529 research outputs found
Study of measured pulsar masses and their possible conclusions
We study the statistics of 61 measured masses of neutron stars (NSs) in
binary pulsar systems, including 18 double NS (DNS) systems, 26 radio pulsars
(10 in our Galaxy) with white dwarf (WD) companions, 3 NSs with main-sequence
companions, 13 NSs in X-ray binaries, and one undetermined system. We derive a
mean value of M = 1.46 +/- 0.30 solar masses. When the 46 NSs with measured
spin periods are divided into two groups at 20 milliseconds, i.e., the
millisecond pulsar (MSP) group and others, we find that their mass averages
are, respectively, M=1.57 +/- 0.35 solar masses and M=1.37+/- 0.23 solar
masses. In the framework of the pulsar recycling hypothesis, this suggests that
an accretion of approximately 0.2 solar mass is sufficient to spin up a neutron
star and place it in the millisecond pulsar group. An empirical relation
between the accreting mass and MSP spin period is \Delta M=0.43 (solar
mass)(P/1 ms)^{-2/3}. UNlike the standard recycling process, if a MSP is formed
by the accretion induced collapse (AIC) of a white dwarf with a mass less than
Chandrasekha limit, e.g. 1.35 solar mass, then the binary MSPs involved in AICs
is not be higher than 20%, which imposes a constraint on the AIC origin of
MSPs.Comment: 6 pages, 5 figures, in press, Astronomy and Astrophysics 2011, 527,
8
Evidence for a Massive Neutron Star from a Radial-Velocity Study of the Companion to the Black Widow Pulsar PSR B1957+20
The most massive neutron stars constrain the behavior of ultra-dense matter,
with larger masses possible only for increasingly stiff equations of state.
Here, we present evidence that the black widow pulsar, PSR B1957+20, has a high
mass. We took spectra of its strongly irradiated companion and found an
observed radial-velocity amplitude of K_obs=324+/-3 km/s. Correcting this for
the fact that, due to the irradiation, the center of light lies inward relative
to the center of mass, we infer a true radial-velocity amplitude of K_2=353+/-4
km/s and a mass ratio q=M_PSR/M_2=69.2+/-0.8. Combined with the inclination
i=65+/-2 deg inferred from models of the lightcurve, our best-fit pulsar mass
is M_PSR=2.40+/-0.12 M_sun. We discuss possible systematic uncertainties, in
particular in the lightcurve modeling. Taking an upper limit of i<85 deg based
on the absence of radio eclipses at high frequency, combined with a
conservative lower-limit to the motion of the center of mass, K_2>343 km/s
(q>67.3), we infer a lower limit to the pulsar mass of M_PSR>1.66 M_sun.Comment: 7 pages, 3 figures, 1 table, accepted for publication in ApJ;
revision includes more detail on the spectral classification and discussion
of other recent high neutron-star masse
A precise mass measurement of the intermediate-mass binary pulsar PSR J1802-2124
PSR J1802-2124 is a 12.6-ms pulsar in a 16.8-hour binary orbit with a
relatively massive white dwarf (WD) companion. These properties make it a
member of the intermediate-mass class of binary pulsar (IMBP) systems. We have
been timing this pulsar since its discovery in 2002. Concentrated observations
at the Green Bank Telescope, augmented with data from the Parkes and Nancay
observatories, have allowed us to determine the general relativistic Shapiro
delay. This has yielded pulsar and white dwarf mass measurements of 1.24(11)
and 0.78(4) solar masses (68% confidence), respectively. The low mass of the
pulsar, the high mass of the WD companion, the short orbital period, and the
pulsar spin period may be explained by the system having gone through a
common-envelope phase in its evolution. We argue that selection effects may
contribute to the relatively small number of known IMBPs.Comment: 9 pages, 4 figures, 3 tables, accepted for publication in the
Astrophysical Journa
The radial velocity of the companion star in the low-mass X-ray binary 2S 0921-630: limits on the mass of the compact object
In this Paper we report on optical spectroscopic observations of the low-mass
X-ray binary 2S 0921-630 obtained with the Very Large Telescope. We found
sinusoidal radial velocity variations of the companion star with a
semi-amplitude of 99.1+-3.1 km s^-1 modulated on a period of 9.006+-0.007 days,
consistent with the orbital period found before for this source, and a systemic
velocity of 44.4+-2.4 km s^-1. Due to X-ray irradiation the centre-of-light
measured by the absorption lines from the companion star is likely shifted with
respect to the centre-of-mass. We try to correct for this using the so-called
K-correction. Conservatively applying the maximum correction possible and using
the previously measured rotational velocity of the companion star, we find a
lower limit to the mass of the compact object in 2S 0921-630 of M_X sin^3 i >
1.90+-0.25 Msun (1 sigma errors). The inclination in this system is well
constrained since partial eclipses have been observed in X-rays and optical
bands. For inclinations between 60< i<90 degrees we find
1.90+-0.25<M_X<2.9+-0.4 Msun. However, using this maximum K-correction we find
that the ratio between the mass of the companion star and that of the compact
object, q, is 1.32+-0.37 implying super-Eddington mass transfer rates; however,
evidence for that has not been found in 2S 0921-630. We conclude that the
compact object in 2S 0921-630 is either a (massive) neutron star or a low-mass
black hole.Comment: 6 pages, 3 figures, accepted for publication in MNRA
Measurement of Relativistic Orbital Decay in the PSR B1534+12 Binary System
We have made timing observations of binary pulsar PSR B1534+12 with radio
telescopes at Arecibo, Green Bank, and Jodrell Bank. By combining our new
observations with data collected up to seven years earlier, we obtain a
significantly improved solution for the astrometric, spin, and orbital
parameters of the system. For the first time in any binary pulsar system, no
fewer than five relativistic or "post-Keplerian" orbital parameters are
measurable with useful accuracies in a theory-independent way. We find the
orbital period of the system to be decreasing at a rate close to that expected
from gravitational radiation damping, according to general relativity, although
the precision of this test is limited to about 15% by the otherwise poorly
known distance to the pulsar. The remaining post-Keplerian parameters are all
consistent with one another and all but one of them have fractional accuracies
better than 1%. By assuming that general relativity is the correct theory of
gravity, at least to the accuracy demanded by this experiment, we find the
masses of the pulsar and companion star each to be 1.339+-0.003 Msun and the
system's distance to be d = 1.1+-0.2 kpc, marginally larger than the d ~ 0.7
kpc estimated from the dispersion measure. The increased distance reduces
estimates of the projected rate of coalescence of double neutron-star systems
in the universe, a quantity of considerable interest for experiments with
terrestrial gravitational wave detectors such as LIGO.Comment: 17 pages, 4 figures, submitted to the Ap
The two-hour orbit of a binary millisecond X-ray pulsar
Typical radio pulsars are magnetized neutron stars that are born rapidly
rotating and slow down as they age on time scales of 10 to 100 million years.
However, millisecond radio pulsars spin very rapidly even though many are
billions of years old. The most compelling explanation is that they have been
"spun up" by the transfer of angular momentum during accretion of material from
a companion star in so-called low-mass X-ray binary systems, LMXBs. (LMXBs
consist of a neutron star or black hole accreting from a companion less than
one solar mass.) The recent detection of coherent X-ray pulsations with a
millisecond period from a suspected LMXB system appears to confirm this link.
Here we report observations showing that the orbital period of this binary
system is two hours, which establishes it as an LMXB. We also find an apparent
modulation of the X-ray flux at the orbital period (at the two per cent level),
with a broad minimum when the pulsar is behind this low-mass companion star.
This system seems closely related to the "black widow" millisecond radio
pulsars, which are evaporating their companions through irradiation. It may
appear as an eclipsing radio pulsar during periods of X-ray quiescence.Comment: 4 pages with 1 figure. Style files included. Fig. 2 deleted and text
revised. To appear in Nature. Press embargo until 18:00 GMT on 1998 July 2
EQ-5D in skin conditions: an assessment of validity and responsiveness
Aims and objectives This systematic literature review aims to assess the reliability, validity and responsiveness of three widely used generic preference-based measures of health-related quality of life (HRQL), i.e., EQ-5D, Health Utility Index 3 (HUI3) and SF-6D in patients with skin conditions. Methods A systematic search was conducted to identify studies reporting health state utility values obtained using EQ-5D, SF-6D, or HUI3 alongside other HRQL measures or clinical indices for patients with skin conditions. Data on test-retest analysis for reliability, known group differences or correlation and regression analyses for validity, and change over time or responsiveness indices analysis were extracted and reviewed. Results A total of 16 papers reporting EQ-5D utilities in people with skin conditions were included in the final review. No papers for SF-6D and HUI3 were found. Evidence of reliability was not found for any of these measures. The majority of studies included in the review (12 out of 16) examined patients with plaque psoriasis or psoriatic arthritis and the remaining four studies examined patients with either acne, hidradenitis suppurativa, hand eczema, or venous leg ulcers. The findings were generally positive in terms of performance of EQ-5D. Six studies showed that EQ-5D was able to reflect differences between severity groups and only one reported differences that were not statistically significant. Four studies found that EQ-5D detected differences between patients and the general population, and differences were statistically different for three of them. Further, moderate-to-strong correlation coefficients were found between EQ-5D and other skin-specific HRQL measures in four studies. Eight studies showed that EQ-5D was able to detect change in HRQL appropriately over time and the changes were statistically significant in seven studies. Conclusions Overall, the validity and responsiveness of the EQ-5D was found to be good in people with skin diseases, especially plaque psoriasis or psoriatic arthritis. No evidence on SF-6D and HUI3 was available to enable any judgments to be made on their performance
Cost-effectiveness analysis of 3-D computerized tomography colonography versus optical colonoscopy for imaging symptomatic gastroenterology patients.
BACKGROUND: When symptomatic gastroenterology patients have an indication for colonic imaging, clinicians have a choice between optical colonoscopy (OC) and computerized tomography colonography with three-dimensional reconstruction (3-D CTC). 3-D CTC provides a minimally invasive and rapid evaluation of the entire colon, and it can be an efficient modality for diagnosing symptoms. It allows for a more targeted use of OC, which is associated with a higher risk of major adverse events and higher procedural costs. A case can be made for 3-D CTC as a primary test for colonic imaging followed if necessary by targeted therapeutic OC; however, the relative long-term costs and benefits of introducing 3-D CTC as a first-line investigation are unknown. AIM: The aim of this study was to assess the cost effectiveness of 3-D CTC versus OC for colonic imaging of symptomatic gastroenterology patients in the UK NHS. METHODS: We used a Markov model to follow a cohort of 100,000 symptomatic gastroenterology patients, aged 50Â years or older, and estimate the expected lifetime outcomes, life years (LYs) and quality-adjusted life years (QALYs), and costs (ÂŁ, 2010-2011) associated with 3-D CTC and OC. Sensitivity analyses were performed to assess the robustness of the base-case cost-effectiveness results to variation in input parameters and methodological assumptions. RESULTS: 3D-CTC provided a similar number of LYs (7.737 vs 7.739) and QALYs (7.013 vs 7.018) per individual compared with OC, and it was associated with substantially lower mean costs per patient (ÂŁ467 vs ÂŁ583), leading to a positive incremental net benefit. After accounting for the overall uncertainty, the probability of 3-D CTC being cost effective was around 60Â %, at typical willingness-to-pay values of ÂŁ20,000-ÂŁ30,000 per QALY gained. CONCLUSION: 3-D CTC is a cost-saving and cost-effective option for colonic imaging of symptomatic gastroenterology patients compared with OC
The Parkes Multibeam Pulsar Survey: PSR J1811-1736 - a pulsar in a highly eccentric binary system
We are undertaking a high-frequency survey of the Galactic plane for radio
pulsars, using the 13-element multibeam receiver on the 64-m Parkes radio
telescope. We describe briefly the survey system and some of the initial
results. PSR J1811-1736, one of the first pulsars discovered with this system,
has a rotation period of 104 ms. Subsequent timing observations using the 76-m
radio telescope at Jodrell Bank show that it is in an 18.8-day,
highly-eccentric binary orbit. We have measured the rate of advance of
periastron which indicates a total system mass of 2.6 +- 0.9 Msun, and the
minimum companion mass is about 0.7 Msun. This, the high orbital eccentricity
and the recycled nature of the pulsar suggests that this system is composed of
two neutron stars, only the fourth or fifth such system known in the disk of
the Galaxy.Comment: 6 pages, 3 embedded EPS figures, to be published in MNRA
Timing stability of millisecond pulsars and prospects for gravitational-wave detection
Analysis of high-precision timing observations of an array of approx. 20
millisecond pulsars (a so-called "timing array") may ultimately result in the
detection of a stochastic gravitational-wave background. The feasibility of
such a detection and the required duration of this type of experiment are
determined by the achievable rms of the timing residuals and the timing
stability of the pulsars involved. We present results of the first long-term,
high-precision timing campaign on a large sample of millisecond pulsars used in
gravitational-wave detection projects. We show that the timing residuals of
most pulsars in our sample do not contain significant low-frequency noise that
could limit the use of these pulsars for decade-long gravitational-wave
detection efforts. For our most precisely timed pulsars, intrinsic
instabilities of the pulsars or the observing system are shown to contribute to
timing irregularities on a five-year timescale below the 100 ns level. Based on
those results, realistic sensitivity curves for planned and ongoing timing
array efforts are determined. We conclude that prospects for detection of a
gravitational-wave background through pulsar timing array efforts within five
years to a decade are good.Comment: 21 pages, 5 figures, submitted to MNRA
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