Tidal capture formation of low-mass X-ray binaries from wide binaries in the field

Michaely, Erez; Perets, Hagai B.

doi:10.1093/mnras/stw368

Cited by 39 publications

(41 citation statements)

References 43 publications

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“…Note that the rate from the scenario of natal kicks corresponds only to binaries with separations >10 AU. The rates for the channel of perturbed wide binaries correspond to the scenario of high rates obtained by Michaely & Perets (2016), for direct-collapse BHs with no natal kicks (reproducing the formation rate of LMXBs in the Galaxy); therefore this channel and the scenario of natal kicks are mutually exclusive.…”

Section: Flare Energysupporting

confidence: 67%

MICRO-TIDAL DISRUPTION EVENTS BY STELLAR COMPACT OBJECTS AND THE PRODUCTION OF ULTRA-LONG GRBs

Perets

Lombardi

et al. 2016

ApJ

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105

129

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We explore full/partial tidal disruption events (TDEs) of stars/planets by stellar compact objects (black holes (BHs) or neutron stars (NSs)), which we term micro-TDEs. Disruption of a star/planet with mass M å may lead to the formation of a debris disk around the BH/NS. Efficient accretion of a fraction = f 0.1 acc ( of the debris may then give rise to bright, energetic, long (10 3 -10 4 s), X-ray/gamma-ray flares, with total energies of up to( ) ( ) erg, possibly resembling ultra-long gamma-ray bursts (GRBs)/X-ray flashes (XRFs). The energy of such flares depends on the poorly constrained accretion processes. Significantly fainter flares might be produced if most of the disk mass is blown away through strong outflows. We suggest three dynamical origins for such disruptions. In the first, a star/planet is tidally disrupted following a close random encounter with a BH/NS in a dense cluster. We estimate the BH (NS) micro-TDE rates from this scenario to be a few´-10 6 (a few´-10 7 )yr 1 per Milky Way galaxy. Another scenario involves the interaction of wide companions due to perturbations by stars in the field, likely producing comparable but lower rates. Finally, a third scenario involves a BH/NS that gains a natal velocity kick at birth, leading to a close encounter with a binary companion and the tidal disruption of that companion. Such events could be associated with a supernova, or even with a preceding GRB/XRF event, and would likely occur hours to days after the prompt explosion; the rates of such events could be larger than those obtained from the other scenarios, depending on the preceding complex binary stellar evolution.

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Section: Flare Energysupporting

confidence: 67%

MICRO-TIDAL DISRUPTION EVENTS BY STELLAR COMPACT OBJECTS AND THE PRODUCTION OF ULTRA-LONG GRBs

Perets

Lombardi

et al. 2016

ApJ

Self Cite

105

129

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“…In particular, Kaib and Raymond [21] calculated the probability of a head-on collision between two main-sequence stars in the Milky-Way Galaxy due to interaction with random stellar perturbers. Michaely and Perets [30] followed these directions and suggested a novel formation scenario for lowmass X-ray binaries from wide-binaries in the field.…”

Section: Introductionmentioning

confidence: 94%

“…In order to do that we need to integrate over all SMA in a given stellar density and over all stellar densities in the galaxy we model. We follow a similar calculation from Michaely and Perets [30]. We model the Galaxy in the following way, let dN (r) = n * (r) · 2π · r · h · dr be the the number of stars in a region dr (and scale height h), located at distance r from the center of the Galaxy.…”

Section: B Analytic Descriptionmentioning

confidence: 99%

“…Here we present a fourth channel of binary evolution, in which we focus of wide (SMA >1000AU) BBHs in the field perturbed by random fly-by interactions of field stars in their host galaxy. Kaib and Raymond [21] and Michaely and Perets [30] showed that although evolution of stars and binaries in the low-density environment in the field is typically thought to be collisionless, wide binary systems can be significantly affected by flyby interactions of field stars stars, and effectively experience a collisional evolution. In particular, Kaib and Raymond [21] calculated the probability of a head-on collision between two main-sequence stars in the Milky-Way Galaxy due to interaction with random stellar perturbers.…”

Section: Introductionmentioning

confidence: 99%

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Gravitational-wave Sources from Mergers of Binary Black Holes Catalyzed by Flyby Interactions in the Field

Michaely

Perets

2019

ApJL

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Several scenarios were suggested for the origins of gravitational-wave (GW) sources from mergers of stellar binary black holes (BBHs). Here we propose a novel origin through catalyzed formation of GW-sources from ultra-wide binaries in the field. Such binaries experience perturbations from random stellar fly-bys which excite their eccentricities. Once a wide-binary is driven to a sufficiently small peri-center approach, GW-emission becomes significant, and the binary inspirals and merges. We derive an analytic model and verify it with numerical calculation to compute the merger rate to be ∼ 10×f wide Gpc −3 yr −1 (f wide is the fraction of wide BH-binaries), which is comparable to the observationally inferred rate. The observational signatures from this channel include spin-orbit misalignment; preference for high mass-ratio BBH; preference for high velocity-dispersion hostgalaxies; and a uniform delay-time distribution.

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“…Such perturbations may also be responsible for triggering white dwarf pollution in extra-solar systems (e.g., Veras et al 2014). In the stellar context, flybys may be important for producing low-mass X-ray binaries (Michaely & Perets 2016), or gravitational wave sources (Michaely & Perets 2019).…”

Section: Introductionmentioning

confidence: 99%

Analytic computation of the secular effects of encounters on a binary: features arising from second-order perturbation theory

Hamers

Samsing

2019

Monthly Notices of the Royal Astronomical Society

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Binary-single interactions play a crucial role in the evolution of dense stellar systems such as globular clusters. In addition, they are believed to drive black hole (BH) binary mergers in these systems. A subset of binary-single interactions are secular encounters, for which the third body approaches the binary on a relatively wide orbit, and such that it is justified to average the equations of motion over the binary's orbital phase. Previous works used firstorder perturbation theory to compute the effects of such secular encounters on the binary. However, this approach can break down for highly eccentric binaries, which are important for BH binary mergers and gravitational wave sources. Here, we present an analytic computation using second-order perturbation techniques, valid to the quadrupole-order approximation. In our calculation, we take into account the instantaneous back-reaction of the binary to the third body, and compute corrections to previous first-order results. Using singly-averaged and direct 3-body integrations, we demonstrate the validity of our expressions. In particular, we show that the eccentricity change for highly eccentric binaries can reach a plateau, associated with a large inclination change, and can even reverse sign. These effects are not captured by previous first-order results. We provide a simple script to conveniently evaluate our analytic expressions, including routines for numerical integration and verification. M R Binary j e Perturber Eccentricity E Periapsis distance Q CM θ x z Figure 1. Sketch of the configuration. A binary (center of mass 'CM') is perturbed by a passing object (mass M) on a parabolic or hyperbolic orbit (eccentricity E) with periapsis distance Q to the binary center of mass (Q > a, where a is the binary's semimajor axis).by Heggie & Rasio (1996) are commonly used to take into account the effects of (distant) encounters on a binary in Monte Carlo-style computations (e.g., Rasio & Heggie 1995; Spurzem et al. 2009;Geller et al. 2019).However, there are situations in which the first-order perturbation approach can break down. In Heggie & Rasio (1996), it was discussed that their method no longer applies if the eccentricity change is of the order of the initial eccentricity, i.e., ∆e ∼ e. However, as we will show here, when the binary is already highly eccentric, then the first-order approach can break down even if ∆e is small, in particular, if ∆e ∼ 1 − e. The latter can occur in highly eccentricity binaries perturbed by distant (i.e., weak) encounters, which can drive relatively large changes in the binary's orbital angular momentum. A binary can be driven to high eccentricities as a result of strong (non-secular) encounters in dense stellar systems. The breakdown of the first-order method originates from the fact that the binary's elements can change significantly during the passage of the perturber. Therefore, it is not justified to assume that these elements are constant when integrating the equations of motion.In this paper, we present an analytic compu...

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Tidal capture formation of low-mass X-ray binaries from wide binaries in the field

Cited by 39 publications

References 43 publications

MICRO-TIDAL DISRUPTION EVENTS BY STELLAR COMPACT OBJECTS AND THE PRODUCTION OF ULTRA-LONG GRBs

MICRO-TIDAL DISRUPTION EVENTS BY STELLAR COMPACT OBJECTS AND THE PRODUCTION OF ULTRA-LONG GRBs

Gravitational-wave Sources from Mergers of Binary Black Holes Catalyzed by Flyby Interactions in the Field

Analytic computation of the secular effects of encounters on a binary: features arising from second-order perturbation theory

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