695 research outputs found
Measuring the spin up of the Accreting Millisecond Pulsar XTE J1751-305
We perform a timing analysis on RXTE data of the accreting millisecond pulsar
XTE J1751-305 observed during the April 2002 outburst. After having corrected
for Doppler effects on the pulse phases due to the orbital motion of the
source, we performed a timing analysis on the phase delays, which gives, for
the first time for this source, an estimate of the average spin frequency
derivative = (3.7 +/- 1.0)E-13 Hz/s. We discuss the torque resulting
from the spin-up of the neutron star deriving a dynamical estimate of the mass
accretion rate and comparing it with the one obtained from X-ray flux.
Constraints on the distance to the source are discussed, leading to a lower
limit of \sim 6.7 kpc.Comment: 7 pages, 3 figures, Accepted for publication by MNRA
Timing of the Accreting Millisecond Pulsar XTE J1814-338
We present a precise timing analysis of the accreting millisecond pulsar XTE
J1814-338 during its 2003 outburst, observed by RXTE. A full orbital solution
is given for the first time; Doppler effects induced by the motion of the
source in the binary system were corrected, leading to a refined estimate of
the orbital period, P_orb=15388.7229(2)s, and of the projected semimajor axis,
a sini/c= 390.633(9) lt-ms. We could then investigate the spin behaviour of the
accreting compact object during the outburst. We report here a refined value of
the spin frequency (nu=314.35610879(1) Hz) and the first estimate of the spin
frequency derivative of this source while accreting (nu^dot=(-6.7 +/- 0.7)
10^(-14) Hz/s). This spin down behaviour arises when both the fundamental
frequency and the second harmonic are taken into consideration. We discuss this
in the context of the interaction between the disc and the quickly rotating
magnetosphere, at accretion rates sufficiently low to allow a threading of the
accretion disc in regions where the Keplerian velocity is slower than the
magnetosphere velocity. We also present indications of a jitter of the pulse
phases around the mean trend, which we argue results from movements of the
accreting hotspots in response to variations of the accretion rate.Comment: 7 pages, 4 figures, Accepted for publication by MNRA
Timing of the accreting millisecond pulsar IGR~J17511--3057
{Timing analysis of Accretion-powered Millisecond Pulsars (AMPs) is a
powerful tool to probe the physics of compact objects. The recently discovered
\newigrj is the 12 discovered out of the 13 AMPs known. The Rossi XTE satellite
provided an extensive coverage of the 25 days-long observation of the source
outburst.} {Our goal is to investigate the complex interaction between the
neutron star magnetic field and the accretion disk, determining the angular
momentum exchange between them. The presence of a millisecond coherent flux
modulation allows us to investigate such interaction from the study of pulse
arrival times. In order to separate the neutron star proper spin frequency
variations from other effects, a precise set of orbital ephemeris is
mandatory.} {Using timing techniques, we analysed the pulse phase delays
fitting differential corrections to the orbital parameters. To remove the
effects of pulse phase fluctuations we applied the timing technique already
successfully applied to the case of an another AMP, XTE J1807-294.} {We report
a precise set of orbital ephemeris. We demonstrate that the companion star is a
main sequence star. We find pulse phase delays fluctuations on the first
harmonic with a characteristic amplitude of about 0.05, similar to what also
observed in the case of the AMP XTE J1814-338. For the second time an AMP shows
a third harmonic detected during the entire outburst. The first harmonic phase
delays show a puzzling behaviour, while the second harmonic phase delays show a
clear spin-up. Also the third harmonic shows a spin-up, although not highly
significant (3 c.l.). The presence of a fourth harmonic is also
reported. In the hypothesis that the second harmonic is a good tracer of the
spin frequency of the neutron star, we find a mean spin frequency derivative
for this source of \np{1.65(18)}{-13} Hz s.} (continue ...)Comment: 9 pages, 12 figures, A&A accepted on 23/10/201
Spin up and phase fluctuations in the timing of the accreting millisecond pulsar XTE J1807-294
We performed a timing analysis of the 2003 outburst of the accreting X-ray
millisecond pulsar XTE J1807-294 observed by RXTE. Using recently refined
orbital parameters we report for the first time a precise estimate of the spin
frequency and of the spin frequency derivative. The phase delays of the pulse
profile show a strong erratic behavior superposed to what appears as a global
spin-up trend. The erratic behavior of the pulse phases is strongly related to
rapid variations of the light curve, making it very difficult to fit these
phase delays with a simple law. As in previous cases, we have therefore
analyzed separately the phase delays of the first harmonic and of the second
harmonic of the spin frequency, finding that the phases of the second harmonic
are far less affected by the erratic behavior. In the hypothesis that the
second harmonic pulse phase delays are a good tracer of the spin frequency
evolution we give for the first time a estimation of the spin frequency
derivative in this source. The source shows a clear spin-up of Hz sec (1 confidence level). The
largest source of uncertainty in the value of the spin-up rate is given by the
uncertainties on the source position in the sky. We discuss this systematics on
the spin frequency and its derivative.Comment: 17 pages, 4 figures, Accepted by Ap
Order in the Chaos: Spin-up and Spin-down during the 2002 Outburst of SAX J1808.4–3658
We present a timing analysis of the 2002 outburst of the accreting millisecond pulsar SAX J1808.4-3658. A study of the phase delays of the entire pulse profile shows a behavior that is surprising and difficult to interpret: superposed to a general trend, a big jump by about 0.2 in phase is visible, starting at day 14 after the beginning of the outburst. An analysis of the pulse profile indicates the presence of a significant first harmonic. Studying the fundamental and the first harmonic separately, we find that the phase delays of the first harmonic are more regular, with no sign of the jump observed in the fundamental. The fitting of the phase delays of the first harmonic with a model which takes into account the observed exponential decay of the X-ray flux (and therefore of the mass accretion rate onto the neutron star) gives important information on the torque acting on the neutron star during the outburst. We find that the source shows spin-up in the first part of the outburst, while a spin-down dominates at the end. From these results we derive an estimate of the neutron star magnetic field strength
The Syrian public opinion versus frames in news media
The study aims at analyzing frames used by the media to report news about the Syrian crisis with the aim of understanding whether the Syrian voice -represented in public opinion data- finds its place in the media. The study conducts content analysis of 276 news stories\u27 frames divided across two periods of time -during 2015 (Obama\u27s administration) and 2017 (Trump\u27s administration). A content analysis methodology is applied to three online newspapers: the American New York Times, the Syrian Syria Times and the Russian Russia Beyond The Headlines. Each of these newspapers represents the governmental stance and policies in relation to the Syrian Crisis. The study attempts to have a deeper understanding of the interplay of powerful elites represented by the governments of the three countries and the Syrian people represented in public opinion polls. The media\u27s ultimate goal is serving public interest; however, and per the literature, the media can be used by elites to achieve wider acceptance of their policies regardless of the public interest (and their opinion in the matter)
Coupling Between Periodic and Aperiodic Variability in SAX J1808.4-3658
We detect a significant broadening in the wings of the 401 Hz peak in the
power spectrum of the accreting millisecond binary pulsar SAX J1808.4-3658.
This feature is consistent with the convolution of the red noise present in the
power spectrum with the harmonic line. We conclude that the flux modulated by
the spin period shows aperiodic variability similar to the red noise in the
overall flux, suggesting such variability also originates at the magnetic caps
close to the neutron star surface. This is analogous to the results found in
some longer period, higher magnetic field pulsators in high mass X-ray
binaries.Comment: 16 pages, 3 figures, to be published in The Astrophysical Journa
Cardiomyopathies: An overview
Background: Cardiomyopathies are a heterogeneous group of pathologies characterized by structural and functional alterations of the heart. Aims: The purpose of this narrative review is to focus on the most important cardiomyopathies and their epidemiology, diagnosis, and manage-ment. Methods: Clinical trials were identified by Pubmed until 30 March 2021. The search keywords were “cardiomyopathies, sudden cardiac arrest, dilated cardiomyopathy (DCM), hypertrophic car-diomyopathy (HCM), restrictive cardiomyopathy, arrhythmogenic cardiomyopathy (ARCV), tako-tsubo syndrome”. Results: Hypertrophic cardiomyopathy (HCM) is the most common primary car-diomyopathy, with a prevalence of 1:500 persons. Dilated cardiomyopathy (DCM) has a prevalence of 1:2500 and is the leading indication for heart transplantation. Restrictive cardiomyopathy (RCM) is the least common of the major cardiomyopathies, representing 2% to 5% of cases. Arrhythmogenic cardiomyopathy (ARCV) is a pathology characterized by the substitution of the myocardium by fibrofatty tissue. Takotsubo cardiomyopathy is defined as an abrupt onset of left ventricular dysfunction in response to severe emotional or physiologic stress. Conclusion: In particular, it has been reported that HCM is the most important cause of sudden death on the athletic field in the United States. It is needless to say how important it is to know which changes in the heart due to physical activity are normal, and when they are pathological
The near-IR counterpart of IGR J17480-2446 in Terzan 5
Some globular clusters in our Galaxy are noticeably rich in low-mass X-ray
binaries. Terzan 5 has the richest population among globular clusters of X- and
radio-pulsars and low-mass X-ray binaries. The detection and study of
optical/IR counterparts of low-mass X-ray binaries is fundamental to
characterizing both the low-mass donor in the binary system and investigating
the mechanisms of the formation and evolution of this class of objects. We aim
at identifying the near-IR counterpart of the 11 Hz pulsar IGRJ17480-2446
discovered in Terzan 5. Adaptive optics (AO) systems represent the only
possibility for studying the very dense environment of GC cores from the
ground. We carried out observations of the core of Terzan 5 in the near-IR
bands with the ESO-VLT NAOS-CONICA instrument. We present the discovery of the
likely counterpart in the Ks band and discuss its properties both in outburst
and in quiescence. Archival HST observations are used to extend our discussion
to the optical bands. The source is located at the blue edge of the turn-off
area in the color-magnitude diagram of the cluster. Its luminosity increase
from quiescence to outburst, by a factor 2.5, allows us to discuss the nature
of the donor star in the context of the double stellar generation population of
Terzan 5 by using recent stellar evolution models.Comment: 7 pages, 4 figure
Timing an Accreting Millisecond Pulsar: Measuring the Accretion Torque in IGR J00291+5934
We present here a timing analysis of the fastest accreting millisecond pulsar
IGR J00291+5934 using RXTE data taken during the outburst of December 2004. We
corrected the arrival times of all the events for the orbital (Doppler) effects
and performed a timing analysis of the resulting phase delays. In this way we
find a clear parabolic trend of the pulse phase delays showing that the pulsar
is spinning up as a consequence of accretion torques during the X-ray outburst.
The accretion torque gives us for the first time an independent estimate of the
mass accretion rate onto the neutron star, which can be compared with the
observed X-ray luminosity. We also report a revised value of the spin period of
the pulsar.Comment: Proceedings of the Frascati Workshop 2005: Multifrequency Behaviour
of High Energy Cosmic Sources, Vulcano, May 23-28. 7 pages including 1 figur
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