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)
· Full Refereed Scanned Article (GIF)
· arXiv e-print (arXiv:astro-ph/0602466)
· References in the article
· Citations to the Article (11) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (5)
· NED Objects (2)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Tracing gas motions in the Centaurus cluster
Authors:
Graham, J.; Fabian, A. C.; Sanders, J. S.; Morris, R. G.
Affiliation:
AA(Institute of Astronomy, Madingley Road, Cambridge), AB(Institute of Astronomy, Madingley Road, Cambridge), AC(Institute of Astronomy, Madingley Road, Cambridge), AD(Institute of Astronomy, Madingley Road, Cambridge; Kavli Institute for Particle Astrophysics and Cosmology, Stanford Linear Accelerator Centre, Stanford, CA 94305-4060, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 368, Issue 3, pp. 1369-1376. (MNRAS Homepage)
Publication Date:
05/2006
Origin:
MNRAS
MNRAS Keywords:
galaxies: clusters: general: galaxies: clusters: individual: Centaurus: cooling flows, galaxies: clusters: general, galaxies: clusters: individual: Centaurus, cooling flows
DOI:
10.1111/j.1365-2966.2006.10218.x
Bibliographic Code:
2006MNRAS.368.1369G

Abstract

We apply the stochastic model of iron transport developed by Rebusco et al. to the Centaurus cluster. Using this model, we find that an effective diffusion coefficient D in the range 2 × 1028-4 × 1028cm2s-1 can approximately reproduce the observed abundance distribution. Reproducing the flat central profile and sharp drop around 30-70kpc, however, requires a diffusion coefficient that drops rapidly with radius so that D > 4 × 1028cm2s-1 only inside about 25kpc. Assuming that all transport is due to fully developed turbulence, which is also responsible for offsetting cooling in the cluster core, we calculate the length- and velocity-scales of energy injection. These length-scales are found to be up to a factor of ~10 larger than expected if the turbulence is due to the inflation and rising of a bubble. We also calculate the turbulent thermal conductivity and find it is unlikely to be significant in preventing cooling.

Printing Options

Print whole paper
Print Page(s) through

Return 600 dpi PDF to Acrobat/Browser. Different resolutions (200 or 600 dpi), formats (Postscript, PDF, etc), page sizes (US Letter, European A4, etc), and compression (gzip,compress,none) can be set through the Printing Preferences


More Article Retrieval Options

HELP for Article Retrieval
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