129 research outputs found
TEMPO2: a new pulsar timing package - III. Gravitational wave simulation
No full textG. Hobbs, F. Jenet, K. J. Lee, J. P. W. Verbiest, D. Yardley, R. Manchester, A. Lommen, W. Coles, R. Edwards and C. Shettigar
Using pulsars to limit the existence of a gravitational wave background
No full textHobbs G, Jenet F, Lommen A, et al. Using pulsars to limit the existence of a gravitational wave background. In: Bassa C, Wang Z, Cumming A, Kaspi VM, eds. 40 years of pulsars : millisecond pulsars, magnetars and more. AIP Conference Proceedings. Vol 983. Melville, NY: AIP Press; 2008: 630
Napier, Jenet (Death, 1888-11-27)
No full textAddress: Glanway Ave.Age at death: 65 yrsPg 129/1888/337/F W W/Scotland/Dr. W. E. De Courcy/J. F. Wiltsee/Spring GroveOriginal record filed in drawer labeled 'N-NEHM'
Detecting the stochastic gravitational wave background using pulsar timing
No full textThe direct detection of gravitational waves is a major goal of current astrophysics. We provide details of a new method for detecting a stochastic background of gravitational waves using pulsar timing data. Our results show that regular timing observations of 40 pulsars each with a timing accuracy of 100 ns will be able to make a direct detection of the predicted stochastic background from coalescing black holes within 5 years. With an improved prewhitening algorithm, or if the background is at the upper end of the predicted range, a significant detection should be possible with only 20 pulsars.http://gateway.webofknowledge.com/gateway/Gateway.cgi?GWVersion=2&SrcApp=PARTNER_APP&SrcAuth=LinksAMR&KeyUT=WOS:000229437000014&DestLinkType=FullRecord&DestApp=ALL_WOS&UsrCustomerID=8e1609b174ce4e31116a60747a720701Astronomy & AstrophysicsSCI(E)150ARTICLE2L123-L12662
Verbal Bullying Experienced by Male Cheerleader Characters in Peyton Reed’s Movie Entitled Bring It on (2000)
No full textJalatirani, Dominika Jenetaugusta. Verbal Bullying Experienced By Male Cheerleader
Characters In Peyton Reed’s Movie Entitled Bring It On (2000). Thesis. Supervisor 1 : Lynda
Susana Widya A F, S.S., M.Hum., Supervisor 2 : Eni Nur Aeni, S.S., M.A., External Examiner :
Dra. Mimien Aminah Sudjaie, M.A. Minister of Research, Technology and Higher Education,
Jenderal Soedirman University, Faculty of Humanities, English Departement, English Literature
Study Program, Purwokerto.
This research entitled ''Verbal Bullying Experienced by Cheerleader Male Characters in
Peyton reed's Movie Bring It On (2000)'' is aimed to find out the form of verbal bullying
experienced by male characters who become member of cheerleader in the movie. Furthermore, it
also explains the background of bullying especially through verbal offense that happens in people's
neighbourhoods nowadays. In this research, qualitative method is used for analyzing the data. The
primary data in this research is the movie, Bring It On (2000) directed by Peyton Reed. In addition,
the points concerning verbal bullying will be the grand theory of this research with verbal insult
as the main focus of the research. The result of this research shows that the Label of Homosexual
and Sissy given by the other character toward male cheerleader members will lead into Verbal
insult act. Then from verbal insults act by another character it will produce Anger and Disapproval
for Cheerleader Male Character as Impact of Verbal Bullying in bring it on movie
Timing as a probe of non-Einsteinian polarizations of gravitational waves
No full textEinstein's theory of gravity predicts waves of the distortion of spacetime with two degrees of polarization; alternative theories predict more polarizations, up to a maximum of six. Although laser interferometric gravity wave detectors can be used to search for at least some of the non-Einsteinian polarizations, their configuration is not optimal for the task. By contrast, the angular distribution of pulsars in the sky makes pulsar timing a flexible tool for detecting all polarizations. We give here an analysis of the sensitivity of pulsar timing to an isotropic stochastic gravitational wave background of waves with non-Einsteinian polarizations and conclude that their detection may be feasible in the near future. In particular, we compute the number of pulsars necessary to detect a stochastic background made up of one type of polarization and to distinguish non-Einsteinian from standard polarizations. We conclude that for biweekly observations made for five years with rms timing accuracy of 100 ns, detecting non-Einsteinian modes will require: 60 pulsars in the case of the longitudinal mode; 60 for the two spin-1 "shear'' modes; and 40 for the spin-0 "breathing'' mode. These are targets that should be easily achievable with the proposed Square Kilometer Array project. To discriminate non-Einsteinian modes from Einsteinian modes, we need 40 pulsars for the breathing mode, 100 pulsars for the longitudinal mode, and 500 pulsars for the shear mode. We confirm the previous estimate that 40 pulsars are needed to detect the spin-2 "transverse'' (Einsteinian) polarizations. Better focused statistical tests may allow improvements in sensitivity for some of these polarizations.Astronomy & AstrophysicsSCI(E)44ARTICLE21304-131968
Pulsar timing sensitivity to very-low-frequency gravitational waves
No full textWe compute the sensitivity, constrained by instrumental, propagation, and other fundamental noises, of pulsar timing to very-low-frequency gravitational waves (GWs). Reaching predicted GW signal strengths will require suppression of time-of-arrival fluctuations caused by interstellar plasma turbulence and a reduction of white rms timing noise to ≲100 ns. Assuming negligible intrinsic pulsar rotational noise, perfect time transfer from time standard to observatory, and stable pulse profiles, the resulting single-pulsar signal-to-noise ratio=1 sensitivity is limited by terrestrial time standards at ℎrms∼2×10−16 [f/(1 cycle/year)]−1/2 for \u3c3×10−8 Hz, where f is the Fourier frequency and a bandwidth of 1 cycle/(10 years) is assumed. Since this sensitivity is comparable to predicted GW signal levels, a reliable detection will require substantial signal-to-noise ratio improvement via pulsar timing array
The mean pulse profile of PSR J0737-3039A
No full textGeneral relativity predicts that the spin axes of the pulsars in the double-pulsar system PSR J0737-3039A/B will precess rapidly, in general leading to a change in the observed pulse profiles. We have observed this system over a 1 yr interval using the Parkes 64 m radio telescope at three frequencies: 680, 1390, and 3030 MHz. These data, combined with the short survey observation made 2 years earlier, show no evidence for significant changes in the pulse profile of PSR J0737-3039A, the 22 ms pulsar. The limit on variations of the profile 10% width is about 0.degrees50 yr(-1). These results imply an angle delta between the pulsar spin axis and the orbit normal of less than or similar to60degrees, consistent with recent evolutionary studies of the system. Although a wide range of system parameters remain consistent with the data, the model recently proposed by F. A. Jenet & S. M. Ransom can be ruled out. A nonzero ellipticity for the radiation beam gives slightly but not significantly improved fits to the data, so that a circular beam describes the data equally well within the uncertainties
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