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/0207576)
· References in the article
· Citations to the Article (65) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
· HEP/Spires Information
·
· Translate This Page
Title:
Jets, winds and bursts from coalescing neutron stars
Authors:
Rosswog, Stephan; Ramirez-Ruiz, Enrico
Affiliation:
AA(Department of Physics and Astronomy, University of Leicester, Leicester LE1 7RH), AB(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA)
Publication:
Monthly Notice of the Royal Astronomical Society, Volume 336, Issue 1, pp. L7-L11. (MNRAS Homepage)
Publication Date:
10/2002
Origin:
MNRAS
Astronomy Keywords:
dense matter, hydrodynamics, neutrinos, methods: numerical, stars: neutron, gamma-rays: bursts
DOI:
10.1046/j.1365-8711.2002.05898.x
Bibliographic Code:
2002MNRAS.336L...7R

Abstract

Recent high-resolution calculations of neutron star coalescences are used to investigate whether annihilation can provide sufficient energy to power gamma-ray bursts, especially those belonging to the short duration category. Late time slices of the simulations, where the neutrino emission has reached a maximum, stationary level are analysed to address this question. We find that annihilation can provide the necessary driving stresses that lead to relativistic jet expansion. Maximum Lorentz factors of the order of 15 are found along the binary rotation axis, but larger values are expected to arise from higher numerical resolution. Yet the accompanying neutrino-driven wind must be absent from the axis when the burst occurs or prohibitive baryon loading may occur. We argue that even under the most favourable conditions, annihilation is unlikely to power a burst in excess of ~1048 erg. Unless the emission is beamed into less than one per cent of the solid angle, which we argue is improbable if it is collimated by gas pressure, this may fail to satisfy the apparent isotropic energies inferred at cosmological distances. This mechanism may none the less drive a precursor fireball, thereby evacuating a cavity into which a later magnetically driven jet could expand. A large range of time delays between the merger and the black hole formation are to be expected. If the magnetically driven jet occurs after the black hole has formed, a time span as long as weeks could pass between the neutrino powered precursor and the magnetically driven GRB.

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