26,769 research outputs found
Spark Model for Pulsar Radiation Modulation Patterns
A non-stationary polar gap model first proposed by Ruderman & Sutherland
(1975) is modified and applied to spark-associated pulsar emission at radio
wave-lengths. It is argued that under physical and geometrical conditions
prevailing above pulsar polar cap, highly non-stationary spark discharges do
not occur at random positions. Instead, sparks should tend to operate in well
determined preferred regions. At any instant the polar cap is populated as
densely as possible with a number of two-dimensional sparks with a
characteristic dimension as well as a typical distance between adjacent sparks
being about the polar gap height. Our model differs, however, markedly from its
original 'hollow cone' version. The key feature is the quasi-central spark
driven by pair production process and anchored to the local pole of a
sunspot-like surface magnetic field. This fixed spark prevents the motion of
other sparks towards the pole, restricting it to slow circumferential drift
across the planes of field lines converging at the local pole. We argue that
the polar spark constitutes the core pulsar emission, and that the annular
rings of drifting sparks contribute to conal components of the pulsar beam. We
found that the number of nested cones in the beam of typical pulsar should not
excced three; a number also found by Mitra & Deshpande (1999) using a
completely different analysis.Comment: 31 pages, 8 figures, accepted by Ap
Time-scales of Radio Emission in PSR J0437-4715 at 327 MHz
Time-scales of radio emission are studied in PSR J0437-4715 at 327 MHz using
almost half a million periods of high quality data from Ooty Radio Telescope.
The radio emission in this milli second pulsar occurs on a short (s) time-scale
of approximately 0.026 +- 0.001 periods, and on a (l) time-scale that is much
longer than the widths of the components of the integrated profile
(approximately 0.05 periods). The width of the s emission increases with its
increasing relative contribution to the total radio emission. This may provide
constraints for the details of discharge of vacuum gaps above pulsar polar
caps. The s emission occasionally takes place in the form of intense spikes,
which are confined to the main component of the integrated profile for 90 per
cent of the time. The positions of spikes within a component of the integrated
profile have no simple relation to the shape of that component. This may have
impact on the interpretation of the integrated profile components in terms of
independent regions of emission on the polar cap.Comment: Accepted for publication in Vol 543 (1 Nov 2000) of The Astrophysical
Journa
Frequency dependence of pulsar radiation patterns
We report on new results from simultaneous, dual frequency, single pulse
observation of PSR B0329+54 using the Giant Metrewave Radio Telescope. We find
that the longitude separation of subpulses at two different frequencies (238
and 612 MHz) is less than that for the corresponding components in the average
profile. A similar behaviour has been noticed before in a number of pulsars. We
argue that subpulses are emitted within narrow flux tubes of the dipolar field
lines and that the mean pulsar beam has a conal structure. In such a model the
longitudes of profile components are determined by the intersection of the line
of sight trajectory with subpulse-associated emission beams. Thus, we show that
the difference in the frequency dependence of subpulse and profile component
longitudes is a natural property of the conal model of pulsar emission beam. We
support our conclusions by numerical modelling of pulsar emission, using the
known parameters for this pulsar, which produce results that agree very well
with our dual frequency observations.Comment: 24 pages, 8 figures. Accepted for publication in Ap
Spot-like Structures of Neutron Star Surface Magnetic Fields
There is growing evidence, based on both X-ray and radio observations of
isolated neutron stars, that besides the large--scale (dipolar) magnetic field,
which determines the pulsar spin--down behaviour, small--scale poloidal field
components are present, which have surface strengths one to two orders of
magnitude larger than the dipolar component. We argue in this paper that the
Hall--effect can be an efficient process in producing such small--scale field
structures just above the neutron star surface. It is shown that due to a
Hall--drift induced instability, poloidal magnetic field structures can be
generated from strong subsurface toroidal fields, which are the result of
either a dynamo or a thermoelectric instability acting at early times of a
neutron star's life. The geometrical structure of these small--scale surface
anomalies of the magnetic field resembles that of some types of
``star--spots''. The magnetic field strength and the length--scales are
comparable with values that can be derived from various observations.Comment: 4 pages, 2 figures, accepted by Astronomy & Astrophysics Letters;
language improved, 2nd para of Sect. 3 change
Asymptotic approximations to the nodes and weights of Gauss-Hermite and Gauss-Laguerre quadratures
Asymptotic approximations to the zeros of Hermite and Laguerre polynomials
are given, together with methods for obtaining the coefficients in the
expansions. These approximations can be used as a standalone method of
computation of Gaussian quadratures for high enough degrees, with Gaussian
weights computed from asymptotic approximations for the orthogonal polynomials.
We provide numerical evidence showing that for degrees greater than the
asymptotic methods are enough for a double precision accuracy computation
(- digits) of the nodes and weights of the Gauss--Hermite and
Gauss--Laguerre quadratures.Comment: Submitted to Studies in Applied Mathematic
Computation of the Marcum Q-function
Methods and an algorithm for computing the generalized Marcum function
() and the complementary function () are described.
These functions appear in problems of different technical and scientific areas
such as, for example, radar detection and communications, statistics and
probability theory, where they are called the non-central chi-square or the non
central gamma cumulative distribution functions.
The algorithm for computing the Marcum functions combines different methods
of evaluation in different regions: series expansions, integral
representations, asymptotic expansions, and use of three-term homogeneous
recurrence relations. A relative accuracy close to can be obtained
in the parameter region ,
, while for larger parameters the accuracy decreases (close to
for and close to for ).Comment: Accepted for publication in ACM Trans. Math. Soft
Discovery of a remarkable subpulse drift pattern in PSR B0818-41
We report the discovery of a remarkable subpulse drift pattern in the
relatively less studied wide profile pulsar, B0818-41, using high sensitivity
GMRT observations. We find simultaneous occurrence of three drift regions with
two different drift rates: an inner region with steeper apparent drift rate
flanked on each side by a region of slower apparent drift rate. Furthermore,
these closely spaced drift bands always maintain a constant phase relationship.
Though these drift regions have significantly different values for the measured
P2, the measured P3 value is the same and equal to 18.3 P1. We interpret the
unique drift pattern of this pulsar as being created by the intersection of our
line of sight (LOS) with two conal rings on the polar cap of a fairly aligned
rotator (inclination angle alpha ~ 11 deg), with an ``inner'' LOS geometry
(impact angle beta ~ -5.4 deg). We argue that both the rings have the same
values for the carousel rotation periodicity P4 and the number of sparks Nsp.
We find that Nsp is 19-21 and show that it is very likely that, P4 is the same
as the measured P3, making it a truly unique pulsar. We present results from
simulations of the radiation pattern using the inferred parameters, that
support our interpretations and reproduce the average profile as well as the
observed features in the drift pattern quite well.Comment: 5 pages and 7 figures, Accepted for publication in MNRAS Letter
Threshold Effects And Perturbative Unification
We discuss the effect of the renormalization procedure in the computation of
the unification point for running coupling constants. We explore the effects of
threshold--crossing on the --functions. We compute the running of the
coupling constants of the Standard Model, between and , using a mass
dependent subtraction procedure, and then compare the results with ,
and with the -- function approximation. We also do this for the Minimal
Supersymmetric extension of the Standard Model. In the latter, the bounds on
susy masses that one obtains by requiring perturbative unification are
dependent, to some extent, on the procedure.Comment: 22 pages, REVTEX-2.1, 6 Post-Script figures are include
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