782 research outputs found
Searching for Weak or Complex Magnetic Fields in Polarized Spectra of Rigel
Seventy-eight high-resolution Stokes V, Q and U spectra of the B8Iae
supergiant Rigel were obtained with the ESPaDOnS spectropolarimeter at CFHT and
its clone NARVAL at TBL in the context of the Magnetism in Massive Stars
(MiMeS) Large Program, in order to scrutinize this core-collapse supernova
progenitor for evidence of weak and/or complex magnetic fields. In this paper
we describe the reduction and analysis of the data, the constraints obtained on
any photospheric magnetic field, and the variability of photospheric and wind
lines.Comment: IAUS272 - Active OB Stars: Structure, Evolution, Mass Loss and
Critical Limit
Resolving the Mystery of X-ray Faint Elliptical Galaxies: Chandra X-ray Observations of NGC 4697
Chandra observations of the X-ray faint elliptical galaxy NGC 4697 resolve
much of the X-ray emission (61% within one effective radius) into ~80 point
sources, of which most are low mass X-ray binaries (LMXBs). These LMXBs provide
the bulk of the hard emission and much of the soft emission as well. Of the
remaining unresolved emission, it is likely that about half is from fainter
LMXBs, while the other half (~23% of the total emission) is from interstellar
gas. Three of the resolved sources are supersoft sources. In the outer regions
of NGC 4697, eight of the LMXBs (about 25%) are coincident with candidate
globular clusters, which indicates that globulars have a high probability of
containing X-ray binaries compared to the normal stellar population. The X-ray
luminosities (0.3-10 keV) of the resolved LMXBs range from ~5e37 to ~2.5e39
ergs/s. The luminosity function of the LMXBs has a "knee" at 3.2e38 ergs/s,
which is roughly the Eddington luminosity of a 1.4 M_sun neutron star (NS);
this knee might be useful as a distance indicator. The highest luminosity
source has the Eddington luminosity of a ~20 M_sun black hole (BH). The
presence of this large population of NS and massive BH stellar remnants in this
elliptical galaxy shows that it (or its progenitors) once contained a large
population of massive main sequence stars.Comment: Astrophysical Journal Letters, in press. 4 pages in emulateapj5 style
with 4 embedded Postscript figures. Higher quality version of paper and
figures 1 and 2 are available at
http://www.astro.virginia.edu/~cls7i/papers/NGC4697-Chandra.ps.gz,
http://www.astro.virginia.edu/~cls7i/papers/NGC4697-Chandra_fig1.ps.gz, and
http://www.astro.virginia.edu/~cls7i/papers/NGC4697-Chandra_fig2.ps.g
A biophysical model of decision making in an antisaccade task through variable climbing activity
We present a biophysical model of saccade initiation based on
competitive integration of planned and reactive cortical saccade decision signals
in the intermediate layer of the superior colliculus. In the model, the variable
slopes of the climbing activities of the input cortical decision signals are
produced from variability in the conductances of Na+, K+, Ca2+ activated K+,
NMDA and GABA currents. These cortical decision signals are integrated in
the activities of buildup neurons in the intermediate layer of the superior
colliculus, whose activities grow nonlinearly towards a preset criterion level.
When the level is crossed, a movement is initiated. The resultant model
reproduces the unimodal distributions of saccade reaction times (SRTs) for
correct antisaccades and erroneous prosaccades as well as the variability of
SRTs (ranging from 80ms to 600ms) and the overall 25% of erroneous
prosaccade responses in a large sample of 2006 young men performing an
antisaccade task
The Globular Cluster Systems in the Coma Ellipticals. II: Metallicity Distribution and Radial Structure in NGC 4874, and Implications for Galaxy Formation
Deep HST/WFPC2 (V,I) photometry is used to investigate the globular cluster
system (GCS) in NGC 4874, the central cD galaxy of the Coma cluster. The
luminosity function of the clusters displays its normal Gaussian-like shape and
turnover level. Other features of the system are surprising: the GCS is (a)
spatially extended, with core radius r_c = 22 kpc, (b) entirely metal-poor (a
narrow, unimodal metallicity distribution with mean [Fe/H] = -1.5), and (c)
modestly populated, with specific frequency S_N = 3.7 +- 0.5. We suggest on the
basis of some simple models that as much as half of this galaxy might have
accreted from low-mass satellites, but no single one of the three classic modes
of galaxy formation (accretion, disk mergers, in situ formation) can supply a
fully satisfactory formation picture. Even when they are used in combination,
strong challenges to these models remain. The principal anomaly in this GCS is
essentially the complete lack of metal-rich clusters. If these were present in
normal (M87-like) numbers in addition to the metal-poor ones that are already
there, then the GCS in total would more closely resemble what we see in many
other giant E galaxies.Comment: 27 pp. with 9 Figures. Astrophys.J. 533, in press (April 10, 2000
Imaging of the protoelliptical NGC 1700 and its globular cluster system
An excellent candidate for a young elliptical, or `protoelliptical' galaxy is
NGC 1700. Here we present new B, V and I band imaging using the Keck telescope
and reanalyse existing V and I band images from the Hubble Space Telescope.
After subtracting a model of the galaxy from the Keck images NGC 1700 reveals
two symmetric tidal tail-like structures. If this interpretation is correct, it
suggests a past merger event involving two spiral galaxies. These tails are
largely responsible for the `boxiness' of the galaxy isophotes observed at a
radius of about 13 kpc. We also show that the B-I colour distribution of the
globular cluster system is bimodal. The mean colour of the blue population is
consistent with those of old Galactic globular clusters. Relative to this old,
metal poor population, we find that the red population is younger and more
metal rich. This young population has a similar age and metallicity as that
inferred for the central stars, suggesting that they are both associated with
an episode of star formation triggered by the merger that may have formed the
galaxy. Although possessing large errors, we find that the majority of the age
estimates of NGC 1700 are reasonably consistent and we adopt a `best estimate'
for the age of 3.0 +/-1.0 Gyr. This relatively young age places NGC 1700 within
the age range where there is a notable lack of obvious candidates for
protoellipticals. The total globular cluster specific frequency is rather low
for a typical elliptical, even after taking into account fading of the galaxy
over the next 10 Gyr. We speculate that NGC 1700 will eventually form a
relatively `globular cluster poor' elliptical galaxy.Comment: 15 pages, 15 figures, accepted for publication in MNRA
Rheophysics of dense granular materials : Discrete simulation of plane shear flows
We study the steady plane shear flow of a dense assembly of frictional,
inelastic disks using discrete simulation and prescribing the pressure and the
shear rate. We show that, in the limit of rigid grains, the shear state is
determined by a single dimensionless number, called inertial number I, which
describes the ratio of inertial to pressure forces. Small values of I
correspond to the quasi-static regime of soil mechanics, while large values of
I correspond to the collisional regime of the kinetic theory. Those shear
states are homogeneous, and become intermittent in the quasi-static regime.
When I increases in the intermediate regime, we measure an approximately linear
decrease of the solid fraction from the maximum packing value, and an
approximately linear increase of the effective friction coefficient from the
static internal friction value. From those dilatancy and friction laws, we
deduce the constitutive law for dense granular flows, with a plastic Coulomb
term and a viscous Bagnold term. We also show that the relative velocity
fluctuations follow a scaling law as a function of I. The mechanical
characteristics of the grains (restitution, friction and elasticity) have a
very small influence in this intermediate regime. Then, we explain how the
friction law is related to the angular distribution of contact forces, and why
the local frictional forces have a small contribution to the macroscopic
friction. At the end, as an example of heterogeneous stress distribution, we
describe the shear localization when gravity is added.Comment: 24 pages, 19 figure
Increased systemic and brain cytokine production and neuroinflammation by endotoxin following ethanol treatment
Abstract Background Cytokines and alcohol share a common modulation of inflammation and hormones as well as being implicated in multiple diseases, but the mechanisms are poorly understood. The purpose of this study was to investigate the interaction of liver, serum and brain cytokines as well as whether ethanol would potentiate endotoxin (Lipopolysaccharide, LPS) responses once ethanol had cleared. Methods Male C57BL/6J mice were treated intragastrically with water (control) or ethanol (5 g/kg, i.g., 25% ethanol, w/v), with volumes matched, for 1 day or daily for 10 days. Mice were then injected intraperitoneally with saline (control) or LPS (3 mg/kg, i.p.) in saline 24 hrs after the last dose of ethanol. Gene expression and protein synthesis of proinflammatory cytokines and anti-inflammatory cytokine, oxidative enzymes, microglial activation and inhibition of neurogenesis were examined using real-time PCR, ELISA, and immunohistochemistry. Results LPS increased proinflammatory cytokines (TNFα, MCP-1, IL-1β) several fold in liver, brain and serum at 1 hr. Ethanol is known to increase liver cytokines and alter the risk of multiple chronic diseases. Ten daily doses of ethanol increased brain and liver TNFα, and pretreatment with ethanol potentiated LPS-induced increases in TNFα, MCP-1, IL-1β in liver, serum and brain. Proinflammatory cytokine levels in liver and serum returned to basal levels within a day, whereas brain proinflammatory cytokines remained elevated for long periods. IL-10, an anti-inflammatory cytokine, is reduced in brain by ethanol and LPS, while brain proinflammatory cytokines remain increased, whereas liver IL-10 is increased when proinflammatory cytokines have returned to control levels. Activation of brain microglia indicated by morphological changes, reduced neurogenesis and increased brain expression of COX-2 and gp91phox NADPH oxidase subunit mRNA were found in the 10 daily doses of ethanol-pretreated LPS group. Conclusion Acute increases in serum cytokines induce long lasting increases in brain proinflammatory cytokines. Ten daily doses of ethanol exposure results in persistent alterations of cytokines and significantly increases the magnitude and duration of central and peripheral proinflammatory cytokines and microglial activation. Ethanol induced differential anti-inflammatory cytokine IL-10 responses in liver and brain could cause long lasting disruption of cytokine cascades that could contribute to protection or increased risk of multiple chronic diseases
The X-ray Faint Early-Type Galaxy NGC4697
We analyze archival ROSAT HRI, ROSAT PSPC, and ASCA data of the X-ray faint
early-type galaxy NGC4697. The joint ROSAT PSPC + ASCA spectrum is fit by a
two-component thermal model, a MEKAL model with kT_{MEKAL}=0.26^{+0.04}_{-0.03}
keV with low metallicity and a bremsstrahlung model with
kT_{BREM}=5.2^{+3.0}_{-1.6} keV. A similar model was found to fit the spectra
of another faint early-type galaxy (NGC4382) and the bulge of M31. We interpret
this soft emission as a combination of emission from a soft component of low
mass X-ray binaries (LMXBs) and from a low temperature interstellar medium,
although the relative contributions of the two components could not be
determined. Twelve point sources were identified within 4' of NGC4697, of which
11 are most likely LMXBs associated with the galaxy. The soft X-ray colors of
four of the LMXBs in NGC4697 support the claim that LMXBs possess a soft
spectral component. Finally, we present a simulation of what we believe the
Chandra data of NGC4697 will look like.Comment: 10 pages, uses emulateapj.sty, accepted by Astrophysical Journa
Granular flow down a rough inclined plane: transition between thin and thick piles
The rheology of granular particles in an inclined plane geometry is studied
using molecular dynamics simulations. The flow--no-flow boundary is determined
for piles of varying heights over a range of inclination angles . Three
angles determine the phase diagram: , the angle of repose, is the
angle at which a flowing system comes to rest; , the maximum angle
of stability, is the inclination required to induce flow in a static system;
and is the maximum angle for which stable, steady state flow is
observed. In the stable flow region , three
flow regimes can be distinguished that depend on how close is to
: i) : Bagnold rheology, characterized by a
mean particle velocity in the direction of flow that scales as
, for a pile of height , ii)
: the slow flow regime, characterized by a linear
velocity profile with depth, and iii) : avalanche flow
characterized by a slow underlying creep motion combined with occasional free
surface events and large energy fluctuations. We also probe the physics of the
initiation and cessation of flow. The results are compared to several recent
experimental studies on chute flows and suggest that differences between
measured velocity profiles in these experiments may simply be a consequence of
how far the system is from jamming.Comment: 19 pages, 14 figs, submitted to Physics of Fluid
M87, Globular Clusters, and Galactic Winds: Issues in Giant Galaxy Formation
New VRI photometry is presented for the globular clusters in the innermost
140'' of the M87 halo. The results are used to discuss several issues
concerning the formation and evolution of globular cluster systems in
supergiant ellipticals like M87. (1) we find no significant change in the
globular cluster luminosity function (GCLF) with galactocentric radius, for
cluster masses M < 10^5 solar masses, indicating that the main effects of
dynamical evolution may be only on lower-mass clusters. (2) Within the core
radius (1') of the globular cluster system, the metallicity distribution is
uniform, but at larger radii the mean metallicity declines steadily as Z ~
r^-0.9. (3) The various options for explaining the existence of high specific
frequency galaxies like M87 are evaluated, and scaling laws for the GCSs in
these galaxies are given. Interpretations involving secondary evolution
(formation of many globular clusters during mergers, intergalactic globular
clusters, etc.) are unlikely to be the primary explanation for high-S_N
galaxies. (4) We suggest that central-supergiant E galaxies may have formed in
an exceptionally turbulent or high-density environment in which an early,
powerful galactic wind drove out a high fraction of the protogalactic gas, thus
artificially boosting the specificComment: 67 pages, 17 figures. To appear in Astronomical Journal, in press for
May 1998. Preprints also available from W.Harris; send e-mail request to
[email protected]
- …