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:0912.1201)
· References in the article
· Citations to the Article (24) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (4)
· NED Objects (1)
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Simulations of the grand design galaxy M51: a case study for analysing tidally induced spiral structure
Authors:
Dobbs, C. L.; Theis, C.; Pringle, J. E.; Bate, M. R.
Affiliation:
AA(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL), AB(Institute of Astronomy, University of Vienna, Türkenschanzstr. 17, 1180 Vienna, Austria), AC(Institute of Astronomy, Madingley Road, Cambridge CB3 0HA), AD(School of Physics, University of Exeter, Stocker Road, Exeter EX4 4QL)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 403, Issue 2, pp. 625-645. (MNRAS Homepage)
Publication Date:
04/2010
Origin:
WILEY
Astronomy Keywords:
hydrodynamics, ISM: clouds, galaxies: ISM, galaxies: kinematics and dynamics, galaxies: spiral, galaxies: structure
DOI:
10.1111/j.1365-2966.2009.16161.x
Bibliographic Code:
2010MNRAS.403..625D

Abstract

We present hydrodynamical models of the grand design spiral M51 (NGC 5194), and its interaction with its companion NGC 5195. Despite the simplicity of our models, our simulations capture the present-day spiral structure of M51 remarkably well, and even reproduce details such as a kink along one spiral arm, and spiral arm bifurcations. We investigate the offset between the stellar and gaseous spiral arms, and find at most times (including the present day) there is no offset between the stars and gas within our error bars. We also compare our simulations with recent observational analysis of M51. We compute the pattern speed versus radius, and similar to observations, find no single global pattern speed. We also show that the spiral arms cannot be fitted well by logarithmic spirals. We interpret these findings as evidence that M51 does not exhibit a quasi-steady density wave, as would be predicted by density wave theory. The internal structure of M51 derives from the complicated and dynamical interaction with its companion, resulting in spiral arms showing considerable structure in the form of short-lived kinks and bifurcations. Rather than trying to model such galaxies in terms of global spiral modes with fixed pattern speeds, it is more realistic to start from a picture in which the spiral arms, while not being simple material arms, are the result of tidally induced kinematic density `waves' or density patterns, which wind up slowly over time.
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