Gravitational redshift for the Pleiad white dwarf LB 1497

Wegner, Gary A.; Reid, I. N.; McMahan, Robert K.

doi:10.1086/170266

Cited by 18 publications

(10 citation statements)

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“…One additional constraint is also reproduced. There is one white dwarf member of the Pleiades with a mass of ∼ 1 M ⊙ (Wegner et al 1991). Our models produce a white dwarf progenitor of ∼ 1 M ⊙ at the age of the cluster from an initial mass of ∼ 5.5 M ⊙ .…”

Section: Comparison With LI Depletion Agesmentioning

confidence: 82%

Stellar Hydrodynamics in Radiative Regions

Young

Knierman

Rigby

et al. 2003

ApJ

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We present an analysis of the response of a radiative region to waves generated by a convective region of the star; this wave treatment of the classical problem of ``overshooting'' gives extra mixing relative to the treatment traditionally used in stellar evolutionary codes. The interface between convectively stable and unstable regions is dynamic and nonspherical, so that the nonturbulent material is driven into motion, even in the absence of ``penetrative overshoot.'' These motions may be described by the theory of nonspherical stellar pulsations, and are related to motion measured by helioseismology. Multi-dimensional numerical simulations of convective flow show puzzling features which we explain by this simplified physical model. Gravity waves generated at the interface are dissipated, resulting in slow circulation and mixing seen outside the formal convection zone. The approach may be extended to deal with rotation and composition gradients. Tests of this description in the stellar evolution code TYCHO produce carbon stars on the asymptotic giant branch (AGB), an isochrone age for the Hyades and three young clusters with lithium depletion ages from brown dwarfs, and lithium and beryllium depletion consistent with observations of the Hyades and Pleiades, all without tuning parameters. The insight into the different contributions of rotational and hydrodynamic mixing processes could have important implications for realistic simulation of supernovae and other questions in stellar evolution.Comment: 27 pages, 5 figures, accepted to the Astrophysical Journa

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Section: Comparison With LI Depletion Agesmentioning

confidence: 82%

Stellar Hydrodynamics in Radiative Regions

Young

Knierman

Rigby

et al. 2003

ApJ

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“…4). This corresponds to a mass of 1.02 ±0.02 M ⊙ , in excellent agreement with the gravitational redshift determination (1.02 ± +0.04 −0.05 M ⊙ ; Wegner, Reid & McMahan 1991). For the WD members of M35 and NGC 2516, we adopt the effective temperatures and surface gravities listed in table 1 of Ferrario et al (2005).…”

Section: Discussionmentioning

confidence: 99%

New Praesepe white dwarfs and the initial mass–final mass relation

Dobbie¹,

Napiwotzki²,

Burleigh³

et al. 2006

Monthly Notices of the Royal Astronomical Society

105

146

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We report the spectroscopic confirmation of four further white dwarf members of Praesepe. This brings the total number of confirmed white dwarf members to 11, making this the second largest collection of these objects in an open cluster identified to date. This number is consistent with the high‐mass end of the initial mass function of Praesepe being Salpeter in form. Furthermore, it suggests that the bulk of Praesepe white dwarfs did not gain a substantial recoil kick velocity from possible asymmetries in their loss of mass during the asymptotic giant branch phase of evolution. By comparing our estimates of the effective temperatures and the surface gravities of WD0833+194, WD0840+190, WD0840+205 and WD0843+184 to modern theoretical evolutionary tracks, we have derived their masses to be in the range 0.72–0.76 M⊙ and their cooling ages ∼300 Myr. For an assumed cluster age of 625 ± 50 Myr, the inferred progenitor masses are between 3.3 and 3.5 M⊙. Examining these new data in the context of the initial mass–final mass relation, we find that it can be adequately represented by a linear function (a0= 0.289 ± 0.051, a1= 0.133 ± 0.015) over the initial mass range 2.7–6 M⊙. Assuming an extrapolation of this relation to larger initial masses is valid and adopting a maximum white dwarf mass of 1.3 M⊙, our results support a minimum mass for core‐collapse supernovae progenitors in the range ∼6.8–8.6 M⊙.

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“…LB 1497 is a member of the Pleiades and Wegner et al (1991) reported a gravitational redshift of v g = 84 ± 9 km s −1 for this DA white dwarf. Bergeron et al (1995) also reported a temperature T eff = 31 660 ± 350 K and a high gravity of log g = 8.78 ± 0.05.…”

Section: Based On Gravitational Redshift: the Cpmb Sample And Clustmentioning

confidence: 90%

“…The massive white dwarf and member of the Pleiades LB 1497 (Wegner, Reid & McMahan 1991) remained a unique candidate for having a mass in excess of 1.0 M ⊙ and possibly in excess of 1.1 M ⊙ among stars with gravitational redshift measurements (Wegner & Reid 1991; Bergeron, Liebert & Fulbright 1995; Reid 1996). However, applying the same techniques to white dwarfs in common proper motion binaries Silvestri et al (2001) proposed new ultramassive white dwarf candidates (Table 1).…”

Section: Based On Gravitational Redshift: the Cpmb Sample And Clustmentioning

confidence: 99%

On the empirical evidence for the existence of ultramassive white dwarfs

Vennes¹,

Kawka²

2008

Monthly Notices of the Royal Astronomical Society

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We re-examine the evidence for the existence of ultramassive (M > 1.1 M ) white dwarfs based on gravitational redshift of white dwarfs in common proper motion binaries or in clusters, on parallax measurements, on orbital solutions and, finally, on the analysis of hydrogen-line profiles. We conclude that the best evidence is largely based on the analysis of Balmerline profiles although the companion to the A8V star HR 8210 is a compelling case made initially using the large binary mass function and confirmed by an analysis of the Lyman-line spectrum. The confirmation and identification of high-mass white dwarfs, more particularly non-hydrogen-rich (non-DA) white dwarfs, using parallax measurements may prove critical in establishing the population fraction of these objects and in constraining the high end of empirical initial-mass to final-mass relations. The existence of a substantial population of ultramassive white dwarfs supports the concept of a steeper initial-mass to final-mass relations linking 6 M progenitors with 1.1 M white dwarfs.

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Gravitational redshift for the Pleiad white dwarf LB 1497

Cited by 18 publications

References 0 publications

Stellar Hydrodynamics in Radiative Regions

Stellar Hydrodynamics in Radiative Regions

New Praesepe white dwarfs and the initial mass–final mass relation

On the empirical evidence for the existence of ultramassive white dwarfs

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