Verification of the equivalence of gravitational and inertial mass for the neutron

Koester, L.

doi:10.1103/physrevd.14.907

Cited by 137 publications

(144 citation statements)

References 18 publications

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“…Similar trends are also predicted for the brighter star in binary systems with two white dwarf stars (Nelemans et al 2001). Figure 3 also includes the long period WD+NS system PSR B0820+02d (Koester & Reimers 2000). This particular system extends the apparent correlation toward higher mass (0.60 ± 0.08 M ) and longer period (1232.5 d).…”

Section: Discussionsupporting

confidence: 60%

The double degenerate system NLTT 11748

Kawka

Vennes

Vaccaro

2010

A&A

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We show that the extremely low-mass white dwarf NLTT 11748 (0.17 M ) is in a close binary with a fainter companion. We obtained a series of radial velocity measurements of the low-mass white dwarf using the Hα core and determined an orbital period of 5.64 h. The velocity semi-amplitude (K = 274.8 km s −1 ) and orbital period imply that it is a degenerate star, and that the minimum mass for the companion is 0.75 M (assuming a mass of 0.167 M for the primary). Our analysis of Balmer line profiles shows that a 0.75 M white dwarf companion does not contribute more than 2% or 5% of the flux (V-band) for helium-or hydrogen-rich surfaces, respectively. The kinematics of the system suggest that it belongs to the Galactic halo.

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Section: Discussionsupporting

confidence: 60%

The double degenerate system NLTT 11748

Kawka

Vennes

Vaccaro

2010

A&A

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“…model GS3), also resemble an observed system: PSR B0820+02. This pulsar is in a 1232 day orbit, has a spin period of 0.86 s, and a CO WD companion of mass >0.52 M (Koester & Reimers 2000). Hence, it is indeed possible that some of the observed radio pulsars with CO WDs could have an AIC origin.…”

Section: Observed Pulsars With Co Wds In the Corbet Diagrammentioning

confidence: 99%

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Tauris

Sanyal

Yoon

et al. 2013

A&A

141

181

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Context. Millisecond pulsars (MSPs) are generally believed to be old neutron stars (NSs), formed via type Ib/c core-collapse supernovae (SNe), which have been spun up to high rotation rates via accretion from a companion star in a low-mass X-ray binary (LMXB). In an alternative formation channel, NSs are produced via the accretion-induced collapse (AIC) of a massive white dwarf (WD) in a close binary. Aims. Here we investigate binary evolution leading to AIC and examine if NSs formed in this way can subsequently be recycled to form MSPs and, if so, how they can observationally be distinguished from pulsars formed via the standard core-collapse SN channel in terms of their masses, spins, orbital periods and space velocities. Methods. Numerical calculations with a detailed stellar evolution code were used for the first time to study the combined pre-and post-AIC evolution of close binaries. We investigated the mass transfer onto a massive WD (treated as a point mass) in 240 systems with three different types of non-degenerate donor stars: main-sequence stars, red giants, and helium stars. When the WD is able to accrete sufficient mass (depending on the mass-transfer rate and the duration of the accretion phase) we assumed it collapses to form a NS and we studied the dynamical effects of this implosion on the binary orbit. Subsequently, we followed the mass-transfer epoch which resumes once the donor star refills its Roche lobe and calculated the continued LMXB evolution until the end. Results. We show that recycled pulsars may form via AIC from all three types of progenitor systems investigated and find that the final properties of the resulting MSPs are, in general, remarkably similar to those of MSPs formed via the standard core-collapse SN channel. However, as a consequence of the fine-tuned mass-transfer rate necessary to make the WD grow in mass, the resultant MSPs created via the AIC channel preferentially form in certain orbital period intervals. In addition, their predicted small space velocities can also be used to identify them observationally. The production time of NSs formed via AIC can exceed 10 Gyr which can therefore explain the existence of relatively young NSs in globular clusters. Our calculations are also applicable to progenitor binaries of SNe Ia under certain conditions.

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“…Fundamentally, the nearly universal lack of hydrogen in DBZ stars has been a glaring problem, even for the larger class of helium atmosphere white dwarfs (Koester, 1976;Wesemael, 1979;Aannestad et al, 1993). In essence, if white dwarfs accrete sufficient material of roughly solar composition, they should all (eventually) exhibit hydrogen-dominated outer layers, whereas a significant fraction of all cool white dwarfs are hydrogen-deficient stars, including many with metals.…”

Section: Stellar Interstellar or Circumstellar Mattermentioning

confidence: 99%

Circumstellar debris and pollution at white dwarf stars

Farihi

2016

New Astronomy Reviews

294

265

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Circumstellar disks of planetary debris are now known or suspected to closely orbit hundreds of white dwarf stars. To date, both data and theory support disks that are entirely contained within the preceding giant stellar radii, and hence must have been produced during the white dwarf phase. This picture is strengthened by the signature of material falling onto the pristine stellar surfaces; disks are always detected together with atmospheric heavy elements. The physical link between this debris and the white dwarf host abundances enables unique insight into the bulk chemistry of extrasolar planetary systems via their remnants. This review summarizes the body of evidence supporting dynamically active planetary systems at a large fraction of all white dwarfs, the remnants of first generation, main-sequence planetary systems, and hence provide insight into initial conditions as well as long-term dynamics and evolution.

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Verification of the equivalence of gravitational and inertial mass for the neutron

Cited by 137 publications

References 18 publications

The double degenerate system NLTT 11748

The double degenerate system NLTT 11748

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Circumstellar debris and pollution at white dwarf stars

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