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

By Elke Roediger, Gerhard Hensler. 2005

152 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a6e60a11c92d773cec678a195ebb172b68a00db3

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

The effect of ram pressure on the star formation, mass distribution and morphology of galaxies (2009, background): “The dependence of the stripping radius on the external ram pressure and the galaxy properties was investigated (e.g. Abadi et al. 1999; Vollmer et al. 2001; Roediger & Hensler 2005) and a remarkable agreement between analytical estimates and numerical simulations was found.”
Environmental effects on satellite galaxies: the link between concentration, size and colour profile (2008, background): “Roediger & Hensler (2005) claim that a galaxy with a mass of 8×1010M⊙ loses all its gas down to a radius of 9 kpc if subject to such ram-pressure for 400 Myr.”
GAS STRIPPING IN SIMULATED GALAXIES WITH A MULTIPHASE INTERSTELLAR MEDIUM (2009, methodology): “Although the stability of this galaxy model is discussed in detail in Roediger & Hensler (2005) and Roediger & Brüggen (2006), it is important to reiterate that using Enzo, the galaxies are stable if there is no radiative cooling and no ICM wind.”
Simultaneous ram pressure and tidal stripping; how dwarf spheroidals lost their gas (2005, methodology): “The results of the WT runs also compare well with those of Roediger & Hensler (2005) which were obtained for larger galaxies being subject to ram pressure forces appropriate for low-density environments as those considered here.”
Quenching and ram pressure stripping of simulated Milky Way satellite galaxies (2017, background): “…gas can be expressed as Prest = ∣∣∣ ∂Φ∂zh ∣∣∣max Σgas, where Σgas is the satellite’s gas surface density, zh is the direction of motion (and gas dis- placement), Φ is the gravitational potential, and ∣∣∣ ∂Φ∂zh ∣∣∣max the the maximum of the derivative of Φ along zh (Roediger & Hensler 2005).”
LoCuSS: THE SLOW QUENCHING OF STAR FORMATION IN CLUSTER GALAXIES AND THE NEED FOR PRE-PROCESSING (2015, background): “The effective timescale for quenching via ram-pressure stripping then becomes the ∼1 Gyr required for galaxies to travel from the cluster outskirts to the pericenter where the peak in ram pressure occurs (Roediger & Hensler 2005).”
A REVISED PARALLEL-SEQUENCE MORPHOLOGICAL CLASSIFICATION OF GALAXIES: STRUCTURE AND FORMATION OF S0 AND SPHEROIDAL GALAXIES (2011, background): “…observations and theoretical developments both suggest that ram-pressure stripping is more effective than we have thought (Mori & Burkert 2000; Quilis et al. 2000; Grebel et al. 2003; Roediger & Hensler 2005; Tonnesen et al. 2007, 2008, 2009, 2010; Boselli et al. 2008; van Gorkom & Kenney 2011).”
Hα Tail, Intracluster H II Regions, and Star Formation: ESO 137-001 in Abell 3627 (2007, methodology): “Compared with simulations by Roediger & Hensler (2005), over 90% of the gas in the original gas disk should have been removed from the disk, either hanging up in the halo or in the tail.”
Ram pressure stripping of disc galaxies orbiting in clusters – I. Mass and radius of the remaining gas disc (2007, methodology): “…simulations of RPS presented so far (Abadi et al. 1999, Quilis et al. 2000, Schulz & Struck 2001 (SS01), Marcolini et al. 2003 (MBD03), Roediger & Hensler 2005 (RH05), Roediger & Brüggen 2006 (RB06)) suggest that this analytical estimate does indeed do a fair job as long as the…”