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White dwarf

About: White dwarf is a research topic. Over the lifetime, 15004 publications have been published within this topic receiving 430597 citations. The topic is also known as: degenerate dwarf.


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Journal ArticleDOI
TL;DR: In this article, the authors used the Modules for Experiments in Stellar Evolution (ME) code to calculate stellar evolution models of low mass rotating stars from the zero-age main sequence to the cooling white dwarf (WD) stage.
Abstract: Asteroseismology of 1.0-2.0 M {sub ☉} red giants by the Kepler satellite has enabled the first definitive measurements of interior rotation in both first ascent red giant branch (RGB) stars and those on the helium burning clump. The inferred rotation rates are 10-30 days for the ≈0.2 M {sub ☉} He degenerate cores on the RGB and 30-100 days for the He burning core in a clump star. Using the Modules for Experiments in Stellar Evolution code, we calculate state-of-the-art stellar evolution models of low mass rotating stars from the zero-age main sequence to the cooling white dwarf (WD) stage. We include transport of angular momentum due to rotationally induced instabilities and circulations, as well as magnetic fields in radiative zones (generated by the Tayler-Spruit dynamo). We find that all models fail to predict core rotation as slow as observed on the RGB and during core He burning, implying that an unmodeled angular momentum transport process must be operating on the early RGB of low mass stars. Later evolution of the star from the He burning clump to the cooling WD phase appears to be at nearly constant core angular momentum. We also incorporate the adiabatic pulsation code, ADIPLS, tomore » explicitly highlight this shortfall when applied to a specific Kepler asteroseismic target, KIC8366239.« less

275 citations

Journal ArticleDOI
TL;DR: Most of the known pulsars are single and located in the disk of the Galaxy as mentioned in this paper, and there is circumstantial evidence that the pulsars in this majority are created in supernova (SN) explosions, by the collapse of the cores of massive massively massive stars.
Abstract: Most of the ~600 known pulsars are single and located in the disk of our Galaxy. There is circumstantial evidence that the pulsars in this majority are created in supernova (SN) explosions, by the collapse of the cores of massive stars (initial mass M_i ≳ M_(cr) ≃ 8 M_⊙). One is created roughly every 100 y in the Galaxy.

273 citations

Journal ArticleDOI
TL;DR: In this article, it was shown that unless mass transfer occurs at a rate less than one-fifth of the Eddington limit for an isolated dwarf, carbon is ignited off-center, and ignition does not lead immediately to a deflagration.
Abstract: Recent studies have suggested that the merging of two degenerate dwarfs composed of carbon and oxygen and of total mass larger than the Chandrasekhar limit occurs at a frequency comparable to that of Type I supernovae. The rate at which mass is transferred in the merging process is at present unknown, except that it must be less than some appropriate Eddington limit. It is found that, unless mass transfer occurs at a rate less than one-fifth of the Eddington limit for an isolated dwarf, carbon is ignited off-center, and ignition does not lead immediately to a deflagration. If carbon continues to burn quiescently until it is exhausted throughout the star, a neon-oxygen-magnesium white dwarf will be formed. If a Type I supernova is to follow from merging white dwarfs, a thick disk must be formed as an intermediate stage in the merging process, with transfer from the disk onto the central degenerate dwarf occurring at a rate sufficiently less than Eddington that a deflagration induced by carbon burning occurs. Thus, the outcome of the merging of two massive carbon-oxygen degenerate dwarfs is not trivially a Type I supernova explosion. 43 references.

273 citations

Journal ArticleDOI
TL;DR: In this article, the current status of research on the observational and theoretical characteristics of isolated and binary magnetic white dwarfs (MWDs) is reviewed, and a review of the existing literature is presented.
Abstract: In this paper we review the current status of research on the observational and theoretical characteristics of isolated and binary magnetic white dwarfs (MWDs).

272 citations

Journal ArticleDOI
TL;DR: In this article, a synthetic model for thermally pulsing asymptotic giant branch (TPAGB) evolution constructed by fitting expressions to full evolutionary models in the metallicity range 0.0001 Z 0.02 was presented.
Abstract: We present a synthetic model for thermally pulsing asymptotic giant branch (TPAGB) evolution constructed by fitting expressions to full evolutionary models in the metallicity range 0.0001 Z 0.02. Our model includes parametrizations of third dredge-up and hot-bottom burning with mass and metallicity. The Large Magellanic Cloud and Small Magellanic Cloud carbon star luminosity functions are used to calibrate third dredge-up. We calculate yields appropriate for galactic chemical evolution models for 1 H, 4 He, 12 C, 13 C, 14 N, 15 N, 16 O and 17 O. The

272 citations


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Performance
Metrics
No. of papers in the topic in previous years
YearPapers
2023367
2022667
2021495
2020557
2019548
2018515