A catalogue of isolated massive white dwarfs

Nalezyty, M.; Madej, J.

doi:10.1051/0004-6361:20040123

Cited by 30 publications

(37 citation statements)

References 52 publications

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“…A substantial numbers of massive and ultra-massive WDs 8 have been discovered in white dwarf surveys; with estimates that about 20 per cent of all WDs are massive WDs Kepler et al 2007) and about 10 per cent ultra-massive WDs (Vennes & Kawka 2008). We note that a second WD mass distribution peak at ∼ 1.04 M⊙ was found by Należyty & Madej (2004) which interestingly closely corresponds to the divide between CO and ONe core compositions (Fig. 6).…”

Section: Final Fatessupporting

confidence: 66%

Super- and massive AGB stars – IV. Final fates – initial-to-final mass relation

Doherty

Gil‐Pons

Siess

et al. 2014

Monthly Notices of the Royal Astronomical Society

233

278

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We explore the final fates of massive intermediate-mass stars by computing detailed stellar models from the zero age main sequence until near the end of the thermally pulsing phase. These super-AGB and massive AGB star models are in the mass range between 5.0 and 10.0 M ⊙ for metallicities spanning the range Z=0.02−0.0001. We probe the mass limits M up , M n and M mass , the minimum masses for the onset of carbon burning, the formation of a neutron star, and the iron core-collapse supernovae respectively, to constrain the white dwarf/electron-capture supernova boundary. We provide a theoretical initial to final mass relation for the massive and ultra-massive white dwarfs and specify the mass range for the occurrence of hybrid CO(Ne) white dwarfs. We predict electron-capture supernova (EC-SN) rates for lower metallicities which are significantly lower than existing values from parametric studies in the literature. We conclude the EC-SN channel (for single stars and with the critical assumption being the choice of mass-loss rate) is very narrow in initial mass, at most ≈ 0.2 M ⊙ . This implies that between ∼ 2−5 per cent of all gravitational collapse supernova are EC-SNe in the metallicity range Z=0.02 to 0.0001. With our choice for mass-loss prescription and computed core growth rates we find, within our metallicity range, that CO cores cannot grow sufficiently massive to undergo a Type 1.5 SN explosion.

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Section: Final Fatessupporting

confidence: 66%

Super- and massive AGB stars – IV. Final fates – initial-to-final mass relation

Doherty

Gil‐Pons

Siess

et al. 2014

Monthly Notices of the Royal Astronomical Society

233

278

View full text Add to dashboard Cite

show abstract

“…Ages are determined through white dwarf cooling; a textbook account appears in [59], with further discussion in [58,60,61]. Several known white dwarfs satisfying our criteria of mass M * M , B p & few Â 10 5 G, and age T * 100 Myr can be found, for example, in [62][63][64][65]. When not given explicitly, the ages can be inferred from the mass-temperature relations, as discussed e.g.…”

Section: Summary Of White Dwarf Constraintsmentioning

confidence: 99%

Astrophysical implications of hypothetical stable TeV-scale black holes

Giddings

Mangano

2008

Phys. Rev. D

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We analyze macroscopic effects of TeV-scale black holes, such as could possibly be produced at the LHC, in what is regarded as an extremely hypothetical scenario in which they are stable and, if trapped inside Earth, begin to accrete matter. We examine a wide variety of TeV-scale gravity scenarios, basing the resulting accretion models on first-principles, basic, and well-tested physical laws. These scenarios fall into two classes, depending on whether accretion could have any macroscopic effect on the Earth at times shorter than the Sun's natural lifetime. We argue that cases with such effect at shorter times than the solar lifetime are ruled out, since in these scenarios black holes produced by cosmic rays impinging on much denser white dwarfs and neutron stars would then catalyze their decay on timescales incompatible with their known lifetimes. We also comment on relevant lifetimes for astronomical objects that capture primordial black holes. In short, this study finds no basis for concerns that TeV-scale black holes from the LHC could pose a risk to Earth on time scales shorter than the Earth's natural lifetime. Indeed, conservative arguments based on detailed calculations and the best-available scientific knowledge, including solid astronomical data, conclude, from multiple perspectives, that there is no risk of any significance whatsoever from such black holes.Comment: Version2: Minor corrections/fixed typos; updated reference

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“…The red line is the theoretical line. The blue triangles and circles are observed WD data, taken from table 1 of Należyty & Madej (2004) and tables 3 and 5 of Provencal et al (1998), respectively. Among these data, the WD RE J0317‐853 is the most massive WD, with mass and radius 1.34 M ⊙ and 2400 km respectively.…”

Section: Submillisecond Quark Stars Formed Through the Aic Of Wdsmentioning

confidence: 99%

The formation of submillisecond pulsars and the possibility of detection

Qiao

et al. 2009

Monthly Notices of the Royal Astronomical Society

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Pulsars have been recognized to be normal neutron stars, but sometimes have been argued to be quark stars. Submillisecond pulsars, if detected, would play an essential and important role in distinguishing quark stars from neutron stars. We focus on the formation of such submillisecond pulsars in this paper. A new approach to the formation of a submillisecond pulsar (quark star) by means of the accretion‐induced collapse (AIC) of a white dwarf is investigated. Under this AIC process, we found that: (i) almost all newborn quark stars could have an initial spin period of ∼0.1 ms; (ii) nascent quark stars (even with a low mass) have a sufficiently high spin‐down luminosity and satisfy the conditions for pair production and sparking process and appear as submillisecond radio pulsars; (iii) in most cases, the times of newborn quark stars in the phase with spin period <1 (or <0.5) ms are long enough for the stars to be detected. As a comparison, an accretion spin‐up process (for both neutron and quark stars) is also investigated. It is found that quark stars formed through the AIC process can have shorter periods (≤0.5 ms), whereas the periods of neutron stars formed in accretion spin‐up processes must be longer than 0.5 ms. Thus, if a pulsar with a period shorter than 0.5 ms is identified in the future, it could be a quark star.

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A catalogue of isolated massive white dwarfs

Cited by 30 publications

References 52 publications

Super- and massive AGB stars – IV. Final fates – initial-to-final mass relation

Super- and massive AGB stars – IV. Final fates – initial-to-final mass relation

Astrophysical implications of hypothetical stable TeV-scale black holes

The formation of submillisecond pulsars and the possibility of detection

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