0836+201 in the Praesepe cluster prompted the question whether magnetic fields affect the IFMR. In this work we investigate this suggestion through investigations of all three known MWDs in open clusters. Methods. We assess the cluster membership by correlating the proper-motion of MWDs with the cluster proper-motion and by analyzing the candidates spectroscopically with our magnetic model spectra in order to estimate the effective temperature and radii. Furthermore, we use mass-radius relations and evolutionary models to constrain the histories of the probable cluster members. Results. We identified SDSS J085523.87+164059.0 to be a proper-motion member of Praesepe. We also included the data of the formerly identified cluster members NGC 6819-8, WD 0836+201 and estimated the mass, cooling age and the progenitor masses of the three probable MWD members of open clusters. According to our analysis, the newly identified cluster member SDSS J085523.87+164059.0 is an ultra-massive MWD of mass 1.12 ± 0.11 M . Conclusions. We increase the sample of MWDs with known progenitor masses to ten, with the rest of the data coming from the common proper motion binaries. Our investigations show that, when effects of the magnetic fields are included in the diagnostics, the estimated properties of these cluster MWDs do not show evidence for deviations from the IFMR. Furthermore we estimate the precision of the magnetic diagnostics which would be necessary to determine quantitatively whether magnetism has any effect on the mass-loss.

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Section: Wd 0836+201mentioning

confidence: 89%

Section: Wd 0836+201mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The progenitors of magnetic white dwarfs in open clusters

Külebi

Kalirai

Jordan

et al. 2013

A&A

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“…3 shows that for a stellar mass equal to the minimum mass considered presently, a 10 M Jup mass planet with an orbital radius >2.5 AU should escape engulfment by the parent star. For a ∼1.5 M star (equivalent to a white dwarf of 0.57 M according to Catalán et al 2008) this limit is ∼3.5 AU.…”

Section: Evolutionary Considerationsmentioning

confidence: 99%

Long-term photometry of the eclipsing dwarf nova V893 Scorpii

Bruch

2014

A&A

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Context. The cataclysmic variable V893 Sco is an eclipsing dwarf nova which, apart from outbursts with comparatively low amplitudes, exhibits a particularly strong variability during quiescence on timescales of days to seconds. Aims. The present study aims to update the outdated orbital ephemerides published previously, to investigate deviations from linear ephemerides, and to characterize non-random brightness variations in a range of timescales. Methods. Light curves of V893 Sco were observed on 40 nights, spanning a total time base of about 14 years. They contain 114 eclipses which were used to significantly improve the precision of the orbital period and to study long-term variations of the time of revolution. Oscillations and similar brightness variations were studied with Fourier techniques in the individual light curves. Results. The orbital period exhibits long-term variations with a cycle time of 10.2 years. They can be interpreted as a light travel time effect caused by the presence of a giant planet with approximately 9.5 Jupiter masses in a 4.5 AU orbit around V893 Sco. On some nights transient semi-periodic variations on timescales of several minutes can be seen which may be identified as quasi-periodic oscillations. However, it is difficult to distinguish whether they are caused by real physical mechanisms or if they are the effect of an accidental superposition of unrelated flickering flares. Simulations to investigate this question are presented.

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“…The initial-to-final mass relation can also be studied using white dwarfs in wide binaries (i.e. main-sequence star plus white dwarf; Catalán et al 2008a; or two white dwarfs; Girven et al 2010;Andrews et al 2015), but star clusters are the most favourable test benches as they can contain samples of white dwarfs, which formed from a coeval population of stars . Ground-based follow-up spectroscopy is achievable for numerous cluster white dwarfs, enabling to assess a wide range of white dwarf progenitor masses, from 1.5-2 M (e.g.…”

Section: Introductionmentioning

confidence: 99%

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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Testing the Initial–Final Mass Relationship of White Dwarfs

Cited by 113 publications

References 92 publications

The progenitors of magnetic white dwarfs in open clusters

The progenitors of magnetic white dwarfs in open clusters

Long-term photometry of the eclipsing dwarf nova V893 Scorpii

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

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