49 research outputs found
A Modified TreePM Code
We discuss the performance characteristics of using the modification of the
tree code suggested by Barnes \citep{1990JCoPh..87..161B} in the context of the
TreePM code. The optimisation involves identifying groups of particles and
using only one tree walk to compute force for all the particles in the group.
This modification has been in use in our implementation of the TreePM code for
some time, and has also been used by others in codes that make use of tree
structures. In this paper, we present the first detailed study of the
performance characteristics of this optimisation. We show that the
modification, if tuned properly can speed up the TreePM code by a significant
amount. We also combine this modification with the use of individual time steps
and indicate how to combine these two schemes in an optimal fashion. We find
that the combination is at least a factor of two faster than the modified
TreePM without individual time steps. Overall performance is often faster by a
larger factor, as the scheme of groups optimises use of cache for large
simulations.Comment: 16 pages, 5 figures; Accepted for publication in Research In
Astronomy and Astrophysics (RAA
Wormhole with varying cosmological constant
It has been suggested that the cosmological constant is a variable dynamical
quantity. A class of solution has been presented for the spherically symmetric
space time describing wormholes by assuming the erstwhile cosmological constant
to be a space variable scalar, viz., = . It
is shown that the Averaged Null Energy Condition (ANEC) violating exotic matter
can be made arbitrarily small.Comment: 8 pages, 2 figures, Accepted in Gen. Rel. Gra
Phenomenology of -CDM model: a possibility of accelerating Universe with positive pressure
Among various phenomenological models, a time-dependent model is selected here to investigate the -CDM cosmology.
Using this model the expressions for the time-dependent equation of state
parameter and other physical parameters are derived. It is shown that
in model accelerated expansion of the Universe takes place at negative
energy density, but with a positive pressure. It has also been possible to
obtain the change of sign of the deceleration parameter during cosmic
evolution.Comment: 16 Latex pages, 11 figures, Considerable modifications in the text;
Accepted in IJT
Robotic ubiquitous cognitive ecology for smart homes
Robotic ecologies are networks of heterogeneous robotic devices pervasively embedded in everyday environments, where they cooperate to perform complex tasks. While their potential makes them increasingly popular, one fundamental problem is how to make them both autonomous and adaptive, so as to reduce the amount of preparation, pre-programming and human supervision that they require in real world applications. The project RUBICON develops learning solutions which yield cheaper, adaptive and efficient coordination of robotic ecologies. The approach we pursue builds upon a unique combination of methods from cognitive robotics, machine learning, planning and agent- based control, and wireless sensor networks. This paper illustrates the innovations advanced by RUBICON in each of these fronts before describing how the resulting techniques have been integrated and applied to a smart home scenario. The resulting system is able to provide useful services and pro-actively assist the users in their activities. RUBICON learns through an incremental and progressive approach driven by the feed- back received from its own activities and from the user, while also self-organizing the manner in which it uses available sensors, actuators and other functional components in the process. This paper summarises some of the lessons learned by adopting such an approach and outlines promising directions for future work
Neutrino Mass Limit from Galaxy Cluster Number Density Evolution
Measurements of the evolution with redshift of the number density of massive
galaxy clusters are used to constrain the energy density of massive neutrinos
and so the sum of neutrino masses . We consider a spatially-flat
cosmological model with cosmological constant, cold dark matter, baryonic
matter, and massive neutrinos. Accounting for the uncertainties in the
measurements of the relevant cosmological parameters we obtain a limit of 2.4 eV (95 % C.L.).Comment: 6 pages, 2 figures and references added, accepted for publication in
Phys. Rev.
Minimum mass-radius ratio for charged gravitational objects
We rigorously prove that for compact charged general relativistic objects
there is a lower bound for the mass-radius ratio. This result follows from the
same Buchdahl type inequality for charged objects, which has been extensively
used for the proof of the existence of an upper bound for the mass-radius
ratio. The effect of the vacuum energy (a cosmological constant) on the minimum
mass is also taken into account. Several bounds on the total charge, mass and
the vacuum energy for compact charged objects are obtained from the study of
the Ricci scalar invariants. The total energy (including the gravitational one)
and the stability of the objects with minimum mass-radius ratio is also
considered, leading to a representation of the mass and radius of the charged
objects with minimum mass-radius ratio in terms of the charge and vacuum energy
only.Comment: 19 pages, accepted by GRG, references corrected and adde
CMB power spectrum estimation with non-circular beam and incomplete sky coverage
Over the last decade, measurements of the CMB anisotropy has spearheaded the
remarkable transition of cosmology into a precision science. However,
addressing the systematic effects in the increasingly sensitive, high
resolution, `full' sky measurements from different CMB experiments pose a stiff
challenge. The analysis techniques must not only be computationally fast to
contend with the huge size of the data, but, the higher sensitivity also limits
the simplifying assumptions which can then be invoked to achieve the desired
speed without compromising the final precision goals. While maximum likelihood
is desirable, the enormous computational cost makes the suboptimal method of
power spectrum estimation using Pseudo-C_l unavoidable for high resolution
data. We provide a (semi)analytic framework to estimate bias in the power
spectrum due to the effect of beam non-circularity and non-uniform sky coverage
including incomplete/masked sky maps and scan strategy. The approach is
perturbative in the distortion of the beam from non-circularity, allowing for
rapid computations when the beam is mildly non-circular. We advocate that it is
computationally advantageous to employ `soft' azimuthally apodized masks whose
spherical harmonic transform die down fast with m. We numerically implement our
method for non-rotating beams. We present preliminary estimates of the
computational cost to evaluate the bias for the upcoming CMB anisotropy probes
l_max~3000, with angular resolution comparable to the Planck surveyor mission.
We further show that this implementation and estimate is applicable for
rotating beams on equal declination scans and possibly can be extended to
simple approximations to other scan strategies.Comment: 22 pages, 7 figures. Revised presentation to highlight significance
of extended results. Matches version accepted to the MNRA
Stochastic motion of test particle implies that G varies with time
The aim of this letter is to propose a new description to the time varying
gravitational constant problem, which naturally implements the Dirac's large
numbers hypothesis in a new proposed holographic scenario for the origin of
gravity as an entropic force. We survey the effect of the Stochastic motion of
the test particle in Verlinde's scenario for gravity\cite{Verlinde}. Firstly we
show that we must get the equipartition values for which
leads to the usual Newtonian gravitational constant. Secondly,the stochastic
(Brownian) essence of the motion of the test particle, modifies the Newton's
2'nd law. The direct result is that the Newtonian constant has been time
dependence in resemblance as \cite{Running}.Comment: Accepted in International Journal of Theoretical Physic
A Better Way to Reconstruct Dark Energy Models ?
To reconstruct dark energy models the redshift , marking the end of
radiation era and the beginning of matter-dominated era, can play a role as
important as , the redshift at which deceleration parameter experiences
a signature flip. To implement the idea we propose a variable equation of state
for matter that can bring a smooth transition from radiation to
matter-dominated era in a single model. A popular dark
energy model is chosen for demonstration but found to be unacceptable. An
alternative model is proposed and found to be more
close to observation.Comment: 17 pages, 5 figures Accepted for publication in `Astrophysics and
Space Science
Statefinder Parameter for Varying G in Three Fluid System
In this work, we have considered variable G in flat FRW universe filled with
the mixture of dark energy, dark matter and radiation. If there is no
interaction between the three fluids, the deceleration parameter and
statefinder parameters have been calculated in terms of dimensionless density
parameters which can be fixed by observational data. Also the interaction
between three fluids has been analyzed due to constant . The statefinder
parameters also calculated in two cases: pressure is constant and pressure is
variable.Comment: 5 pages, Accepted for publication in "Astrophysics and Space Science