Optical Characteristics of X-Ray Binaries

Ilovaisky, S. A.

doi:10.1007/978-94-009-5337-6_9

Cited by 3 publications

(2 citation statements)

References 78 publications

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“…It thus seems reasonable to assume that accretion accounts for a substantial fraction of the quiescent X-ray luminosity in most NSXN. The optical variability of NSXN in quiescence (McClintock & Remillard 2000;Jain et al 2000;Ilovaisky & Chevalier 2000) provides ample evidence that accretion continues during quiescence.…”

Section: Discussionmentioning

confidence: 99%

New Evidence for Black Hole Event Horizons from [ITAL]Chandra[/ITAL]

Garcia

McClintock

Narayan

et al. 2001

The Astrophysical Journal

230

267

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Previously we claimed that Black Hole X-ray Novae (BHXN) in quiescence are much less luminous than equivalent Neutron Star X-ray Novae (NSXN). This claim was based on the quiescent detection of a single short period BHXN (A0620-00, P orb =7.8 hrs) and two longer period BHXN (GRO J1655-40, P orb =62.9 hrs; V404 Cyg, P orb =155.3 hrs), along with sensitive upper limits. We announce the detection of two more short period BHXN (GRO J0422+32, P orb =5.1 hrs; GS 2000+25, P orb =8.3 hrs), an upper limit for a third which is improved by two orders of magnitude (4U 1543-47, P orb =27.0 hrs) and a new, much lower quiescent measurement of GRO J1655-40. Taken together, these new Chandra measurements confirm that the quiescent X-ray luminosities of BHXN are significantly lower than those of NSXN. We argue that this provides strong evidence for the existence of event horizons in BHXN.

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Section: Discussionmentioning

confidence: 99%

New Evidence for Black Hole Event Horizons from [ITAL]Chandra[/ITAL]

Garcia

McClintock

Narayan

et al. 2001

The Astrophysical Journal

230

267

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“…As the top panel shows, there is a fairly large range of initial orbital periods (13 -18 hr) which leads to ultra-compact LMXBs with a minimum orbital period less than 30 min. Indeed, it is remarkable that one of our binary sequences, with an initial orbital period around 17 hr, appears to be a suitable sequence to explain all five LMXBs in globular clusters whose orbital periods are presently known, from the system with the longest period (AC211/X2127+119 in M15; P orb = 17.1 hr; Ilovaisky et al 1993) to the 11-min binary. Furthermore, systems with an initial period in the range of 13 -18 hr are quite naturally produced as a result of the tidal capture of a neutron star by a main-sequence star (Fabian, Pringle, & Rees 1975) and are not the generally expected outcome of a 3-or 4body exchange interaction (see, e.g., Rasio et al 2000;Rasio 2001).…”

Section: The Formation Of Ultra-compact Binariesmentioning

confidence: 92%

Binary Population Synthesis: Low- and Intermediate-Mass X-Ray Binarie

Podsiadlowski

Rappaport

Pfahl

2001

The Influence of Binaries on Stellar Population Studies

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As has only recently been recognized, X-ray binaries with intermediatemass secondaries are much more important than previously believed. To assess the relative importance of low-and intermediate-mass X-ray binaries (LMXBs and IMXBs), we have initiated a systematic study of these systems consisting of two parts: an exploration of the evolution of LMXBs and IMXBs for a wide range of initial masses and orbital periods using detailed binary stellar evolution calculations, and an integration of these results into a Monte-Carlo binary population synthesis code. Here we present some of the main results of our binary calculations and some preliminary results of the population synthesis study for a "standard" reference model. While the inclusion of IMXBs improves the agreement with the observed properties of "LMXBs", several significant discrepancies remain, which suggests that additional physical processes need to be included in the model. 1

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