Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:0705.4223)
· References in the article
· Citations to the Article (5) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (6)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Predictions for triple stars with and without a pulsar in star clusters
Authors:
Trenti, Michele; Ransom, Scott; Hut, Piet; Heggie, Douglas C.
Affiliation:
AA(Space Telescope Science Institute, Baltimore, MD 21210, USA), AB(National Radio Astronomy Observatory, 520 Edgemont Rd., Charlottesville, VA 22903, USA), AC(Institute for Advanced Study, Princeton, NJ 08540, USA), AD(School of Mathematics and Maxwell Institute of Mathematical Sciences, University of Edinburgh, King's Buildings, Edinburgh EH9 3JZ)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 387, Issue 2, pp. 815-824. (MNRAS Homepage)
Publication Date:
06/2008
Origin:
MNRAS
MNRAS Keywords:
stellar dynamics , methods: N-body simulations , pulsars: general , globular clusters: general
DOI:
10.1111/j.1365-2966.2008.13285.x
Bibliographic Code:
2008MNRAS.387..815T

Abstract

Though about 80 pulsar binaries have been detected in globular clusters so far, no pulsar has been found in a triple system in which all three objects are of comparable mass. Here, we present predictions for the abundance of such triple systems, and for the most likely characteristics of these systems. Our predictions are based on an extensive set of more than 500 direct simulations of star clusters with primordial binaries, and a number of additional runs containing primordial triples. Our simulations employ a number Ntot of equal-mass stars from Ntot = 512 to 19661 and a primordial binary fraction from 0 to 50 per cent. In addition, we validate our results against simulations with N = 19661 that include a mass spectrum with a turn-off mass at 0.8Msolar, appropriate to describe the old stellar populations of Galactic globular clusters. Based on our simulations, we expect that typical triple abundances in the core of a dense cluster are two orders of magnitude lower than the binary abundances, which in itself already suggests that we do not have to wait too long for the first comparable-mass triple with a pulsar to be detected.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints