Formation and evolution of compact stellar X-ray sources

Tauris, T. M.; Heuvel, E. P. J. van den

doi:10.1017/cbo9780511536281.017

Cited by 427 publications

(396 citation statements)

References 119 publications

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“…The disk extends to a finite outer radius, which we set at r R 4000  = . Certain binaries with long orbital periods may have up to 50 times more extended disks (e.g., Frank et al 2002;Tauris & van den Heuvel 2006). We find, however, that an extent of a=4000 accounts for all but a fraction of 10 4 -of the flux received by a flat disk that extends to infinity ( Table 1).…”

Section: Numerical Modelmentioning

confidence: 64%

Anisotropy of X-Ray Bursts From Neutron Stars With Concave Accretion Disks

Keek

2016

ApJ

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Emission from neutron stars and accretion disks in low-mass X-ray binaries is anisotropic. The non-spherical shape of the disk as well as blocking of the neutron star by the disk make the observed flux dependent on the inclination angle of the disk with respect to the line of sight. This is of importance for the interpretation of thermonuclear X-ray bursts from neutron stars. Because part of the X-ray burst is reflected off the disk, the observed burst flux depends on the anisotropies for both direct emission from the neutron star and reflection off the disk. This influences measurements of source distance, mass accretion rate, and constraints on the neutron star's equation of state. Previous predictions of the anisotropy factors assumed a geometrically flat disk. Detailed observations of two so-called superbursts allowed for the direct and the reflected burst fluxes to each be measured separately. The reflection fraction was much higher than what the anisotropies of a flat disk can account for. We create numerical models to calculate the anisotropy factors for different disk shapes, including concave disks. We present the anisotropy factors of the direct and reflected burst fluxes separately, as well as the anisotropy of the persistent flux. Reflection fractions substantially larger than unity are produced in the case where the inner accretion disk increases steeply in height, such that part of the star is blocked from view. Such a geometry could possibly be induced by the X-ray burst if X-ray heating causes the inner disk to puff up.

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Section: Numerical Modelmentioning

confidence: 64%

Anisotropy of X-Ray Bursts From Neutron Stars With Concave Accretion Disks

Keek

2016

ApJ

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“…For a general review on the formation and evolution of HMXBs, see e.g. Tauris & van den Heuvel (2006). Of particular interest for the scenario discussed in this paper is mass transfer by Roche-lobe overflow (RLO) initiated by the helium-star expansion after core helium depletion, i.e.…”

Section: Introductionmentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

394

609

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The explosion of ultra-stripped stars in close binaries can lead to ejecta masses < 0.1 M ⊙ and may explain some of the recent discoveries of weak and fast optical transients. In Tau ris et al. (2013), it was demonstrated that helium star companions to neutron stars (NSs) may experience mass transfer and evolve into naked ∼ 1.5 M ⊙ metal cores, barely above the Chandrasekhar mass limit. Here we elaborate on this work and present a systematic investigation of the progenitor evolution leading to ultra-stripped supernovae (SNe). In particular, we examine the binary parameter space leading to electron-capture (EC SNe) and iron core-collapse SNe (Fe CCSNe), respectively, and determine the amount of helium ejected with applications to their observational classification as Type Ib or Type Ic. We mainly evolve systems where the SN progenitors are helium star donors of initial mass M He = 2.5 − 3.5 M ⊙ in tight binaries with orbital periods of P orb = 0.06 − 2.0 days, and hosting an accreting NS, but we also discuss the evolution of wider systems and of both more massive and lighter -as well as single -helium stars. In some cases we are able to follow the evolution until the onset of silicon burning, just a few days prior to the SN explosion. We find that ultra-stripped SNe are possible for both EC SNe and Fe CCSNe. EC SNe only occur for M He = 2.60 − 2.95 M ⊙ depending on P orb . The general outcome, however, is an Fe CCSN above this mass interval and an ONeMg or CO white dwarf for smaller masses. For the exploding stars, the amount of helium ejected is correlated with P orb -the tightest systems even having donors being stripped down to envelopes of less than 0.01 M ⊙ . We estimate the rise time of ultra-stripped SNe to be in the range 12 hr − 8 days, and light curve decay times between 1 and 50 days. A number of fitting formulae for our models are provided with applications to population synthesis. Ultrastripped SNe may produce NSs in the mass range 1.10 − 1.80 M ⊙ and are highly relevant for LIGO/VIRGO since most (possibly all) merging double NS systems have evolved through this phase. Finally, we discuss the low-velocity kicks which might be imparted on these resulting NSs at birth.

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“…In particuar, Tauris et al (2013); Tauris, Langer, & Podsiadlowski (2015) proposed an "ultra-stripped" core-collapse SN scenario to explain small ejecta masses. They showed that tight helium star-neutron star (NS) binary systems, presumably created in the common-envelope phase from high-mass X-ray binaries (Tauris & van den Heuvel 2006), can lead to the extreme stripping of the helium envelope and result in SNe with ejecta masses of the order of 0.1 M⊙ or less. The SN ejecta mass from these systems is even less than those typically obtained in SN progenitors from the first exploding stars (∼ 1 M⊙) during binary evolution (e.g., Yoon, Woosley, & Langer 2010;Lyman et al 2016a).…”

Section: Introductionmentioning

confidence: 99%

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

Moriya

Mazzali

Tominaga

et al. 2016

Mon. Not. R. Astron. Soc.

103

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We investigate light-curve and spectral properties of ultra-stripped core-collapse supernovae. Ultra-stripped supernovae are the explosions of heavily stripped massive stars which lost their envelopes via binary interactions with a compact companion star. They eject only ∼ 0.1 M ⊙ and may be the main way to form double neutronstar systems which eventually merge emitting strong gravitational waves. We follow the evolution of an ultra-stripped supernova progenitor until iron core collapse and perform explosive nucleosynthesis calculations. We then synthesize light curves and spectra of ultra-stripped supernovae using the nucleosynthesis results and present their expected properties. Ultra-stripped supernovae synthesize ∼ 0.01 M ⊙ of radioactive 56 Ni, and their typical peak luminosity is around 10 42 erg s −1 or −16 mag. Their typical rise time is 5 − 10 days. Comparing synthesized and observed spectra, we find that SN 2005ek, some of the so-called calcium-rich gap transients, and SN 2010X may be related to ultra-stripped supernovae. If these supernovae are actually ultra-stripped supernovae, their event rate is expected to be about 1 per cent of core-collapse supernovae. Comparing the double neutron-star merger rate obtained by future gravitational-wave observations and the ultra-stripped supernova rate obtained by optical transient surveys identified with our synthesized light-curve and spectral models, we will be able to judge whether ultra-stripped supernovae are actually a major contributor to the binary neutron star population and provide constraints on binary stellar evolution.

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Formation and evolution of compact stellar X-ray sources

Abstract: Single star (X=0.70, Z=0.02 and α = 2.0, δ ov = 0.10). * * Binary star (at onset of RLO: P orb ≃ 60 days and M NS = 1.3 M ⊙ ). After Tauris & Savonije (1999).

Cited by 427 publications

References 119 publications

Anisotropy of X-Ray Bursts From Neutron Stars With Concave Accretion Disks

Anisotropy of X-Ray Bursts From Neutron Stars With Concave Accretion Disks

Ultra-stripped supernovae: progenitors and fate

Light-curve and spectral properties of ultrastripped core-collapse supernovae leading to binary neutron stars

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