scholarly journals Abundance ratios in stars vs. hot gas in elliptical galaxies

2009 ◽  
Vol 5 (H15) ◽  
pp. 281-281
Author(s):  
Antonio Pipino
Keyword(s):  
Interstellar Medium ◽  
Chemical Evolution ◽  
Elliptical Galaxies ◽  
Evolution Model ◽  
X Ray ◽  
Galactic Wind ◽  
Hot Gas ◽  
Self Consistent ◽  
Chemical Evolution Model ◽  
Gas Properties

AbstractI present predictions from a chemical evolution model for a self-consistent study of optical (i.e., stellar) and X-ray (i.e., gas) properties of present-day elliptical galaxies. Detailed cooling and heating processes in the interstellar medium are taken into account and allow a reliable modelling of the SN-driven galactic wind. The model simultaneously reproduces the mass-metallicity, colour-magnitude, LX - LB and LX - T relations, and the observed trend of [Mg/Fe] with σ. The "iron discrepancy" can be solved by taking into account the dust presence.

scholarly journals Hot gas morpoloy, thermal structure, and the AGN connection in elliptical galaxies

2009 ◽  
Vol 5 (H15) ◽  
pp. 275-276
Author(s):  
Thomas S. Statler ◽  
Steven Diehl
Keyword(s):  
Interstellar Medium ◽  
Thermal Structure ◽  
Elliptical Galaxies ◽  
Temperature Gradients ◽  
Fundamental Plane ◽  
Nuclear Activity ◽  
X Ray ◽  
Hot Gas ◽  
Gas Properties

AbstractRecent studies of the hot interstellar medium in normal elliptical galaxies have shown that (1) the gas is only approximately hydrostatic; (2) morphological disturbances are corrleated with radio and X-ray signatures of AGN; and (3) temperature gradients in the main bodies of the galaxies are correlated with nuclear activity but not with environment. An X-ray Gas Fundamental Plane (XGFP), unrelated to the stellar fundamental plane, links the global gas properties in a relation whose origin is not yet understood.

scholarly journals The Enrichment of the Intracluster Medium

1996 ◽  
Vol 171 ◽  
pp. 381-381
Author(s):  
B.K. Gibson ◽  
F. Matteucci
Keyword(s):  
Chemical Evolution ◽  
Dwarf Galaxy ◽  
Observational Evidence ◽  
Intracluster Medium ◽  
X Ray ◽  
Galactic Wind ◽  
Galactic Winds ◽  
Luminosity Functions ◽  
Self Consistent

Recent observational evidence for steep dwarf galaxy luminosity functions in several rich clusters has led to speculation that their precursors, via supernovae (SNe)-driven galactic winds, may be the source of the majority of gas and metals inferred from intracluster medium (ICM) x-ray observations (Trentham 1994). Utilising a fully self-consistent photo-chemical evolution package (Gibson 1995), and insisting that the post-galactic wind dwarfs obey the observed colour-luminosity-metallicity relations, we demonstrate that the bulk of the ICM gas does not originate within their precursors (Gibson & Matteucci 1995).

scholarly journals Chandra X-ray Observations of Dwarf Starburst Galaxies

2004 ◽  
Vol 217 ◽  
pp. 304-309
Author(s):  
Jürgen Ott ◽  
Fabian Walter ◽  
Elias Brinks ◽  
Ulrich Klein
Keyword(s):  
Interstellar Medium ◽  
Gravitational Potential ◽  
Thermal Plasma ◽  
Theoretical Models ◽  
Starburst Galaxies ◽  
Host Galaxy ◽  
X Ray ◽  
Hot Gas ◽  
Neutral Gas

We obtained X-ray observations for a sample of eight nearby dwarf starburst galaxies from the Chandra X-ray Observatory. Five galaxies of our sample show extended (size: 1-10 kpc), diffuse X-ray emission which can be attributed to a hot thermal plasma. This phase of the interstellar medium purportedly drives the expansion of supergiant shells. A comparison of the derived gas parameters with theoretical models reveals that the hot gas in principle is capable to escape from the gravitational potential of the host galaxy. However, the outflows appear to be contained in those cases where an extended envelope or massive tidal features of neutral gas exist.

scholarly journals A Chemical Evolution Model for the Fornax Dwarf Spheroidal Galaxy

2016 ◽  
Vol 109 ◽  
pp. 02002 ◽  
Author(s):  
Zhen Yuan ◽  
Yong-Zhong Qian ◽  
Yi Peng Jing
Keyword(s):  
Chemical Evolution ◽  
Evolution Model ◽  
Chemical Evolution Model

scholarly journals Evolution of Multiphase Hot Interstellar Medium in Elliptical Galaxies

1998 ◽  
Vol 188 ◽  
pp. 281-282
Author(s):  
Y. Fujita ◽  
J. Fukumoto ◽  
K. Okoshi
Keyword(s):  
Interstellar Medium ◽  
Supernova Remnants ◽  
Elliptical Galaxies ◽  
Galactic Wind ◽  
Long Time

Theoretical arguments indicate that the ISM is inhomogeneous; Mathews estimated that the ~ 1M⊙ of metal ejected by each supernova event into the ISM is trapped locally within the hot bubbles. Since in elliptical galaxies, there is no overlapping of expanding supernova remnants after galactic wind period, it is expected that this inhomogeneity persists for a long time. The observations also suggests that the ISM of elliptical galaxies is inhomogeneous. Based on these arguments, we studied the evolution of the multiphase (inhomogeneous) ISM.

scholarly journals Chempy: A flexible chemical evolution model for abundance fitting

2017 ◽  
Vol 605 ◽  
pp. A59 ◽  
Author(s):  
Jan Rybizki ◽  
Andreas Just ◽  
Hans-Walter Rix
Keyword(s):  
Chemical Evolution ◽  
Evolution Model ◽  
Chemical Evolution Model

scholarly journals Interstellar Scintillation of Radio Sources as a Probe for Investigations of the Local Interstellar Medium

1997 ◽  
Vol 166 ◽  
pp. 215-218
Author(s):  
N. Bochkarev ◽  
M. Ryabov
Keyword(s):  
Interstellar Medium ◽  
Small Scale ◽  
Radio Sources ◽  
Local Interstellar Medium ◽  
Star Formation Region ◽  
X Ray ◽  
Extragalactic Radio Sources ◽  
Hot Gas ◽  
The North ◽  
Scintillation Indices

AbstractA possibility of obtaining information on small scale inhomogeneities of the electron component of the local interstellar medium (LISM) is investigated using interstellar scintillations of extragalactic radio sources. We analyse Culgoora array observational data on variability of 190 extragalactic radio sources, covering most of the sky, at 80 and 160 MHz. The variability at time scales from 1 month to 15 years is interpreted as refractive interstellar scintillations in fast-moving nearby (less than 150 pc) hot gas near shock waves in the LISM. All-sky map of scintillation indices m averaged over 3–5 sources closest to one another shows several m maxima. Two of the 3 most pronounced maxima are probably connected with Loop I; the third one coincides with the soft X-ray (0.1–0.3 keV) background maximum near the South Galactic Pole. Other, less certain, m maxima probably correspond to the Orion star-formation region and to a soft X-ray maximum near the North Galactic Pole. The ”free-of-gas” tunnel in the direction l = 240° corresponds to low values of m. The estimated time scale of interstellar scintillations on the above-mentioned LISM structures is in agreement with that of the observed radio-source variations.

scholarly journals 3D gas dynamics in triaxial systems

1993 ◽  
Vol 153 ◽  
pp. 273-274
Author(s):  
D. Friedli ◽  
S. Udry
Keyword(s):  
Gas Dynamics ◽  
Elliptical Galaxies ◽  
Stellar Systems ◽  
Gas Temperature ◽  
3D Simulations ◽  
Hot Gas ◽  
Chaotic Orbits ◽  
Self Consistent ◽  
Triaxial Stellar Systems ◽  
Pattern Speed

Depending on the nature of the various components (stars, gas) present in triaxial stellar systems (elliptical galaxies, bulges and bars), the dynamics is expected to be rather different. The stars are collisionless, dissipationless, and dynamically hot; they are mainly trapped by quasi-periodic or chaotic orbits. On the contrary, the gas is collisional, dissipational, and dynamically cold; the cold or warm gas (≲ 104 K) is a powerful orbital tracer, however shocks prevent it from following self-crossing orbits. The hot gas (≲ 106 K) is influenced by “repulsive” pressure forces which prevent in close encounters the flow from being strongly shocked; it rather follows chaotic trajectories. By means of fully self-consistent 3D simulations with stars and gas using PM (Pfenniger & Friedli 1992) and SPH (Friedli & Benz 1992) techniques, we investigate the response of gaseous components in the following situations: 1) slow or fast pattern speed Ωp, 2) direct or retrograde gas motion with respect to the stars, and 3) warm or hot gas temperature T. Initial parameters and final characteristics of each runs are reported in Table I.

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