Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Full Refereed Journal Article (PDF/Postscript)
· Full Refereed Scanned Article (GIF)
· arXiv e-print (arXiv:astro-ph/0602042)
· References in the article
· Citations to the Article (17) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (4)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Collisions and close encounters involving massive main-sequence stars
Authors:
Dale, James E.; Davies, Melvyn B.
Affiliation:
AA(Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH), AB(Lund Observatory, Box 43, SE-221 00 Lund, Sweden)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 366, Issue 4, pp. 1424-1436. (MNRAS Homepage)
Publication Date:
03/2006
Origin:
MNRAS
Astronomy Keywords:
blue stragglers, supernovae: general, gamma-rays: bursts
DOI:
10.1111/j.1365-2966.2005.09937.x
Bibliographic Code:
2006MNRAS.366.1424D

Abstract

We study close encounters involving massive main-sequence stars and the evolution of the exotic products of these encounters as common-envelope systems or possible hypernova progenitors. We show that parabolic encounters between low- and high-mass stars and between two high-mass stars with small periastrons result in mergers on time-scales of a few tens of stellar free-fall times (a few tens of hours). We show that such mergers of unevolved low-mass stars with evolved high-mass stars result in little mass-loss (~0.01Msolar) and can deliver sufficient fresh hydrogen to the core of the collision product to allow the collision product to burn for several million years. We find that grazing encounters enter a common-envelope phase which may expel the envelope of the merger product. The deposition of energy in the envelopes of our merger products causes them to swell by factors of ~100. If these remnants exist in very densely populated environments (n>~ 107pc-3), they will suffer further collisions which may drive off their envelopes, leaving behind hard binaries. We show that the products of collisions have cores rotating sufficiently rapidly to make them candidate hypernova/gamma-ray burst progenitors and that ~0.1 per cent of massive stars may suffer collisions, sufficient for such events to contribute significantly to the observed rates of hypernovae and gamma-ray bursts.

Printing Options

Send high resolution image to Level 2 Postscript Printer
Send low resolution image to Level 2 Postscript Printer
Send low resolution image to Level 1 Postscript Printer
Get high resolution PDF image
Get low resolution PDF
Send 300 dpi image to PCL Printer
Send 150 dpi image to PCL Printer

More Article Retrieval Options

HELP for Article Retrieval
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
  New!

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