5,360 research outputs found
Clumpy Ultracompact HII Regions I: Fully Supersonic Wind-blown Models
We propose that a significant fraction of the ultracompact HII regions found
in massive star-forming clouds are the result of the interaction of the wind
and ionizing radiation from a young massive star with the clumpy molecular
cloud gas in its neighbourhood. Distributed mass loading in the flow allows the
compact nebulae to be long-lived. In this paper, we discuss a particularly
simple case, in which the flow in the HII region is everywhere supersonic. The
line profiles predicted for this model are highly characteristic, for the case
of uniform mass loading. We discuss briefly other observational diagnostics of
these models.Comment: To appear in Monthly Notices of the Royal Astronomical Society. 5
pages LaTeX (uses mn.sty and epsf.sty macros) + 4 PS figures. Also available
via http://axp2.ast.man.ac.uk:8000/Preprints.htm
Asymptotic Level Spacing of the Laguerre Ensemble: A Coulomb Fluid Approach
We determine the asymptotic level spacing distribution for the Laguerre
Ensemble in a single scaled interval, , containing no levels,
E_{\bt}(0,s), via Dyson's Coulomb Fluid approach. For the
Unitary-Laguerre Ensemble, we recover the exact spacing distribution found by
both Edelman and Forrester, while for , the leading terms of
, found by Tracy and Widom, are reproduced without the use of the
Bessel kernel and the associated Painlev\'e transcendent. In the same
approximation, the next leading term, due to a ``finite temperature''
perturbation (\bt\neq 2), is found.Comment: 10pp, LaTe
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&
Distribution of the Riemann zeros represented by the Fermi gas
The multiparticle density matrices for degenerate, ideal Fermi gas system in
any dimension are calculated. The results are expressed as a determinant form,
in which a correlation kernel plays a vital role. Interestingly, the
correlation structure of one-dimensional Fermi gas system is essentially
equivalent to that observed for the eigenvalue distribution of random unitary
matrices, and thus to that conjectured for the distribution of the non-trivial
zeros of the Riemann zeta function. Implications of the present findings are
discussed briefly.Comment: 7 page
The tails in the Helix Nebula NGC 7293
We have examined a stream-source model for the production of the cometary
tails observed in the Helix Nebula NGC 7293 in which a transonic or moderately
supersonic stream of ionized gas overruns a source of ionized gas. Hydrodynamic
calculations reveal velocity structures which are in good agreement with the
observational data on tail velocities and are consistent with observations of
the nebular structure. The results also are indicative of a stellar atmosphere
origin for the cometary globules. Tail remnants persist for timescales long
enough for their identification with faint striations visible in the nebula gas
to be plausible.Comment: 7 pages, 6 figures, accepted for publication in A&
The Probability of an Eigenvalue Number Fluctuation in an Interval of a Random Matrix Spectrum
We calculate the probability to find exactly eigenvalues in a spectral
interval of a large random matrix when this interval contains eigenvalues on average. The calculations exploit an analogy to the
problem of finding a two-dimensional charge distribution on the interface of a
semiconductor heterostructure under the influence of a split gate.Comment: 4 pages, postscrip
The evolution of mass loaded supernova remnants: II. Temperature dependent mass injection rates
We investigate the evolution of spherically symmetric supernova remnants in which mass loading takes place due to conductively driven evaporation of embedded clouds. Numerical simulations reveal significant differences between the evolution of conductively mass loaded and the ablatively mass loaded remnants studied in Paper I. A main difference is the way in which conductive mass loading is extinguished at fairly early times, once the interior temperature of the remnant falls below ~ 107 K. Thus, at late times remnants that ablatively mass load are dominated by loaded mass and thermal energy, while those that conductively mass load are dominated by swept-up mass and kinetic energy. Simple approximations to the remnant evolution, complementary to those in Paper I, are given
Impact of localization on Dyson's circular ensemble
A wide variety of complex physical systems described by unitary matrices have
been shown numerically to satisfy level statistics predicted by Dyson's
circular ensemble. We argue that the impact of localization in such systems is
to provide certain restrictions on the eigenvalues. We consider a solvable
model which takes into account such restrictions qualitatively and find that
within the model a gap is created in the spectrum, and there is a transition
from the universal Wigner distribution towards a Poisson distribution with
increasing localization.Comment: To be published in J. Phys.
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