scholarly journals Self-Consistency of Relativistic Observables with General Relativity in the White Dwarf-Neutron Star Binary PSR J1141-6545

2003 ◽  
Vol 595 (1) ◽  
pp. L49-L52 ◽  
Author(s):  
M. Bailes ◽  
S. M. Ord ◽  
H. S. Knight ◽  
A. W. Hotan
Keyword(s):  
General Relativity ◽  
Neutron Star ◽  
White Dwarf ◽  
Star Binary ◽  
Self Consistency

scholarly journals Binary pulsars and tests of general relativity

2009 ◽  
Vol 5 (S261) ◽  
pp. 218-227 ◽  
Author(s):  
I. H. Stairs
Keyword(s):  
General Relativity ◽  
Neutron Star ◽  
White Dwarf ◽  
Strong Field ◽  
Binding Energies ◽  
Tests Of General Relativity ◽  
Binary Pulsars ◽  
The Difference

AbstractBinary pulsars are a valuable laboratory for gravitational experiments. Double-neutron-star systems such as the double pulsar provide the most stringent tests of strong-field gravity available to date, while pulsars with white-dwarf companions constrain departures from general relativity based on the difference in gravitational binding energies in the two stars. Future observations may open up entirely new tests of the predictions of general relativity.

scholarly journals The Green Bank Northern Sky Survey: Discovery of a New Neutron Star-Neutron Star Binary

1996 ◽  
Vol 160 ◽  
pp. 11-12
Author(s):  
David J. Nice ◽  
Ronald W. Sayer ◽  
Joseph H. Taylor
Keyword(s):  
Fourier Transform ◽  
Neutron Star ◽  
White Dwarf ◽  
Rotation Period ◽  
Fourier Transform Spectrometer ◽  
Millisecond Pulsars ◽  
Flux Limit ◽  
Sky Survey ◽  
Star Binary

We have surveyed 15,900 deg2of the northern sky for millisecond pulsars at 370 MHz with the Green Bank 140ft telescope. The telescope was driven along lines of constant declination such that a given point on the sky was observed for two minutes. A Fourier transform spectrometer synthesized 512-channel spectra across 40 MHz in each of two polarizations. Total intensity levels were boxcar averaged at intervals of 256μs, quantized to 1 bit, and written to tape. Data were processed with the Cray C90 of the Pittsburgh Supercomputer Center. The flux limit of the survey was 8 mJy for slow pulsars. A further 1500 deg2were observed with 20 MHz bandwidth, yielding 71% the usual sensitivity.Eighty-four slow pulsars were detected, of which six were previously unknown. Three recycled pulsars were detected: the relativistic binary B1534+12; the neutron star-white dwarf binary J1022+1001, discovered nearly simultaneously at Arecibo; and J1518+4904, a previously unknown pulsar with a 41 ms rotation period.

scholarly journals Recent Observations of PSR B1534+12

2001 ◽  
Vol 205 ◽  
pp. 408-409
Author(s):  
I.H. Stairs ◽  
S.E. Thorsett ◽  
J.H. Taylor ◽  
Z. Arzoumanian
Keyword(s):  
General Relativity ◽  
Neutron Star ◽  
Spin Axis ◽  
Pulse Profile ◽  
High Quality ◽  
Orbital Parameters ◽  
General Relativistic ◽  
Star Binary

We present the results of recent Arecibo observations of the relativistic double-neutron-star binary PSR B1534+12. The timing solution includes measurements of five post-Keplerian orbital parameters, whose values agree well with the predictions of general relativity. The observations show that the pulse profile is evolving secularly at both 1400 MHz and 430 MHz. This effect is similar to that seen in PSR B1913+16, and is almost certainly due to general relativistic precession of the pulsar's spin axis. We also present high-quality polarimetric profiles at both observing frequencies.

scholarly journals Merger of white dwarf-neutron star binaries: Prelude to hydrodynamic simulations in general relativity

2009 ◽  
Vol 80 (2) ◽  
Author(s):  
Vasileios Paschalidis ◽  
Morgan MacLeod ◽  
Thomas W. Baumgarte ◽  
Stuart L. Shapiro
Keyword(s):  
General Relativity ◽  
Neutron Star ◽  
White Dwarf ◽  
Hydrodynamic Simulations

The Development of a Black Hole—The Oppenheimer-Snyder Dust Cloud

1972 ◽  
Vol 2 (2) ◽  
pp. 110-111
Author(s):  
P. Szekeres
Keyword(s):  
General Relativity ◽  
Black Hole ◽  
Neutron Star ◽  
Gravitational Collapse ◽  
White Dwarf ◽  
Physical Mechanism ◽  
Critical Radius ◽  
Dust Cloud ◽  
Schwarzschild Solution

When a star of mass ≳ 2M⊙ collapses there does not appear to exist any physical mechanism to prevent total gravitational collapse, unless in some miraculous way the star always manages to blow off enough mass for it to settle down into a stable neutron star or white dwarf configuration. General relativity is needed in order to handle the ultimate situation, and the theory predicts a critical radius ρ = 2m (in units such that G = c = 1) at which the coordinates in the Schwarzschild solutionbecome invalid.

scholarly journals Interpretation of Binary Pulsar Observations

1981 ◽  
Vol 95 ◽  
pp. 371-378 ◽  
Author(s):  
R. D. Blandford ◽  
W. M. DeCampli
Keyword(s):  
General Relativity ◽  
Neutron Star ◽  
White Dwarf ◽  
Radio Pulsar ◽  
Binary Pulsar ◽  
Orbital Decay

The nature, dynamics and evolution of the three known radio pulsar binaries are discussed. The system containing 1913+16 appears to comprise two ~1.4 M⊙ components, and to undergo orbital decay as predicted by general relativity. It is proposed that 1913+16 has a neutron star companion and that 0655+64 and 0820+02 have white dwarf companions which should be observable optically.

scholarly journals 3D magnetized jet break-out from neutron-star binary merger ejecta: afterglow emission from the jet and the ejecta

2021 ◽  
Vol 502 (2) ◽  
pp. 1843-1855
Author(s):  
Antonios Nathanail ◽  
Ramandeep Gill ◽  
Oliver Porth ◽  
Christian M Fromm ◽  
Luciano Rezzolla
Keyword(s):  
Neutron Star ◽  
Thermal Emission ◽  
Opening Angle ◽  
Hollow Core ◽  
Binary Neutron Star ◽  
Vlbi Observations ◽  
Superluminal Motion ◽  
General Relativistic ◽  
Star Binary ◽  
Magnetohydrodynamic Simulations

ABSTRACT We perform 3D general-relativistic magnetohydrodynamic simulations to model the jet break-out from the ejecta expected to be produced in a binary neutron-star merger. The structure of the relativistic outflow from the 3D simulation confirms our previous results from 2D simulations, namely, that a relativistic magnetized outflow breaking out from the merger ejecta exhibits a hollow core of θcore ≈ 4°, an opening angle of θjet ≳ 10°, and is accompanied by a wind of ejected matter that will contribute to the kilonova emission. We also compute the non-thermal afterglow emission of the relativistic outflow and fit it to the panchromatic afterglow from GRB170817A, together with the superluminal motion reported from VLBI observations. In this way, we deduce an observer angle of $\theta _{\rm obs}= 35.7^{\circ \, \, +1.8}_{\phantom{\circ \, \, }-2.2}$. We further compute the afterglow emission from the ejected matter and constrain the parameter space for a scenario in which the matter responsible for the thermal kilonova emission will also lead to a non-thermal emission yet to be observed.

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