Compact Object Modeling with the StarTrack Population Synthesis Code

Belczyński, Krzysztof; Kalogera, V.; Rasio, Frederic A.; Taam, Ronald E.; Zezas, A.; Bulik, T.; Maccarone, Thomas J.; Іванова, Наталя

doi:10.1086/521026

Cited by 773 publications

(1,125 citation statements)

References 156 publications

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“…We evolve a Galactic population of massive binaries using StarTrack stellar population synthesis code (Belczyński et al 2008). We adopt solar metallicity (Z = 0.02) for the 330 J. Zió lkowski & K. Belczyński Galactic population and low metallicity (Z = 0.008) for the Magellanic Clouds.…”

Section: Stellar Population Synthesis (Sps) Calculationsmentioning

confidence: 99%

On the apparent lack of Be X-ray binaries with black holes in the galaxy and in the Magellanic Clouds

Ziółkowski

Belczyński

2010

Proc. IAU

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Abstract. In the Galaxy there are 67 Be X-ray binaries known to-date. Out of those, 45 host a neutron star, and for the reminder the nature of a companion is not known. None, so far, is known to host a black hole. This disparity is referred to as a missing Be -black hole X-ray binary problem. The stellar population synthesis calculations following the formation of Be X-ray binaries (Belczyński & Zió lkowski 2009) predict that the ratio of the binaries with neutron stars to the ones with black holes is rather high F N S/ B H ∼ 30 − 50. A comparison of this ratio with the number of confirmed Be -neutron star X-ray binaries (45) indicates that the expected number of Be -black hole X-ray binaries is of the order of only ∼ 0 − 2. This is entirely consistent with the observed Galactic sample. Therefore, there is no problem of the missing Be+BH X-Ray Binaries for the Galaxy In the Magellanic Clouds there are 94 Be X-ray binaries known to-date. Out of those, 60 host a neutron star. Again, none hosts a black hole. The stellar population synthesis calculations carried out specifically for the Magellanic Clouds (Zió lkowski & Belczyński 2010) predict that the ratio of the Be X-ray binaries with neutron stars to the ones with black holes is only F N S/ B H ∼ 10. This value is rather too low, as it implies the expected number of Be+BH X-ray binaries of the order of ∼ 6, while none is observed. We found, that to remove the discrepancy, one has to take into account a different history of the star formation rate in the Magellanic Clouds, with the respect to the Galaxy. New stellar population synthesis calculations are currently being carried out.

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Section: Stellar Population Synthesis (Sps) Calculationsmentioning

confidence: 99%

On the apparent lack of Be X-ray binaries with black holes in the galaxy and in the Magellanic Clouds

Ziółkowski

Belczyński

2010

Proc. IAU

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“…Important to all of these investigations is the realization that massive black hole formation is suppressed in stellar populations with higher metallicites (Spera et al, 2015;Belczynski et al, 2008). For example, according to the calculations of Spera et al (2015), a star of mass M 90M will be required to produce a remnant of mass m bh = 30M if its metallicity is Z/Z = −0.5.…”

Section: Introductionmentioning

confidence: 99%

Counting black holes: The cosmic stellar remnant population and implications for LIGO

Elbert

Bullock

Kaplinghat

2017

Monthly Notices of the Royal Astronomical Society

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We present an empirical approach for interpreting gravitational wave signals of binary black hole mergers under the assumption that the underlying black hole population is sourced by remnants of stellar evolution. Using the observed relationship between galaxy mass and stellar metallicity, we predict the black hole count as a function of galaxy stellar mass. We show, for example, that a galaxy like the Milky Way should host millions of ∼ 30 M black holes and dwarf satellite galaxies like Draco should host ∼ 100 such remnants, with weak dependence on the assumed IMF and stellar evolution model. Most low-mass black holes (∼ 10M ) typically reside within massive galaxies (M 10 11 M ) while massive black holes (∼ 50 M ) typically reside within dwarf galaxies (M 10 9 M ) today. If roughly 1% of black holes are involved in a binary black hole merger, then the reported merger rate densities from Advanced LIGO can be accommodated for a range of merger timescales, and the detection of mergers with > 50 M black holes should be expected within the next decade. Identifying the host galaxy population of the mergers provides a way to constrain both the binary neutron star or black hole formation efficiencies and the merger timescale distributions; these events would be primarily localized in dwarf galaxies if the merger timescale is short compared to the age of the universe and in massive galaxies otherwise. As more mergers are detected, the prospect of identifying the host galaxy population, either directly through the detection of electromagnetic counterparts of binary neutron star mergers or indirectly through the anisotropy of the events, will become a realistic possibility.

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“…This simple scenario leads to an energy balance equation of CE evolution, of which the uncertainties are encapsulated into two parameters, the CE efficiency parameter, α CE , and the stellar structure parameter, λ, related to the binding energy of the CE. Much uncertainty surrounds the evaluation of α CE (Tutukov & Yungelson 1996;Kiel & Hurley 2006), however, typically α CE = 1 (Willems & Kolb 2002;Pfahl et al 2003;Voss & Tauris 2003;Kiel & Hurley 2006), α CE λ = 1 (Belczynski et al 2002;Nelemans & Tout 2005;Pfahl, Podsiadlowski & Rappaport 2005;Belczynski et al 2008) or α CE = 3 (Kiel & Hurley 2006;Kiel et al 2008;Kiel, Hurley & Bailes 2010;Hurley et al 2010).…”

Section: Population Synthesis Methodsmentioning

confidence: 99%

Accretion, ablation and propeller evolution in close millisecond pulsar binary systems

Kiel¹,

Taam²

2013

Astrophys Space Sci

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A model for the formation and evolution of binary millisecond radio pulsars in systems with low mass companions (< 0.1 M ⊙ ) is investigated using a binary population synthesis technique. Taking into account the non conservative evolution of the system due to mass loss from an accretion disk as a result of propeller action and from the companion via ablation by the pulsar, the transition from the accretion powered to rotation powered phase is investigated. It is shown that the operation of the propeller and ablation mechanisms can be responsible for the formation and evolution of black widow millisecond pulsar systems from the low mass X-ray binary phase at an orbital period of ∼ 0.1 day. For a range of population synthesis input parameters, the results reveal that a population of black widow millisecond pulsars characterized by orbital periods as long as ∼ 0.4 days and companion masses as low as ∼ 0.005 M ⊙ can be produced. The orbital periods and minimum companion mass of this radio millisecond pulsar population critically depend on the thermal bloating of the semi-degenerate hydrogen mass losing component, with longer orbital periods for a greater degree of bloating. Provided that the radius of the companion is increased by about a factor of 2 relative to a fully degenerate, zero temperature configuration, an approximate agreement between observed long orbital periods and theoretical modeling of hydrogen rich donors can be achieved. We find no discrepancy between the estimated birth rates for LMXBs and black

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Compact Object Modeling with the StarTrack Population Synthesis Code

Cited by 773 publications

References 156 publications

On the apparent lack of Be X-ray binaries with black holes in the galaxy and in the Magellanic Clouds

On the apparent lack of Be X-ray binaries with black holes in the galaxy and in the Magellanic Clouds

Counting black holes: The cosmic stellar remnant population and implications for LIGO

Accretion, ablation and propeller evolution in close millisecond pulsar binary systems

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