Explosive common-envelope ejection: implications for gamma-ray bursts and low-mass black-hole binaries

Podsiadlowski, Philipp; Иванова, Н. М.; Justham, Stephen; Rappaport, S.

doi:10.1111/j.1365-2966.2010.16751.x

Cited by 115 publications

(113 citation statements)

References 66 publications

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“…In this study, the density profile of the donor envelope is parametrized by λ = 1/2, the efficiency with which orbital energy is used on unbinding the common envelope by α CE = 4 (justified by explosive shell burning in massive stars during the common-envelope phase, Podsiadlowski et al 2010) and the specific angular momentum of the envelope after it has left the system, relative to the specific angular momentum of the pre-common-envelope binary, by γ = 7/4. In choosing a value of α CE λ = 2 for massive stars we follow Portegies Zwart & Yungelson (1998); Yungelson et al (2006); Yungelson & Lasota (2008).…”

Section: Population Synthesismentioning

confidence: 99%

Population synthesis of ultracompact X-ray binaries in the Galactic bulge

Haaften

Nelemans

Voss

et al. 2013

A&A

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Aims.We model the present-day number and properties of ultracompact X-ray binaries (UCXBs) in the Galactic bulge. The main objective is to compare the results to the known UCXB population as well as to data from the Galactic Bulge Survey, in order to learn about the formation of UCXBs and their evolution, such as the onset of mass transfer and late-time behavior. Methods. The binary population synthesis code SeBa and detailed stellar evolutionary tracks have been used to model the UCXB population in the Bulge. The luminosity behavior of UCXBs has been predicted using long-term X-ray observations of the known UCXBs as well as the thermal-viscous disk instability model. Results. In our model, the majority of UCXBs initially have a helium burning star donor. Of the white dwarf donors, most have helium composition. In the absence of a mechanism that destroys old UCXBs, we predict (0.2−1.9) × 10 5 UCXBs in the Galactic bulge, depending on assumptions, mostly at orbital periods longer than 60 min (a large number of long-period systems also follows from the observed short-period UCXB population). About 5−50 UCXBs should be brighter than 10 35 erg s −1 , mostly persistent sources with orbital periods shorter than about 30 min and with degenerate helium and carbon-oxygen donors. This is about one order of magnitude more than the observed number of (probably) three. Conclusions. This overprediction of short-period UCXBs by roughly one order of magnitude implies that fewer systems are formed, or that a super-Eddington mass transfer rate is more difficult to survive than we assumed. The very small number of observed longperiod UCXBs with respect to short-period UCXBs, the surprisingly high luminosity of the observed UCXBs with orbital periods around 50 min, and the properties of the PSR J1719−1438 system all point to much faster UCXB evolution than expected from angular momentum loss via gravitational wave radiation alone. Old UCXBs, if they still exist, probably have orbital periods longer than 2 h and have become very faint due to either reduced accretion or quiescence, or have become detached. UCXBs are promising candidate progenitors of isolated millisecond radio pulsars.

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Section: Population Synthesismentioning

confidence: 99%

Population synthesis of ultracompact X-ray binaries in the Galactic bulge

Haaften

Nelemans

Voss

et al. 2013

A&A

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“…For example, Ivanova (2002) argued that nuclear fusion should be added into the energy sources that may contribute to the envelope ejection. Podsiadlowski et al (2010) proposed that a thermonuclear runaway which is caused by the mixing hydrogen from the secondary into the helium-burning shell of the primary would assist the ejection. When treating the binding energy of the envelope, Ivanova & Chaichenets (2011) pointed out that there might be mass outflows during the slow spiral-in stage, when the orbital energy is balanced with the enthalpy rather than merely the internal energy of the envelope.…”

Section: Introductionmentioning

confidence: 99%

On the formation of galactic black hole low-mass X-ray binaries

Wang

Jia

2016

Mon. Not. R. Astron. Soc.

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Currently, there are 24 black hole (BH) X-ray binary systems that have been dynamically confirmed in the Galaxy. Most of them are low-mass X-ray binaries (LMXBs) comprised of a stellar-mass BH and a low-mass donor star. Although the formation of these systems has been extensively investigated, some crucial issues remain unresolved. The most noticeable one is that, the low-mass companion has difficulties in ejecting the tightly bound envelope of the massive primary during the spiral-in process. While initially intermediate-mass binaries are more likely to survive the common envelope (CE) evolution, the resultant BH LMXBs mismatch the observations. In this paper, we use both stellar evolution and binary population synthesis to study the evolutionary history of BH LMXBs. We test various assumptions and prescriptions for the supernova mechanisms that produce BHs, the binding energy parameter, the CE efficiency, and the initial mass distributions of the companion stars. We obtain the birthrate and the distributions of the donor mass, effective temperature and orbital period for the BH LMXBs in each case. By comparing the calculated results with the observations, we put useful constraints on the aforementioned parameters. In particular, we show that it is possible to form BH LMXBs with the standard CE scenario if most BHs are born through failed supernovae.

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“…Close massive binary systems that experience mass trans- fer, common-envelope evolution, or a merger (Podsiadlowski et al 2010;Langer 2012) are possible progenitors of LGRBs, because they can likely produce the required rapidly rotating massive stars without H or He envelopes. Recent observations of Galactic O-type stars show that, in fact, 70% of massive stars experience mass transfer with a companion and ∼ 30% undergo a merger (Sana et al 2012).…”

Section: Introductionmentioning

confidence: 99%

The Host Galaxies of Fast-Ejecta Core-Collapse Supernovae

Kelly

Filippenko

Modjaz

et al. 2014

ApJ

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Spectra of broad-lined Type Ic supernovae (SN Ic-BL), the only kind of SN observed at the locations of long-duration gamma-ray bursts (LGRBs), exhibit wide features indicative of high ejecta velocities (∼ 0.1c). We study the host galaxies of a sample of 245 low-redshift (z < 0.2) core-collapse SN, including 17 SN Ic-BL, discovered by galaxy-untargeted searches, and 15 optically luminous and dust-obscured z < 1.2 LGRBs. We show that, in comparison with SDSS galaxies having similar stellar masses, the hosts of low-redshift SN Ic-BL and z < 1.2LGRBs have high stellar-mass and star-formation-rate densities. Core-collapse SN having typical ejecta velocities, in contrast, show no preference for such galaxies. Moreover, we find that the hosts of SN Ic-BL, unlike those of SN Ib/Ic and SN II, exhibit high gas velocity dispersions for their stellar masses. The patterns likely reflect variations among star-forming environments, and suggest that LGRBs can be used as probes of conditions in high-redshift galaxies. They may be caused by efficient formation of massive binary progenitors systems in densely star-forming regions, or, less probably, a higher fraction of stars created with the initial masses required for a SN Ic-BL or LGRB. Finally, we show that the preference of SN Ic-BL and LGRBs for galaxies with high stellar-mass and star-formation-rate densities cannot be attributed to a preference for low metal abundances but must reflect the influence of a separate environmental factor.

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Explosive common-envelope ejection: implications for gamma-ray bursts and low-mass black-hole binaries

Cited by 115 publications

References 66 publications

Population synthesis of ultracompact X-ray binaries in the Galactic bulge

Population synthesis of ultracompact X-ray binaries in the Galactic bulge

On the formation of galactic black hole low-mass X-ray binaries

The Host Galaxies of Fast-Ejecta Core-Collapse Supernovae

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