3,151 research outputs found
Studies of the Relativistic Binary Pulsar PSR B1534+12. II. Origin and Evolution
We have recently measured the angle between the spin and orbital angular
momenta of PSR B1534+12 to be either 25+/-4 deg or 155+/-4 deg. This
misalignment was almost certainly caused by an asymmetry in the supernova
explosion that formed its companion neutron star. Here we combine the
misalignment measurement with measurements of the pulsar and companion masses,
the orbital elements, proper motion, and interstellar scintillation. We show
that the orbit of the binary in the Galaxy is inconsistent with a velocity kick
large enough to produce a nearly antialigned spin axis, so the true
misalignment must be ~25 deg. Similar arguments lead to bounds on the mass of
the companion star immediately before its supernova: 3+/-1 Msun. The result is
a coherent scenario for the formation of the observed binary. After the first
supernova explosion, the neutron star that would eventually become the observed
pulsar was in a Be/X-ray type binary system with a companion of at least 10--12
Msun. During hydrogen (or possibly helium) shell burning, mass transfer
occurred in a common envelope phase, leaving the neutron star in a roughly
half-day orbit with a helium star with mass above ~3.3 Msun. A second phase of
mass transfer was then initiated by Roche lobe overflow during shell helium
burning, further reducing both the helium star mass and orbital period before
the second supernova. Scenarios that avoid Roche lobe overflow by the helium
star require larger helium star masses and predict space velocities
inconsistent with our measurements. The companion neutron star experienced a
velocity kick of 230+/-60 km/s at birth, leading to a systemic kick to the
binary of 180+/-60 km/s.Comment: 9 pages, submitted to ApJ. Abstract shortened. Version with
high-resolution figures available at
http://www.astro.ubc.ca/people/stairs/papers/tds04_orig.ps.g
An X-ray and Optical Investigation of the Starburst-driven Superwind in the Galaxy Merger Arp 299
We present a detailed investigation of the X-ray and optical properties of
the starburst-merger system Arp299 (NGC 3690, Mrk 171), with an emphasis on its
spectacular gaseous nebula. We analyse \rosat and \asca X-ray data and optical
spectra and narrow-band images. We suggest that the on-going galaxy collision
has tidally-redistributed the ISM of the merging galaxies. The optical
emission-line nebula results as this gas is photoionized by radiation that
escapes from the starburst, and is shock-heated, accelerated, and pressurized
by a `superwind' driven by the collective effect of the starburst supernovae
and stellar winds. The X-ray nebula in Arp 299 is is plausibly a mass-loaded
flow of adiabatically-cooling gas that carries out a substantial fraction of
the energy and metals injected by the starburst at close to the escape velocity
from Arp 299. The mass outflow rate likely exceeds the star-formation rate in
this system. We conclude that powerful starbursts are able to heat (and
possibly eject) a significant fraction of the ISM in merging galaxies.Comment: 54 pages, 17 postscript figures, AAS late
The Evolution of X-ray Bursts in the "Bursting Pulsar" GRO J1744-28
GRO J1744-28, commonly known as the `Bursting Pulsar', is a low mass X-ray
binary containing a neutron star and an evolved giant star. This system,
together with the Rapid Burster (MXB 1730-33), are the only two systems that
display the so-called Type II X-ray bursts. These type of bursts, which last
for 10s of seconds, are thought to be caused by viscous instabilities in the
disk; however the Type II bursts seen in GRO J1744-28 are qualitatively very
different from those seen in the archetypal Type II bursting source the Rapid
Burster. To understand these differences and to create a framework for future
study, we perform a study of all X-ray observations of all 3 known outbursts of
the Bursting Pulsar which contained Type II bursts, including a population
study of all Type II X-ray bursts seen by RXTE. We find that the bursts from
this source are best described in four distinct phenomena or `classes' and that
the characteristics of the bursts evolve in a predictable way. We compare our
results with what is known for the Rapid Burster and put out results in the
context of models that try to explain this phenomena.Comment: Accepted to MNRAS Aug 17 201
Variability of the X-ray P Cygni Line Profiles from Circinus X-1 Near Zero Phase
The luminous X-ray binary Circinus X-1 has been observed twice near zero
orbital phase using the High-Energy Transmission Grating Spectrometer (HETGS)
onboard Chandra. The source was in a high-flux state during a flare for the
first observation, and it was in a low-flux state during a dip for the second.
Spectra from both flux states show clear P Cygni lines, predominantly from
H-like and He-like ion species. These indicate the presence of a high-velocity
outflow from the Cir X-1 system which we interpret as an equatorial
accretion-disk wind, and from the blueshifted resonance absorption lines we
determine outflow velocities of 200 - 1900 km/s with no clear velocity
differences between the two flux states. The line strengths and profiles,
however, are strongly variable both between the two observations as well as
within the individual observations. We characterize this variability and
suggest that it is due to both changes in the amount of absorbing material
along the line of sight as well as changes in the ionization level of the wind.
We also refine constraints on the accretion-disk wind model using improved
plasma diagnostics such as the He-like Mg XI triplet, and we consider the
possibility that the X-ray absorption features seen from superluminal jet
sources can generally be explained via high-velocity outflows.Comment: 12 pages, 8 figures, accepted by ApJ (Main
Correlation Between Mucosal IL-6 mRNA Expression Level and Virulence Factors of Helicobacter pylori in Iranian Adult Patients With Chronic Gastritis
Background: Helicobacter pylori infection is associated with gastritis and marked infiltration of the gastric mucosa by several cytokines secreting inflammatory cells that contribute to sustained local inflammation. In this study, we sought to examine IL-6 expression in H. pylori-infected and uninfected gastric mucosa and elucidate the implication in the pathogenesis of H. pylori-associated gastritis in human. Objectives: The current study aimed to determine mucosal IL-6 mRNA expression level and their correlation with virulence factors and the grade of chronic gastritis among H. pylori infected patients with chronic gastritis from Shahrekord, Iran. Patients and Methods: Mucosal IL-6 mRNA levels was measured by real-time PCR using endoscopic biopsies taken from the gastric antrum of 58 subjects infected with H. pylori and 44 uninfected subjects. Presence of vacA and cagA virulence factors was evaluated using PCR. Results: The IL-6 mRNA expression levels were significantly more elevated in H. pylori-positive patients than uninfected individuals and expression of this cytokine was independent from the virulence factors. There was a correlation between IL-6 expression level and the grade of chronic gastritis. Conclusions: Enhanced induction of IL-6 may be involved in the pathogenesis of H. pylon-associated gastritis
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