199 research outputs found
Magnetic ionization fronts II: Jump conditions for oblique magnetization
We present the jump conditions for ionization fronts with oblique magnetic
fields. The standard nomenclature of R- and D-type fronts can still be applied,
but in the case of oblique magnetization there are fronts of each type about
each of the fast- and slow-mode speeds. As an ionization front slows, it will
drive first a fast- and then a slow-mode shock into the surrounding medium.
Even for rather weak upstream magnetic fields, the effect of magnetization on
ionization front evolution can be important. [Includes numerical MHD models and
an application to observations of S106.]Comment: 9 pages, 10 figures, Latex, to be published in MNRA
Generation of density inhomogeneities by magnetohydrodynamic waves in two dimensions
Using two dimensional simulations, we study the formation of structures with
a high-density contrast by magnetohydrodynamic waves in regions in which the
ratio of thermal to magnetic pressure is small. The initial state is a uniform
background perturbed by fast-mode wave. Our most significant result is that
dense structures persist for far longer in a two-dimensional simulation than in
the one-dimensional case. Once formed, these structures persist as long as the
fast-mode amplitude remains high.Comment: 6 pages, 7 figures, accepted by MNRA
A Laboratory Investigation of Supersonic Clumpy Flows: Experimental Design and Theoretical Analysis
We present a design for high energy density laboratory experiments studying
the interaction of hypersonic shocks with a large number of inhomogeneities.
These ``clumpy'' flows are relevant to a wide variety of astrophysical
environments including the evolution of molecular clouds, outflows from young
stars, Planetary Nebulae and Active Galactic Nuclei. The experiment consists of
a strong shock (driven by a pulsed power machine or a high intensity laser)
impinging on a region of randomly placed plastic rods. We discuss the goals of
the specific design and how they are met by specific choices of target
components. An adaptive mesh refinement hydrodynamic code is used to analyze
the design and establish a predictive baseline for the experiments. The
simulations confirm the effectiveness of the design in terms of articulating
the differences between shocks propagating through smooth and clumpy
environments. In particular, we find significant differences between the shock
propagation speeds in a clumpy medium compared to a smooth one with the same
average density. The simulation results are of general interest for foams in
both inertial confinement fusion and laboratory astrophysics studies. Our
results highlight the danger of using average properties of inhomogeneous
astrophysical environments when comparing timescales for critical processes
such as shock crossing and gravitational collapse times.Comment: 7 pages, 6 figures. Submitted to the Astrophysical Journal. For
additional information, including simulation animations and the pdf and ps
files of the paper with embedded high-quality images, see
http://pas.rochester.edu/~wm
Shock-triggered formation of magnetically-dominated clouds
To understand the formation of a magnetically dominated molecular cloud out
of an atomic cloud, we follow the dynamical evolution of the cloud with a
time-dependent axisymmetric magnetohydrodynamic code. A thermally stable warm
atomic cloud is initially in static equilibrium with the surrounding hot
ionised gas. A shock propagating through the hot medium interacts with the
cloud. As a fast-mode shock propagates through the cloud, the gas behind it
becomes thermally unstable. The value of the gas also becomes much
smaller than the initial value of order unity. These conditions are ideal for
magnetohydrodynamic waves to produce high-density clumps embedded in a rarefied
warm medium. A slow-mode shock follows the fast-mode shock. Behind this shock a
dense shell forms, which subsequently fragments. This is a primary region for
the formation of massive stars. Our simulations show that only weak and
moderate-strength shocks can form cold clouds which have properties typical of
giant molecular clouds.Comment: 7 pages, 6 figures, accepted by Astronomy and Astrophysic
H3+ in Diffuse Interstellar Clouds: a Tracer for the Cosmic-Ray Ionization Rate
Using high resolution infrared spectroscopy we have surveyed twenty
sightlines for H3+ absorption. H3+ is detected in eight diffuse cloud
sightlines with column densities varying from 0.6x10^14 cm^-2 to 3.9x10^14
cm^-2. This brings to fourteen the total number of diffuse cloud sightlines
where H3+ has been detected. These detections are mostly along sightlines
concentrated in the Galactic plane, but well dispersed in Galactic longitude.
The results imply that abundant H3+ is common in the diffuse interstellar
medium. Because of the simple chemistry associated with H3+ production and
destruction, these column density measurements can be used in concert with
various other data to infer the primary cosmic-ray ionization rate, zeta_p.
Values range from 0.5x10^-16 s^-1 to 3x10^-16 s^-1 with an average of 2x10^-16
s^-1. Where H3+ is not detected the upper limits on the ionization rate are
consistent with this range. The average value of zeta_p is about an order of
magnitude larger than both the canonical rate and rates previously reported by
other groups using measurements of OH and HD. The discrepancy is most likely
due to inaccurate measurements of rate constants and the omission of effects
which were unknown when those studies were performed. We believe that the
observed column density of H3+ is the most direct tracer for the cosmic-ray
ionization rate due to its simple chemistry. Recent models of diffuse cloud
chemistry require cosmic-ray ionization rates on the order of 10^-16 s^-1 to
reproduce observed abundances of various atomic and molecular species, in rough
accord with our observational findings.Comment: Accepted to ApJ, 35 pages, 5 figures, 5 table
The Thermal Stability of Mass-Loaded Flows
We present a linear stability analysis of a flow undergoing
conductively-driven mass-loading from embedded clouds. We find that
mass-loading damps isobaric and isentropic perturbations, and in this regard is
similar to the effect of thermal conduction, but is much more pronounced where
many embedded clumps exist. The stabilizing influence of mass-loading is
wavelength independent against isobaric (condensing) perturbations, but
wavelength dependent against isentropic (wave-like) perturbations. We derive
equations for the degree of mass-loading needed to stabilize such
perturbations. We have also made 1D numerical simulations of a mass-loaded
radiative shock and demonstrated the damping of the overstability when
mass-loading is rapid enough.Comment: 4 pages, 1 figure, to be published in A&
The Formation of Broad Emission Line Regions in Supernova-QSO Wind Interactions
We show that a cooled region of shocked supernova ejecta forms in a type II
supernova-QSO wind interaction, and has a density, an ionization parameter, and
a column density compatible with those inferred for the high ionization
component of the broad emission line regions in QSOs. The calculations are
based on the assumption that the ejecta flow is described initially by a
similarity solution investigated by Chevalier (1982) and Nadyozhin (1985) and
is spherically symmetric. Heating and cooling appropriate for gas irradiated by
a nearby powerful continuum source is included in our model, together with
reasonable assumptions for the properties of the QSO wind. The model results
are also in agreement with observational correlations and imply reasonable
supernova rates.Comment: 13 pages, 7 figures, to be published in A&
Self-Similar Evolution of Wind-Blown Bubbles with Mass-loading by Conductive Evaporation
We present similarity solutions for mass-loaded adiabatic bubbles that are
blown by winds having time dependent mechanical luminosities. We consider
mass-loading through conductive evaporation of clumps. In the limit of little
mass loading a similarity solution found by Dyson (1973) for expansion into a
smooth ambient medium is recovered. We find that the Mach number in the shocked
mass-loaded wind shows a radial dependence that varies qualitatively from
solution to solution. In some cases it is everywhere less than unity in the
frame of the clumps being evaporated, while in others it is everywhere greater
than unity. In some solutions the mass-loaded shocked wind undergoes one or two
sonic transitions in the clump frame. Maximum possible values of the ratio of
evaporated mass to stellar wind mass are found as a consequence of the
evaporation rates dependence on temperature and the lowering of the temperature
by mass-loading. Mass-loading tends to reduce the emissivity in the interior of
the bubble relative to its limb, whilst simultaneously increasing the central
temperature relative to the limb temperature.Comment: 12 pages, 8 figures, accepted for publication by A&
On the Energy Required to Eject Processed Matter from Galaxies
We evaluate the minimum energy input rate that starbursts require for
expelling their newly processed matter from their host galaxies. Special
attention is given to the pressure caused by the environment in which a galaxy
is situated, as well as to the intrinsic rotation of the gaseous component. We
account for these factors and for a massive dark matter distribution, and
develop a self-consistent solution for the interstellar matter gas
distribution. Our results are in excellent agreement with the results of Mac
Low & Ferrara (1999) for galaxies with a flattened disk-like ISM density
distribution and a low intergalactic gas pressure ( 1
cm K). However, our solution also requires a much larger energy input
rate threshold when one takes into consideration both a larger intergalactic
pressure and the possible existence of a low-density, non-rotating, extended
gaseous halo component.Comment: 7 pages, 4 figures, 1 table, Accepted for publication in Ap
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