2005A&A...433..875R


C.D.S. - SIMBAD4 rel 1.7 - 2021.03.04CET23:58:03

2005A&A...433..875R - Astronomy and Astrophysics, volume 433, 875-895 (2005/4-3)

Ram pressure stripping of disk galaxies. From high to low density environments.

ROEDIGER E. and HENSLER G.

Abstract (from CDS):

Galaxies in clusters and groups moving through the intracluster or intragroup medium (abbreviated ICM for both) are expected to lose at least a part of their interstellar medium (ISM) by the ram pressure they experience. We perform high resolution 2D hydrodynamical simulations of face-on ram pressure stripping (RPS) of disk galaxies to compile a comprehensive parameter study varying galaxy properties (mass, vertical structure of the gas disk) and covering a large range of ICM conditions, reaching from high density environments like in cluster centres to low density environments typical for cluster outskirts or groups. We find that the ICM-ISM interaction proceeds in three phases: firstly the instantaneous stripping phase, secondly the dynamic intermediate phase, thirdly the quasi-stable continuous viscous stripping phase. In the first phase (time scale 20 to 200Myr) the outer part of the gas disk is displaced but only partially unbound. In the second phase (10 times as long as the first phase) a part of the displaced gas falls back (about 10% of the initial gas mass) despite the constant ICM wind, but most displaced gas is now unbound. In the third phase the galaxy continues to lose gas at a rate of about 1M/yr by turbulent viscous stripping. We find that the stripping efficiency depends slightly on the Mach number of the flow, however, the main parameter is the ram pressure. The stripping efficiency does not depend on the vertical structure and thickness of the gas disk. We discuss uncertainties in the classic estimate of the stripping radius of Gunn & Gott (1972ApJ...176....1G), which compares the ram pressure to the gravitational restoring force. In addition, we adapt the estimate used by Mori & Burkert (2000ApJ...538..559M) for spherical galaxies, namely the comparison of the central pressure with ram pressure. We find that the latter estimate predicts the radius and mass of the gas disk remaining at the end of the second phase very well, and better than the Gunn & Gott (1972ApJ...176....1G) criterion. From our simulations we conclude that gas disks of galaxies in high density environments are heavily truncated or even completely stripped, but also the gas disks of galaxies in low density environments are disturbed by the flow and back-falling material, so that they should also be pre-processed.

Abstract Copyright:

Journal keyword(s): galaxies: spiral - galaxies: evolution - galaxies: ISM - galaxies clusters: general

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 4402 GiP 12 26 07.566 +13 06 46.06   12.55       ~ 364 1
2 NAME Vir I ClG 12 26 32.1 +12 43 24   10.00 8.49     ~ 5986 0
3 NGC 4522 GiG 12 33 39.657 +09 10 29.54   13.6       ~ 334 0
4 M 91 LIN 12 35 26.430 +14 29 46.75   14.63 13.57     ~ 534 0
5 M 90 Sy2 12 36 49.816 +13 09 46.33 10.56 10.26 9.54     ~ 810 1
6 NGC 4848 AGN 12 58 05.5774186519 +28 14 33.264194270   14.2   13.53   ~ 175 0

    Equat.    Gal    SGal    Ecl

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2021.03.04-23:58:03

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