5,815 research outputs found
Starburst-driven galactic winds: I. Energetics and intrinsic X-ray emission
We have performed an extensive hydrodynamical parameter study of
starburst-driven galactic winds, motivated by the latest observation data on
the best-studied starburst galaxy M82. We study how the wind dynamics,
morphology and X-ray emission depend on the host galaxy's ISM distribution,
starburst star formation history and strength, and presence and distribution of
mass-loading by dense clouds. We find that the soft X-ray emission from
galactic winds comes from low filling factor (ff < 2 per cent) gas, which
contains only a small fraction (f < 10 per cent) of the mass and energy of the
wind, irrespective of whether the wind models are strongly mass-loaded or not.
X-ray observations of galactic winds therefore do not directly probe the gas
that contains the majority of the energy, mass or metal-enriched gas in the
outflow. The soft X-ray emission comes from gas at a wide range different
temperatures and densities. Estimates of the physical properties of the hot gas
in starburst galaxies, based on fitting the standard simple spectral models to
existing X-ray spectra, should therefore be treated with extreme suspicion. The
majority of the thermal and kinetic energy of these winds is in a volume
filling hot, T approx 10^7 K, component which is extremely difficult to probe
observationally due to its low density and hence low emissivity. Most of the
total energy is in the kinetic energy of this hot gas, a factor which must be
taken into account when attempting to constrain wind energetics
observationally. We also find that galactic winds are efficient at transporting
large amounts of energy out of the host galaxy, in contrast to their
inefficiency at transporting mass out of star-forming galaxies. (Abridged)Comment: Accepted for publication in MNRAS. Letter page size postscript
available from http://adcam.pha.jhu.edu/~dks/dks_published.htm
Predicting X-ray emission from wind-blown bubbles - Limitations of fits to ROSAT spectra
Wind-blown bubbles, from those around massive O and Wolf-Rayet stars, to
superbubbles around OB associations and galactic winds in starburst galaxies,
have a dominant role in determining the structure of the Interstellar Medium.
X-ray observations of these bubbles are particularly important as most of their
volume is taken up with hot gas, 1E5 < T (K) < 1E8. However, it is difficult to
compare X-ray observations, usually analysed in terms of single or two
temperature spectral model fits, with theoretical models, as real bubbles do
not have such simple temperature distributions. In this introduction to a
series of papers detailing the observable X-ray properties of wind-blown
bubbles, we describe our method with which we aim to solve this problem,
analysing a simulation of a wind-blown bubble around a massive star. We model a
wind of constant mass and energy injection rate, blowing into a uniform ISM,
from which we calculate X-ray spectra as would be seen by the ROSAT PSPC. We
compare the properties of the bubble as would be inferred from the ROSAT data
with the true properties of the bubble in the simulation. We find standard
spectral models yield inferred properties that deviate significantly from the
true properties, even though the spectral fits are statistically acceptable,
and give no indication that they do not represent to true spectral
distribution. Our results suggest that in any case where the true source
spectrum does not come from a simple single or two temperature distribution the
"observed" X-ray properties cannot naively be used to infer the true
properties.Comment: 14 pages, LaTeX with 13 eps figures, condensed abstract. MNRAS in
pres
Thermalization and the chromo-Weibel instability
Despite the apparent success of ideal hydrodynamics in describing the
elliptic flow data which have been produced at Brookhaven National Lab's
Relativistic Heavy Ion Collider, one lingering question remains: is the use of
ideal hydrodynamics at times t < 1 fm/c justified? In order to justify its use
a method for rapidly producing isotropic thermal matter at RHIC energies is
required. One of the chief obstacles to early isotropization/thermalization is
the rapid longitudinal expansion of the matter during the earliest times after
the initial nuclear impact. As a result of this expansion the parton
distribution functions become locally anisotropic in momentum space. In
contrast to locally isotropic plasmas anisotropic plasmas have a spectrum of
soft unstable modes which are characterized by exponential growth of transverse
chromo-magnetic/-electric fields at short times. This instability is the QCD
analogue of the Weibel instability of QED. Parametrically the chromo-Weibel
instability provides the fastest method for generation of soft background
fields and dominates the short-time dynamics of the system.Comment: 8 pages, 4 figures, Invited plenary talk given at the 19th
International Conference on Ultrarelativistic Nucleus-Nucleus Collisions:
Quark Matter 2006 (QM 2006), Shanghai, China, 14-20 Nov 200
Matching pre-equilibrium dynamics and viscous hydrodynamics
We demonstrate how to match pre-equilibrium dynamics of a 0+1 dimensional
quark gluon plasma to 2nd-order viscous hydrodynamical evolution. The matching
allows us to specify the initial values of the energy density and shear tensor
at the initial time of hydrodynamical evolution as a function of the lifetime
of the pre-equilibrium period. We compare two models for the pre-equilibrium
quark-gluon plasma, longitudinal free streaming and collisionally-broadened
longitudinal expansion, and present analytic formulas which can be used to fix
the necessary components of the energy-momentum tensor. The resulting dynamical
models can be used to assess the effect of pre-equilibrium dynamics on
quark-gluon plasma observables. Additionally, we investigate the dependence of
entropy production on pre-equilibrium dynamics and discuss the limitations of
the standard definitions of the non-equilibrium entropy.Comment: 24 pages, 5 figures,v2: minor modifications and updated references.
Accepted for publication in Phys. Rev.
The Energetics and Mass-loss of Mrk33
We present ROSAT HRI X-ray data and optical imaging of the important dwarf
starburst Markarian 33. We find an extended, complex, shell-like morphology in
the X-ray emission, with an extent of 2.3 x 1.9kpc, coincident with the bright
star-forming regions at the centre of the galaxy. The physical extent of this
X-ray emission from Mrk 33 is very similar to the observed Halpha emission, and
suggests that the bulk of the X-ray emission is coming from an expanding
superbubble.
We estimate the age and mass of Mrk 33's starburst to be 5.8 Myr and 6.9 x
10^{6} Msolar respectively with the energy injection rate in the central
regions of the galaxy being 10^{41} erg/s, while the associated mass-loss rate
from the star-forming regions is estimated to be 0.2 Msolar/yr. We suggest that
the X-ray emission is predominantly powered by starburst type activity and
argue that a blowout in the form of a galactic wind is the most likely fate for
Mrk 33 resulting in the loss of most of the galaxy's metal-enriched material
and a small fraction (<1 per cent) of the ISM.Comment: 13 pages, 6 figures, accepted for publication in MNRA
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