The Formation and Evolution of Relativistic Binaries

Heuvel, E. P. J. van den

doi:10.1007/978-1-4020-9264-0_4

Cited by 20 publications

(2 citation statements)

References 128 publications

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“…In the in-situ formation scenario, ordinary pulsars form out of regular star formation and should be found where young massive stars are observed, ∼ 0.5 pc (Bartko et al 2009;Yusef-Zadeh et al 2013;Mapelli & Gualandris 2016). Field binaries and binaries that form via dynamical interactions in the densest regions of the NSC can produce a population of MSPs (Faucher-Giguère & Loeb 2011).…”

Section: Introductionmentioning

confidence: 99%

Probing the formation history of the nuclear star cluster at the Galactic Centre with millisecond pulsars

Abbate

Mastrobuono-Battisti

Colpi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The origin of the Nuclear Star Cluster in the centre of our Galaxy is still unknown. One possibility is that it formed after the disruption of stellar clusters that spiralled into the Galactic Centre due to dynamical friction. We trace the formation of the Nuclear Star Cluster around the central black hole, using state-of-the-art N-body simulations, and follow the dynamics of the neutron stars born in the clusters. We then estimate the number of Millisecond Pulsars (MSPs) that are released in the Nuclear Star Cluster during its formation. The assembly and tidal dismemberment of globular clusters lead to a population of MSPs distributed over a radius of about 20 pc, with a peak near 3 pc. No clustering is found on the sub-parsec scale. We simulate the detectability of this population with future radio telescopes like the MeerKAT radio telescope and SKA1, and find that about of order ten MSPs can be observed over this large volume, with a paucity of MSPs within the central parsec. This helps discriminating this scenario from the in-situ formation model for the Nuclear Star Cluster that would predict an over abundance of MSPs closer to the black hole. We then discuss the potential contribution of our MSP population to the gamma-ray excess at the Galactic Centre.

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Section: Introductionmentioning

confidence: 99%

Probing the formation history of the nuclear star cluster at the Galactic Centre with millisecond pulsars

Abbate

Mastrobuono-Battisti

Colpi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Hence, the mass-transfer efficiency, i.e., the fraction of matter accreted onto the secondary among all transferred matter, is a key factor determining whether a binary system evolves into contact. This efficiency has been widely discussed in the literature (e.g., Vanbeveren et al 1979;De Loore & De Greve 1992;Wellstein et al 2001;Petrovic et al 2005;de Mink et al 2007;Shao & Li 2014, 2016. It is suggested that the secondary star with rapid rotation will suppress its mass increment and drop the masstransfer efficiency (Petrovic et al 2005;Stancliffe & Eldridge 2009).…”

Section: The Case Of Bh Binaries With a High-mass Secondarymentioning

confidence: 98%

On the Neutron Star/Black Hole Mass Gap and Black Hole Searches

Shao

2022

Res. Astron. Astrophys.

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Mass distribution of black holes in low-mass X-ray binaries previously suggested the existence of a $ \sim 2-5M_{\odot} $ mass gap between the most massive neutron stars and the least massive black holes, while some recent evidence appears to support that this mass gap is being populated. Whether there is a mass gap or not can potentially shed light on the physics of supernova explosions that form neutron stars and black holes, although significant mass accretion of neutron stars including binary mergers may lead to the formation of mass-gap objects. In this review, I collect the compact objects that are probable black holes with masses being in the gap. Most of them are in binaries, their mass measurements are obviously subject to some uncertainties. Current observations are still unable to confidently infer an absence or presence of the mass gap. Ongoing and future surveys are expected to build the mass spectrum of black holes which can be used to constrain the process of their formation especially in binaries. I describe the theoretical predictions for the formation of black holes in various types of binaries, and present some prospects of searching for black holes via electromagnetic and gravitational wave observations.

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Where do the progenitors of millisecond pulsars come from?

et al. 2012

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Observations of a large population of millisecond pulsars (MSPs) show a wide divergence in the orbital periods (from approximately hours to a few months). In the standard view, low-mass X-ray binaries (LMXBs) are considered as progenitors for some MSPs during the recycling process. We present a systematic study that combines different types of compact objects in binaries such as cataclysmic variables (CVs), LMXBs, and MSPs. We plot them together in the so called Corbet diagram. Larger and different samples are needed to better constrain the result as a function of the environment and formations. A scale diagram showing the distribution of MSPs for different orbital periods and the aspects for their progenitors relying on accretion induced collapse (AIC) of white dwarfs in binaries. Thus massive CVs (M ≥ 1.1 M ) can play a vital role on binary evolution, as well as of the physical processes involved in the formation and evolution of neutron stars and their magnetic fields, and could turn into binary MSPs with different scales of orbital periods; this effect can be explained by the AIC process. This scenario also suggests that some fraction of isolated MSPs in the Galactic disk could be formed through the same channel, forming the contribution of some CVs to the single-degenerate progenitors of Type Ia supernova. Furthermore, we have refined the statistical distribution and evolution by using updated data. This implies that the significant studies of compact objects in binary systems can benefit from the Corbet diagram.

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The Formation and Evolution of Relativistic Binaries

Cited by 20 publications

References 128 publications

Probing the formation history of the nuclear star cluster at the Galactic Centre with millisecond pulsars

Probing the formation history of the nuclear star cluster at the Galactic Centre with millisecond pulsars

On the Neutron Star/Black Hole Mass Gap and Black Hole Searches

Where do the progenitors of millisecond pulsars come from?

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