631 research outputs found
New Limits on Gravitational Radiation using Pulsars
We calculate a new gravitational wave background limit using timing residuals
from PSRs J1713+0747, B1855+09, and B1937+21. The new limit is based on 17
years of continuous data pieced together from 3 different observing projects: 2
at the Arecibo Observatory and 1 at the 140ft Green Bank Telescope. This
project represents the earliest results from the `Pulsar Timing Array' which
will soon be able detect the stochastic background from early massive black
hole mergers.Comment: 12 pages, 11 figures, 3 tables. To appear in the Proceedings of the
270. WE-Heraeus Seminar on Neutron Stars, Pulsars and Supernova Remnants,
Jan. 21-25, 2002, Physikzentrum Bad Honnef, eds W. Becker, H. Lesch & J.
Truemper. Proceedings are available as MPE-Report 27
Analysis of Seed Potato Systems in Ethiopia
This study aimed to analyze the seed potato systems in Ethiopia, identify constraints and prioritize improvement options, combining desk research, rapid appraisal and formal surveys, expert elicitation, field observations and local knowledge. In Ethiopia, informal, alternative and formal seed systems co-exist. The informal system, with low quality seed, is dominant. The formal system is too small to contribute significantly to improve that situation. The informal seed system should prioritize improving seed quality by increasing awareness and skills of farmers, improving seed tuber quality of early generations and market access. The alternative and formal seed systems should prioritize improving the production capacity of quality seed by availing new varieties, designing quality control methods and improving farmer’s awareness. To improve overall seed potato supply in Ethiopia, experts postulated co-existence and linkage of the three seed systems and development of self-regulation and selfcertification in the informal, alternative and formal cooperative seed potato systems. Resumen Este estudio tuvo el propósito de analizar los sistemas de producción de papa en Etiopia, identificar limitantes, y priorizar opciones de mejorar, mediante la combinación de investigación de escritorio, apreciaciones rápidas y estudios formales, encuestas a expertos, observaciones de campo y conocimiento local. En Etiopia co-existen sistemas de semilla informal, alternativo y formal. Domina el sistema informal, con baja calidad de semilla. El sistema formal es muy pequeño como para contribuir significativamente al mejoramiento de esa situación. El sistema informal de semilla debería tener como prioridad el mejoramiento en la calidad de la semilla mediante el aumento en la atención y habilidades de los productores, mejorando la calidad de la semilla-tubérculo de las generaciones tempranas y el acceso al mercado. Los sistemas alternativo y formal de semilla deberían priorizar el mejoramiento en la capacidad de producción de semilla de calidad, mediante la validación de nuevas variedades, el diseño de métodos de control de calidad, y mejorando la atención del productor. Para mejorar el suministro general de semilla de papa en Etiopia, los expertos postularon la co-existencia y asociación de los tres sistemas de semillas y el desarrollo de autorregulación y autocertificación en los sistemas cooperativos de semilla de papa informal, alternativo y formal. Keywords Potato . Seed quality . Seed tuber . Seed system . Quality improvement . Expert elicitation . Solanum tuberosum Introductio
Quantum effects in gravitational wave signals from cuspy superstrings
We study the gravitational emission, in Superstring Theory, from fundamental
strings exhibiting cusps. The classical computation of the gravitational
radiation signal from cuspy strings features strong bursts in the special null
directions associated to the cusps. We perform a quantum computation of the
gravitational radiation signal from a cuspy string, as measured in a
gravitational wave detector using matched filtering and located in the special
null direction associated to the cusp. We study the quantum statistics
(expectation value and variance) of the measured filtered signal and find that
it is very sharply peaked around the classical prediction. Ultimately, this
result follows from the fact that the detector is a low-pass filter which is
blind to the violent high-frequency quantum fluctuations of both the string
worldsheet, and the incoming gravitational field.Comment: 16 pages, no figur
Gravitational Wave Hotspots: Ranking Potential Locations of Single-Source Gravitational Wave Emission
The steadily improving sensitivity of pulsar timing arrays (PTAs) suggests
that gravitational waves (GWs) from supermassive black hole binary (SMBHB)
systems in the nearby universe will be de- tectable sometime during the next
decade. Currently, PTAs assume an equal probability of detection from every sky
position, but as evidence grows for a non-isotropic distribution of sources, is
there a most likely sky position for a detectable single source of GWs? In this
paper, a collection of galactic catalogs is used to calculate various metrics
related to the detectability of a single GW source resolv- able above a GW
background, assuming that every galaxy has the same probability of containing a
SMBHB. Our analyses of these data reveal small probabilities that one of these
sources is currently in the PTA band, but as sensitivity is improved regions of
consistent probability density are found in predictable locations, specifically
around local galaxy clusters.Comment: 9 pages, 9 figures, accepted for submission in Ap
Gravitational Waves Probe the Coalescence Rate of Massive Black Hole Binaries
We calculate the expected nHz--Hz gravitational wave (GW) spectrum from
coalescing Massive Black Hole (MBH) binaries resulting from mergers of their
host galaxies. We consider detection of this spectrum by precision pulsar
timing and a future Pulsar Timing Array. The spectrum depends on the merger
rate of massive galaxies, the demographics of MBHs at low and high redshift,
and the dynamics of MBH binaries. We apply recent theoretical and observational
work on all of these fronts. The spectrum has a characteristic strain
, just below the detection limit from
recent analysis of precision pulsar timing measurements. However, the amplitude
of the spectrum is still very uncertain owing to approximations in the
theoretical formulation of the model, to our lack of knowledge of the merger
rate and MBH population at high redshift, and to the dynamical problem of
removing enough angular momentum from the MBH binary to reach a GW-dominated
regime.Comment: 31 Pages, 8 Figures, small changes to match the published versio
Constraints on cosmic string tension imposed by the limit on the stochastic gravitational wave background from the European Pulsar Timing Array
We investigate the constraints that can be placed on the cosmic string
tension by using the current Pulsar Timing Array limits on the stochastic
gravitational wave background (SGWB). We have developed a code to compute the
spectrum of gravitational waves (GWs) based on the widely accepted one-scale
model. In its simplest form the one-scale model allows one to vary: (i) the
string tension, G\mu/c^2; (ii) the size of cosmic string loops relative to the
horizon at birth, \alpha; (iii) the spectral index of the emission spectrum, q;
(iv) the cut-off in the emission spectrum, n_*; and (v) the intercommutation
probability, p. The amplitude and slope of the spectrum in the nHz frequency
range is very sensitive to these unknown parameters. We have also investigated
the impact of more complicated scenarios with multiple initial loop sizes, in
particular the 2-\alpha models proposed in the literature and a log-normal
distribution for \alpha. We have computed the constraint on G\mu/c^2 due to the
limit on a SGWB imposed by data from the European Pulsar Timing Array. Taking
into account all the possible uncertainties in the parameters we find a
conservative upper limit of G\mu/c^2<5.3x 10^{-7} which typically occurs when
the loop production scale is close to the gravitational backreaction scale,
\alpha\approx\Gamma G\mu/c^2. Stronger limits are possible for specific values
of the parameters which typically correspond to the extremal cases \alpha\ll
\Gamma G\mu/c^2 and \alpha\gg \Gamma G\mu/c^2. This limit is less stringent
than the previously published limits which are based on cusp emission, an
approach which does not necessarily model all the possible uncertainties. We
discuss the prospects for lowering this limit by two orders of magnitude, or
even a detection of the SGWB, in the very near future in the context of the
Large European Array for Pulsars and the Square Kilometre Array.Comment: 24 pages, 14 figures, accepted for publication in Physical Review D.
Minor corrections and additional comments - updated to match the published
versio
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