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Astrophysics astro-ph new abstracts 25 August 2000

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August 25, 2000
Filed under

Astrophysics


astro-ph new abstracts, Fri, 25 Aug 00 04:00:12 GMT
0008376 — 0008391 received




astro-ph/0008376 [abs, src, ps, other] :




Title: Strangeness in Neutron Stars

Authors:
Fridolin Weber

Comments: 15 pages, 6 figures, Presented at the 5th International Conference on
Strangeness in Quark Matter (Strangeness 2000), Berkeley, California, USA,
July 20-25, 2000

It is generally agreed on that the tremendous densities reached in the
centers of neutron stars provide a high-pressure environment in which numerous
novel particles processes are likely to compete with each other. These
processes range from the generation of hyperons to quark deconfinement to the
formation of kaon condensates and H-matter. There are theoretical suggestions
of even more exotic processes inside neutron stars, such as the formation of
absolutely stable strange quark matter, a configuration of matter even more
stable than the most stable atomic nucleus, iron. In the latter event, neutron
stars would be largely composed of pure quark matter, eventually enveloped in a
thin nuclear crust. No matter which physical processes are actually realized
inside neutron stars, each one leads to fingerprints, some more pronounced than
others though, in the observable stellar quantities. This feature combined with
the unprecedented progress in observational astronomy, which allows us to see
vistas with remarkable clarity that previously were only imagined, renders
neutron stars to nearly ideal probes for a wide range of physical studies,
including the role of strangeness in dense matter.
(49kb)




astro-ph/0008377 [abs, src, ps, other] :




Title: Detectability of Gravitational Lensing Effect on the Two-point
Correlation Function of Hotspots in the CMB maps

Authors:
Masahiro Takada,
Toshifumi Futamase (Tohoku University, Japan)

Comments: Accepted by ApJ. Received June 14, Accepted August 24. 24 pages
including 9 figures


We present quantitative investigations of the weak lensing effect on the
two-point correlation functions of local maxima (hotspots),

$xipk( heta)$, in the cosmic microwave background (CMB) maps. The lensing
effect depends on the projected mass fluctuations between today and the
redshift $z_{
m rec}approx1100$. If adopting the Gaussian assumption for the
primordial temperature fluctuations field, the peak statistics can provide an
additional information about the intrinsic distribution of hotspots that those
pairs have some characteristic separation angles. The weak lensing then
redistributes hotspots in the observed CMB maps from the intrinsic distribution
and consequently imprints non-Gaussian signatures onto $xipk( heta)$.
Especially, since the intrinsic $xipk( heta)$ has a pronounced depression
feature around the angular scale of $ hetaapprox 70’$ for a flat universe,
the weak lensing induces a large smoothing at the scale. We show that the
lensing signature therefore has an advantage to effectively probe mass
fluctuations with large wavelength modes around $lambdaapprox 50 h^{-1}{
m
Mpc}$. To reveal the detectability, we performed numerical experiments with
specifications of {em MAP} and {em Planck Surveyor} including the
instrumental effects of beam smoothing and detector noise. It is then found
that our method can successfully provide constraints on amplitude of the mass
fluctuations and cosmological parameters in a flat universe with and without
cosmological constant, provided that we use maps with 65% sky coverage expected
from Planck.
(133kb)




astro-ph/0008378 [abs, src, ps, other] :




Title: The warm circumstellar envelope and wind of the G9 IIb star HR 6902

Authors:
T. Kirsch,
R. Baade,
D. Reimers (Universitaet Hamburg, Hamburger Sternwarte)

Comments: 11 pages, 8 figures, submitted to Astronomy Astrophysics main Journal


IUE observations of the eclipsing binary system HR 6902 obtained at various
epochs spread over four years indicate the presence of warm circumstellar
material enveloping the G9 IIb primary. The spectra show Si IV and C IV
absorption up to a distance of 3.3 giant radii (R_g}. Line ratio diagnostics
yields an electron temperature of ~ 78000 K which appears to be constant over
the observed height range.

Applying a least square fit absorption line analysis we derive column
densities as a function of height. We find that the inner envelope (< 3 R_g) of
the bright giant is consistent with a hydrostatic density distribution. The
derived line broadening velocity of ~ 70 kms^{-1} is sufficient to provide
turbulent pressure support for the required scale height. However, an improved
agreement with observations over the whole height regime including the emission
line region is obtained with an outflow model. We demonstrate that the common
beta power-law as well as a P propto rho wind yield appropriate fit models.
Adopting a continuous mass outflow we obtain a mass-loss rate of M_loss= (0.8 –
3.4)*10^{-11} M_{sun}yr^{-1} depending on the particular wind model.
(138kb)




astro-ph/0008379 [abs, src, ps, other] :




Title: A New interpretation of chain galaxies at high redshift

Authors:
Yoshiaki Taniguchi,
Yasuhiro Shioya

Comments: 11 pages with 2 figures, Accepted for publication in ApJ


We propose a possible new model for the formation of chain galaxies at high
redshift. Our model is summarized as follows. Step I: Successive merging of
subgalactic gas clumps results in the formation of a galaxy with a mass of
$10^{11-12} M_odot$ at redshift $z sim 5$. Step II: Subsequently, supernova
explosions occur inside the galaxy and then blow out as a galactic wind (or a
superwind). This wind expands into the intergalactic space and then causes a
large-scale shell with a radius of several hundreds of kpc. Since this radius
may be smaller than the typical separation between galaxies, interactions of
shells may also occur, resulting in the formation of a large-scale gaseous
slab. Step III: Since the shell or the slab can be regarded as a gaseous sheet,
filament-like gravitational instability is expected to occur. Step IV: Further
gravitational instability occurs in each filament, leading to intense star
formation along the filament. This is the chain galaxy phase. Step V: The
filament collapses gravitationally into one spheroidal system like an
elliptical galaxy within one dynamical timescale of the filament ($sim 10^8$
yr). Therefore, it seems quite difficult to find remnants of chain galaxies. We
also discuss that shocked shells driven by superwinds may be responsible for
some Lyman limit systems and damped Ly$alpha$ systems because their H {sc i}
column densities are expected to be $N_{
m HI} gtrsim 10^{19}$ cm$^{-2}$.
(26kb)




astro-ph/0008380 [abs, src, ps, other] :




Title: High redshift radio galaxies: Beacons to biased hierarchical galaxy
formation within large scale structure

Authors:
C.L. Carilli (NRAO),
G.K. Miley,
H. Rottgering,
J. Kurk,
L.Pentericci (Leiden),
D.E. Harris (SAO),
F. Bertoldi,
K.M. Menten (MPIfR),
Wil van Breugel (LLNL)

Comments: Gas & Galaxy Evolution, ASP Conference Series, eds. Hibbard, Rupen,
and van Gorkom. For higher quality figures see:
this http URL


We summarize observations of the properties of powerful radio galaxies and
their environments from z = 0 to 5. These data show that some high redshift
radio galaxies inhabit regions of gas and galaxy over-densities indicative of
proto-cluster environments.
(371kb)




astro-ph/0008381 [abs, src, ps, other] :




Title: Chemical Evolution of Galaxies

Author:
B.E.J. Pagel (Sussex University, Brighton, UK)

Comments: 6 pages, AAS LaTeX macros v5.0, Millennium Essay to appear in PASP,
Feb 2001


Chemical evolution of galaxies brings together ideas on stellar evolution and
nucleosynthesis with theories of galaxy formation, star formation and galaxy
evolution, with all their associated uncertainties. In a new perspective
brought about by the Hubble Deep Field and follow-up investigations of global
star formation rates, diffuse background etc., it has become necessary to
consider the chemical composition of dark baryonic matter as well as that of
visible matter in galaxies.
(13kb)




astro-ph/0008382 [abs, src, ps, other] :




Title: On Solar System and Cosmic Rays Nucleosynthesis and Spallation
Processes

Authors:
Stepan G. Mashnik

Comments: 46 pages, 12 figures, 1 table, LaTeX, submitted to the World Wide
Web

A brief survey of nuclide abundances in the solar-system and in cosmic rays
and of the believed mechanisms of their synthesis is given. The role of
spallation processes in nucleosynthesis is discussed. A short review of recent
measurements, compilations, calculations, and evaluations of spallation cross
sections relevant to nuclear astrophysics is given as well. It is shown that in
some past astrophysical simulations, old experimental nuclear data and
theoretical cross sections that are in poor agreement with recent measurements
and calculations were used. New astrophysical simulations using recently
measured and reliably calculated nuclear cross sections, further researches in
obtaining better cross sections, and production of evaluated spallation cross
sections libraries for astrophysics are suggested.
(280kb)




astro-ph/0008383 [abs, src, ps, other] :




Title: Eros 2 proper motion survey for halo white dwarfs

Authors:
Bertrand Goldman (College de France),
Eros Collaboration

Comments: 5 pages, TeX, 3 Postscript figures, moriond2000.sty. To appear in the
Proceedings of the XXth Moriond Astrophysics Meeting “Cosmological Physics
with Gravitational Lensing”, eds. J.-P. Kneib, Y. Mellier, M. Moniez and J.
Tran Thanh Van


Since 1996 EROS 2 has surveyed 440 square degrees at high Galactic latitude
in order to search for high proper motion stars in the Solar neighbourhood. We
present here the analysis of 250 square degrees for which we have three years
of data. No object with halo-like kinematics has been detected. Using a
detailed Monte-Carlo simulation of the observations, we calculate our detection
efficiency for this kind of object and place constraints on their contribution
to various halo models. If 14 Gyr old, the halo cannot be made of more than 18%
of hydrogen white dwarfs (95% C.L.).
(54kb)




astro-ph/0008384 [abs, src, ps, other] :




Title: Abundance analysis of two extremely metal-poor stars from the
Hamburg/ESO Survey

Authors:
E. Depagne,
V. Hill,
N. Christlieb,
F. Primas

Comments: 8 pages, 7 figures


We report on the first high spectral resolution analysis of extremely
metal-poor halo stars from the Hamburg/ESO objective-prism survey (HES). The
spectra were obtained with UVES at VLT-UT2. The two stars under investigation
(object {HE 1303–2708} and object {HE 1353–2735}) are main-sequence
turnoff-stars having metal abundances of [Fe/H]=-2.85 and -3.20, respectively.
The stellar parameters derived from the UVES spectra are in very good agreement
with those derived from moderate-resolution follow-up spectra. HE 1353–2735 is
a double-lined spectroscopic binary.

The two stars nicely reproduce the strong scatter in [Sr/Fe] observed for
extremely metal-poor stars. While we see a strong Sr II $lambda 4215$ {AA}
line in the spectrum of HE 1303–2708 ([Sr/Fe]=-0.08), we can only give an
upper limit for HE 1353–2735 ([Sr/Fe]<-1.2), since the line is not detected.
We report abundances of Mg, Ca, Sc, Ti, Cr for both stars, and Co, Y for
respect to known trends for metal-poor stars.Lithium is also detected in these
stars, to a level which places them among Lithium-plateau metal-poor dwarfs.
(62kb)




astro-ph/0008385 [abs, src, ps, other] :




Title: Evidences for two Gamma-Ray Burst afterglow emission regimes

Authors:
Michel Boer,
Bruce Gendre

Comments: 4 pages, 2 figures, letter to be published in Astronomy and
Astrophysics


We applied cosmological and absorption corrections to the X-ray and optical
afterglow fluxes of a sample of Gamma-Ray Burst sources of known distance. We
find a good correlation in X-rays and that the GRBs in our sample form two well
defined classes. We tentatively interpret them as radiative and adiabatic
afterglow behaviours in the framework of the fireball model for GRBs. We do not
observe this correlation at optical wavelengths. This discrepancy with the
model may be due to the absorption in the source vicinity.
(50kb)




astro-ph/0008386 [abs, pdf] :




Title: Hubble Redshift

Authors:
W. Q. Sumner,
E. E. Vityaev

Comments: 8 pages, 4 figures

The dependence of luminosity distance on observed resdhift and the
cosmological parameters H and q is derived for a contracting Friedmann universe
with no cosmological constant. The result is consistent with recent supernovae
observations.
(54kb)




astro-ph/0008387 [abs, src, ps, other] :




Title: Variable Galaxies in the Hubble Deep Field

Authors:
V. L. Sarajedini,
R. L. Gilliland,
M. M. Phillips

Comments: 31 pages, 8 figures, accepted to the AJ


We present results from a study to detect variable galaxies in the Hubble
Deep Field North. The goal of this project is to investigate the number density
of AGN at z=1 through the detection of variable galaxy nuclei. The advantage of
HST is the ability to do accurate photometry within smaller apertures, thus
allowing us to probe much lower AGN/host galaxy luminosity ratios than can be
done from the ground. The primary data sets analyzed for galactic variability
follow from the original HDF-N observations in December 1995 and a second epoch
obtained two years later.

We have detected nuclear variability at or above the 3 sigma level in 8 of
633 HDF galaxies at I<27. Only 2 detections would be expected by chance in a
normal distribution. At least one of these 8 has been spectroscopically
confirmed as a Seyfert 1 galaxy. Based on the AGN structure function for
variability, the estimated luminosity of the varying component in each galaxy
lies in the range -19.5<M<-15.0. We construct an upper limit to the luminosity
function for the variable nuclei and compare this to the local Seyfert LF and
the LF for QSOs at z=1. Assuming we have detected all Seyfert-like nuclei in
the HDF-N, we find no evidence for an increase in the number density of AGN at
M=-19. We estimate that ~1-3% of field galaxies with I<27 may contain a nuclear
AGN.
(265kb)




astro-ph/0008388 [abs, src, ps, other] :




Title: Chandra Observations of the Young Pulsar PSR B0540-69

Authors:
P. Kaaret (1),
H.L. Marshall (2),
T.L. Aldcroft (1),
D.E. Graessle (1),
M. Karovska (1),
S.S. Murray (1),
A.H. Rots (1),
N.S. Schulz (2),
F.D. Seward (1) ((1) SAO, (2) MIT)

Comments: 12 pages, accepted by the Astrophysical Journal


The young pulsar PSR B0540-69 was one of the first targets observed with the
Chandra X-Ray Observatory. The high angular resolution of Chandra allows us to
resolve the compact nebula surrounding the pulsar. We have determined a
position for PSR B0540-69 of R.A. = 05h 40m 11s.221, decl. = -69o 19′ 54″.98
(J2000) with a 1-sigma radial uncertainty of 0.7″. Combining our measurements
of the pulsar period with previous measurements covering a span of 12 years, we
derive a braking index of 2.08. The spectrum of the pulsed emission is
consistent with a power-law with a photon index of 1.83 +/- 0.13. The compact
nebula has a softer spectrum with a photon index of 1.85 to 2.26.
(53kb)




astro-ph/0008389 [abs, src, ps, other] :




Title: Evolution of Proto-Neutron stars with kaon condensates

Authors:
Jose A. Pons,
Juan A. Miralles,
M. Prakash,
James M. Lattimer

Comments: 25 pages, 14 figures. Submitted to Astrophysical Journal


We present simulations of the evolution of a proto-neutron star in which
kaon-condensed matter might exist, including the effects of finite temperature
and trapped neutrinos. The phase transition from pure nucleonic matter to the
kaon condensate phase is described using Gibbs’ rules for phase equilibrium,
which permit the existence of a mixed phase. A general property of neutron
stars containing kaon condensates, as well as other forms of strangeness, is
that the maximum mass for cold, neutrino-free matter can be less than the
maximum mass for matter containing trapped neutrinos or which has a finite
entropy. A proto-neutron star formed with a baryon mass exceeding that of the
maximum mass of cold, neutrino-free matter is therefore metastable, that is, it
will collapse to a black hole at some time during the Kelvin-Helmholtz cooling
stage.

The effects of kaon condensation on metastable stars are dramatic. In these
cases, the neutrino signal from a hypothetical galactic supernova (distance
$sim8.5$ kpc) will stop suddenly, generally at a level above the background in
the SuperK and SNO detectors, which have low energy thresholds and backgrounds.
This is in contrast to the case of a stable star, for which the signal
exponentially decays, eventually disappearing into the background. We find the
lifetimes of kaon-condensed metastable stars to be restricted to the range
40–70 s and weakly dependent on the proto-neutron star mass, in sharp contrast
to the significantly larger mass dependence and range (1–100 s) of
hyperon-rich metastable stars.
(91kb)




astro-ph/0008390 [abs, src, ps, other] :




Title: Constraints on Galaxy Density Profiles from Strong Gravitational
Lensing: The Case of B 1933+503

Authors:
J.D. Cohn,
C.S. Kochanek,
B. A. McLeod,
C.R. Keeton

Comments: 26 pages, 10 figures


We consider a wide range of parametric mass models for B~1933+503, a
ten-image radio lens, and identify shared properties of the models with the
best fits. The approximate rotation curve varies by less than 7% from the
average value between the innermost and the outermost image (1.5h^{-1} kpc to
4.1h^{-1} kpc) for models within 1 sigma of the best fit, and the radial
dependence of the shear strength and angle also have common behavior for the
best models. The time delay between images 1 and 6, the longest delay between
the radio cores, is Delta t = (11.0 pm 1.7)h^{-1} days (Omega_0=0.3,
lambda_0=0.7) including all the modeling uncertainties. Deeper infrared
observations, to more precisely register the lens galaxy with the radio images
and to measure the properties of the Einstein ring image of the radio source’s
host galaxy, would significantly improve the model constraints and further
reduce the uncertainties in the time delay.
(87kb)




astro-ph/0008391 [abs, src, ps, other] :




Title: A Shock-Induced PDR in the HH 80/81 Flow. Far Infrared Spectroscopy

Authors:
Sergio Molinari,
Alberto Noriega-Crespo,
Luigi Spinoglio

Comments: to be published in ApJ


The two spectrometers on board the Infrared Space Observatory were used to
observe the Herbig-Haro objects HH 80, 81 and 80N, as well as their candidate
exciting source IRAS 18162-2048. The fine structure lines of [OI]63um,
[OI]145um and [CII]158um are detected everywhere, while [NII]122um and
[OIII]88um are only detected toward the HH objects; line ratios confirm for the
first time the collisionally excited HH nature of HH 80N. No molecular line is
detected in any of the observed positions. We use a full shock code to diagnose
shock velocities vs~100 km/s toward the HH objects, as expected from the
optical spectroscopy. Since proper motions suggest velocities in excess of 600
km/s, the HH objects probably represent the interface between two flow
components with velocity differing by ~vs. Aside from the flow exciting source,
the [CII]158um line is everywhere brighter than the [OI]63um line, indicating
the presence of a Photo-Dissociation Region (PDR) all along the flow. Continuum
emission from the HH objects and from other positions along the flow is only
detected longword of ~50 micron, and its proportionality to the [CII]158um line
flux suggests it is PDR in origin. We propose that the FUV continuum irradiated
by the HH objects and the jet is responsible for the generation of a PDR at the
walls of the flow cavity. We develop a very simple model which strengthens the
plausibility of this hypothesis.
(169kb)




Cross-listings




gr-qc/0002005 [abs, src, ps, other] :




Title: Wave-Particle duality at the Planck scale: Freezing of neutrino
oscillations

Authors:
D. V. Ahluwalia

Comments: Revised re-written version, accepted for publication in Phys. Lett. A

A gravitationally-induced modification to de Broglie wave-particle duality is
presented. At Planck scale, the gravitationally-modified matter wavelength
saturates to a few times the Planck length in a momentum independent manner. In
certain frameworks, this circumstance freezes neutrino oscillations in the
Planck realm. This effect is apart, and beyond, the gravitational red-shift. A
conclusion is drawn that in a complete theory of quantum gravity the notions of
“quantum” and “gravity” shall carry new meanings — meanings, that are yet
to be deciphered from theory and observations in their entirety.
(8kb)




gr-qc/0008057 [abs, src, ps, other] :




Title: Scattering of particles by neutron stars: Time-evolutions for axial
perturbations

Authors:
V.Ferrari (Rome),
K.D.Kokkotas (Thessaloniki)

Comments: 7 pages, 5 figures, Phys. Rev. D in press


The excitation of the axial quasi-normal modes of a relativistic star by
scattered particles is studied by evolving the time dependent perturbation
equations. This work is the first step towards the understanding of more
complicated perturbative processes, like the capture or the scattering of
particles by rotating stars. In addition, it may serve as a test for the
results of the full nonlinear evolution of binary systems.
(61kb)




physics/0008214 [abs, src, ps, other] :




Title: Predictions about the behaviour of diamond, silicon, SiC and some AIIIBV
semiconductor materials in hadron fields

Authors:
Ionel Lazanu,
Sorina Lazanu

Comments: 12 pages, 7 figures, submitted to Radiation Measurements

Subj-class: Instrumentation and Detectors; Materials Science


The utilisation of crystalline semiconductor materials as detectors and
devices operating in high radiation environments, at the future particle
colliders, in space applications, in medicine and industry, makes necessary to
obtain radiation harder materials. Diamond, SiC and different AIIIBV compounds
(GaAs, GaP, InP, InAs, InSb) are possible competitors for silicon to different
electronic devices for the up-mentioned applications. The main goal of this
paper is to give theoretical predictions about the behaviour of these
semiconductors in hadron fields (pions, protons). The effects of the
interaction between the incident particle and the semiconductor are
characterised in the present paper both from the point of view of the
projectile, the relevant quantity being the energy loss by nuclear
interactions, and of the target, using the concentration of primary radiation
induced defects on unit particle fluence. Some predictions about the damage
induced by hadrons in these materials in possible applications in particle
physics and space experiments are done.
(86kb)




Replacements




astro-ph/9901425 [abs, html] :




Title: A gravitationally powered oscillatory pulsar model

Authors:
G. Osborn

Comments: HTML, Submitted to Classical and Quantum Gravity 23 Aug 2000

Note: replaced with revised version Thu, 24 Aug 2000 00:34:49 GMT (11kb)



astro-ph/9905162 [abs, src, ps, other] :




Title: EROS 2 proper motion survey: a field brown dwarf and an L dwarf
companion to LHS 102

Authors:
B. Goldman,
X. Delfosse,
T. Forveille,
C. Afonso et al:
the EROS collaboration

Comments: 5 pages, LaTeX, 6 postscript figures, style correction, two spectra
of the discovered objects added, coordinates of the LHS102 pair corrected

Journal-ref: Astronomy & Astrophysics, 351, L5-L9 (1999)

Note: replaced with revised version Thu, 24 Aug 2000 16:37:04 GMT (391kb)



astro-ph/9907006 [abs, src, ps, other] :




Title: Partially ionized hydrogen plasma in strong magnetic fields

Authors:
A.Y. Potekhin (1),
G. Chabrier (2),
Yu.A. Shibanov (1) ((1) Ioffe Phys.-Tech. Inst., St.Petersburg; (2) CRAL, ENS-Lyon)

Comments: 17 pages, 11 figures (embedded using epsf.sty), REVTeX. Two curves on
the right panel of Fig. 8 are corrected

Subj-class: Astrophysics; Plasma Physics

Journal-ref: Phys.Rev. E60 (1999) 2193

Note: replaced with revised version Thu, 24 Aug 2000 11:13:38 GMT (138kb)



astro-ph/0005263 [abs, src, ps, other] :




Title: Probing High Redshift Radiation Fields with Gamma-Ray Absorption

Authors:
S. Peng Oh (Princeton)

Comments: 17 pages, 5 figures; slightly modified version submitted to ApJ

Note: replaced with revised version Thu, 24 Aug 2000 05:55:49 GMT (32kb)



astro-ph/0007124 [abs, src, ps, other] :




Title: Proper Motions of Pre-Main Sequence Stars in Southern Star-Forming
Regions

Authors:
R. Teixeira (1),
C. Ducourant (2),
M. J. Sartori (1),
J. I. B. Camargo (1),
J. P. Perié (2),
J. R. D. Lépine (1),
P. Benevides-Soares (1) ((1) Departamento de Astronomia, USP, Brazil, (2) Observatoire de Bordeaux, France)

Comments: 14 pages, LaTeX, 12 PostScript figures, 6 tables; figures 3, 6 and 7
replaced, tables 3 and 4 updated. Accepted for publication in A&A

Note: replaced with revised version Thu, 24 Aug 2000 02:32:18 GMT (127kb)



astro-ph/0008118 [abs, src, ps, other] :




Title: Relativistic Iron Emission and Disk Reflection in Galactic Microquasar
XTE J1748-288

Authors:
J. M. Miller (MIT),
D. W. Fox (MIT),
T. DiMatteo (CfA),
R. Wijnands (MIT),
T. Belloni (Oss. di Brera),
D. Pooley (MIT),
C. Kouveliotou (MSFC),
W. H. G. Lewin (MIT)

Comments: 32 pages, 8 figures, 5 tables. ApJ accepted 8/16/00

Note: replaced with revised version Thu, 24 Aug 2000 12:47:46 GMT (95kb)



astro-ph/0008368 [abs, src, ps, other] :




Title: Ionization, Magneto-rotational, and Gravitational Instabilities in Thin
Accretion Disks Around Supermassive Black Holes

Authors:
Kristen Menou (Princeton Univ.),
Eliot Quataert (IAS)

Comments: submitted to ApJ Letters; email address corrected

Note: replaced with revised version Thu, 24 Aug 2000 20:30:12 GMT (19kb)




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