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:astro-ph/0602553)
· On-line Data
· References in the article
· Citations to the Article (3) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (4)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
A high-resolution ultraviolet absorption spectrum of supernova ejecta in SN1006
Authors:
Hamilton, Andrew J. S.; Fesen, Robert A.; Blair, William P.
Affiliation:
AA(JILA and Department Astrophysical & Planetary Sciences, Box 440, U. Colorado, Boulder, CO 80309, USA), AB(Dartmouth College, Hanover, NH 03755, USA), AC(Johns Hopkins University, Baltimore, MD 21218, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 381, Issue 2, pp. 771-778. (MNRAS Homepage)
Publication Date:
10/2007
Origin:
MNRAS
MNRAS Keywords:
shock waves, supernovae: individual: SN1006, supernova remnants, ultraviolet: stars
DOI:
10.1111/j.1365-2966.2007.12264.x
Bibliographic Code:
2007MNRAS.381..771H

Abstract

We report a high-resolution, far-ultraviolet, Space Telescope Imaging Spectrograph (STIS) E140M spectrum of the strong, broad SiII, III and IV features produced by the ejecta of the supernova of 1006 AD (SN1006) seen in absorption against the background Schweizer-Middleditch OB subdwarf star. The spectrum confirms the extreme sharpness of the red edge of the redshifted Si II 1260 Å feature, supporting the idea that this edge represents the location of the reverse shock moving into the freely expanding Si-rich ejecta. The expansion velocity of ejecta at the reverse shock is measured to be 7026 +/- 3(relative) +/-10(absolute) km s-1. If the shock model is correct, then the expansion velocity should be decreasing at the observable rate of 2.7 +/- 0.1 km s-1 yr-1. The pre-shock velocity, post-shock velocity and post-shock velocity dispersion are all measured from the Si II 1260 Å feature, and consistency of these velocities with the shock jump conditions implies that there is little or no electron heating in this fast (2680 km s-1) Si-rich shock; the 3σ upper limit on the fraction of shock energy that goes into electron heating is 0.26.
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