702 research outputs found
The Parkes Pulsar Timing Array
Detection and study of gravitational waves from astrophysical sources is a
major goal of current astrophysics. Ground-based laser-interferometer systems
such as LIGO and VIRGO are sensitive to gravitational waves with frequencies of
order 100 Hz, whereas space-based systems such as LISA are sensitive in the
millihertz regime. Precise timing observations of a sample of millisecond
pulsars widely distributed on the sky have the potential to detect
gravitational waves at nanohertz frequencies. Potential sources of such waves
include binary super-massive black holes in the cores of galaxies, relic
radiation from the inflationary era and oscillations of cosmic strings. The
Parkes Pulsar Timing Array (PPTA) is an implementation of such a system in
which 20 millisecond pulsars have been observed using the Parkes radio
telescope at three frequencies at intervals of two -- three weeks for more than
two years. Analysis of these data has been used to limit the gravitational wave
background in our Galaxy and to constrain some models for its generation. The
data have also been used to investigate fluctuations in the interstellar and
Solar-wind electron density and have the potential to investigate the stability
of terrestrial time standards and the accuracy of solar-system ephemerides.Comment: 9 pages, 6 figures, Proceedings of "40 Years of Pulsars: Millisecond
Pulsars, Magnetars and More", Montreal, August 2007. Corrected SKA detection
limi
Radio Emission Signatures in the Crab Pulsar
Our high time resolution observations of individual pulses from the Crab
pulsar show that both the time and frequency signatures of the interpulse are
distinctly different from those of the main pulse. Main pulses can occasionally
be resolved into short-lived, relatively narrow-band nanoshots. We believe
these nanoshots are produced by soliton collapse in strong plasma turbulence.
Interpulses at centimeter wavelengths are very different. Their dynamic
spectrum contains regular, microsecond-long emission bands. We have detected
these bands, proportionately spaced in frequency, from 4.5 to 10.5 GHz. The
bands cannot easily be explained by any current theory of pulsar radio
emission; we speculate on possible new models.Comment: 26 pages, 10 figures, to appear in Ap
Observations of Six Glitches in PSR B1737-30
Six glitches have been recently observed in the rotational frequency of the
young pulsar PSR B1737-30 (J1740-3015) using the 25-m Nanshan telescope of
Urumqi Observatory. With a total of 20 glitches in 20 years, it is one of the
most frequently glitching pulsars of the about 1750 known pulsars. Glitch
amplitudes are very variable with fractional increases in rotation rate ranging
from 10^{-9} to 10^{-6}. Inter-glitch intervals are also very variable, but no
relationship is observed between interval and the size of the preceding glitch.
There is a persistent increase in |\dot\nu|, opposite in sign to that expected
from slowdown with a positive braking index, which may result from changes in
the effective magnetic dipole moment of the star during the glitch.Comment: 7 pages, 10 figure
Timing measurements and proper motions of 74 pulsars using the Nanshan radio telescope
We have measured the positions of 74 pulsars from regular timing observations
using the Nanshan radio telescope at Urumqi Observatory between 2000 January
and 2004 August (MJD 51500 -- 53240). Proper motions were determined for these
pulsars by comparing their current positions with positions given in pulsar
catalogues. We compare our results to earlier measurements in the literature
and show that, in general, the values agree. New or improved proper motions are
obtained for 16 pulsars. The effect of period fluctuations and other timing
noise on the determination of pulsar positions is investigated. For our sample,
the mean and rms transverse velocities are 443 and 224 km/s respectively,
agreeing with previous work even though we determine distances using the new
NE2001 electron density model.Comment: 9 pages, 7 figures and 3 tables. Accepted by MNRA
On the peculiarities in the rotational frequency evolution of isolated neutron stars
The measurements of pulsar frequency second derivatives have shown that they
are times larger than expected for standard pulsar spin-down law,
and are even negative for about half of pulsars. We explain these paradoxical
results on the basis of the statistical analysis of the rotational parameters
, and of the subset of 295 pulsars taken mostly
from the ATNF database. We have found a strong correlation between
and for both and , as well as between
and . We interpret these dependencies as evolutionary ones due
to being nearly proportional to the pulsars' age. The derived
statistical relations as well as "anomalous" values of are well
described by assuming the long-time variations of the spin-down rate. The
pulsar frequency evolution, therefore, consists of secular change of
, and according to the power
law with , the irregularities, observed within a timespan as a
timing noise, and the variations on the timescale larger than that timespan --
several tens of years.Comment: 4 pages, 3 figures. Accepted for publication in ApSS, in the
proceedings of the conference "Isolated Neutron Stars: from the Interior to
the Surface", London, April 2006; eds. S. Zane, R. Turolla and D. Pag
Constraining the coalescence rate of supermassive black-hole binaries using pulsar timing
Pulsar timing observations are used to place constraints on the rate of
coalescence of supermassive black-hole (SMBH) binaries as a function of mass
and redshift. In contrast to the indirect constraints obtained from other
techniques, pulsar timing observations provide a direct constraint on the
black-hole merger rate. This is possible since pulsar timing is sensitive to
the gravitational waves (GWs) emitted by these sources in the final stages of
their evolution. We find that upper bounds calculated from the recently
published Parkes Pulsar Timing Array data are just above theoretical
predictions for redshifts below 10. In the future, with improved timing
precision and longer data spans, we show that a non-detection of GWs will rule
out some of the available parameter space in a particular class of SMBH binary
merger models. We also show that if we can time a set of pulsars to 10ns timing
accuracy, for example, using the proposed Square Kilometre Array, it should be
possible to detect one or more individual SMBH binary systems
Unusual glitch behaviours of two young pulsars
In this paper we report unusual glitches in two young pulsars, PSR J1825-0935
(B1822-09) and PSR J1835-1106. For PSR J1825-0935, a slow glitch characterised
by a temporary decrease in the slowdown rate occurred between 2000 December 31
to 2001 December 6. This event resulted in a permanent increase in frequency
with fractional size , however little
effect remained in slowdown rate. The glitch in PSR J1835-1106 occurred
abruptly in November 2001 (MJD 52220\pm3) with
and little or no change in the
slow-down rate. A significant change in apparently occurred at the
glitch with having opposite sign for the pre- and post-glitch data.Comment: Latex format, six files, 5 pages with 4 figues. accepted for MNRA
- …