Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997ap%26ss.254..233i&link_type=abstract
Astrophysics and Space Science, v. 254, Issue 2, p. 233-251 (1997).
Astronomy and Astrophysics
Astrophysics
4
Scientific paper
Time-dependent, X-ray emission properties of merging subclusters of galaxies are studied by N-body + Hydrodynamic simulations. We consider rather idealized cases, in which two virialized subclusters with the same or different masses collide with each other, eventually merging into one bigger cluster. We find that the various observable quantities, such as the cluster temperature, Tg, the line-of-sight velocity dispersion of galaxies, σ1, and the specific energy ratio, βspec ≡ µ mp σ_1^2 /kB Tg (where µ is the mean molecular weight in amu, mp is the proton mass and kB is the Boltzmann constant) are distinct in merging clusters from those in isolated clusters. When merging, especially, in addition to having large velocity dispersions, σl ≳ 2000 km s-1, clusters will have large deviations of βspec from unity; that is, βspec ≳ 2.0 (or βspec ≲ 0.5) when seen from the direction parallel (perpendicular) to the collision axis. Temperature profiles are the best indicator of merging process. The calculated temperature maps of merging clusters are compared with those of the observed clusters, such as the Coma cluster, A754, and A401/399 supercluster. These simulated features are in good agreement with what ASCA revealed. Further, we present rather unique features in the temperature profiles that can be caused by a merger (or an encounter) with a subgroup of galaxies.
No associations
LandOfFree
On the βSPEC Values of Galaxy Clusters During the Merger does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with On the βSPEC Values of Galaxy Clusters During the Merger, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and On the βSPEC Values of Galaxy Clusters During the Merger will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1179107