scholarly journals Gravitational waves from remnant massive neutron stars of binary neutron star merger: Viscous hydrodynamics effects

2017 ◽  
Vol 95 (12) ◽  
Author(s):  
Masaru Shibata ◽  
Kenta Kiuchi
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Gravitational Waves ◽  
Binary Neutron Star ◽  
Viscous Hydrodynamics

Pan Galactic Gargle Blaster

2019 ◽  
pp. 132-137
Author(s):  
Nicholas Mee
Keyword(s):  
General Relativity ◽  
Neutron Star ◽  
Neutron Stars ◽  
Gravitational Waves ◽  
Gamma Ray ◽  
Great Accuracy ◽  
Gamma Ray Bursts ◽  
Tests Of General Relativity ◽  
Binary Neutron Star

The sources of short gamma ray bursts (GRBs) have been identified with neutron star merger events. Hulse and Taylor discovered the first binary neutron star in 1974. By monitoring the pulsar in this system the orbital characteristics of the system have been determined with great accuracy. This has led to tests of general relativity, including the first confirmation of the existence of gravitational waves. The emission of this radiation is gradually bringing the two neutron stars together. They will collide and merge in about 300 million years.

scholarly journals Gravitational waves from binary neutron stars

2022 ◽  
Author(s):  
Luca Baiotti
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Gravitational Wave ◽  
Gravitational Waves ◽  
Compact Stars ◽  
Binary Neutron Star ◽  
Gravitational Wave Detectors ◽  
Global Status ◽  
General Relativistic

AbstractI review the current global status of research on gravitational waves emitted from mergers of binary neutron star systems, focusing on general-relativistic simulations and their use to interpret data from the gravitational-wave detectors, especially in relation to the equation of state of compact stars.

scholarly journals Remnant massive neutron stars of binary neutron star mergers: Evolution process and gravitational waveform

2013 ◽  
Vol 88 (4) ◽  
Author(s):  
Kenta Hotokezaka ◽  
Kenta Kiuchi ◽  
Koutarou Kyutoku ◽  
Takayuki Muranushi ◽  
Yu-ichiro Sekiguchi ◽  
...  
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Evolution Process ◽  
Binary Neutron Star

scholarly journals Spectral analysis of gravitational waves from binary neutron star merger remnants

2017 ◽  
Vol 96 (6) ◽  
Author(s):  
Francesco Maione ◽  
Roberto De Pietri ◽  
Alessandra Feo ◽  
Frank Löffler
Keyword(s):  
Spectral Analysis ◽  
Neutron Star ◽  
Gravitational Waves ◽  
Binary Neutron Star

LIGO/Virgo Listens to Neutron Stars

2020 ◽  
pp. 137-145
Author(s):  
John W. Moffat
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Gravitational Waves ◽  
Gamma Ray ◽  
Accurate Determination ◽  
Hubble Constant ◽  
Gravitational Theory ◽  
Optical Signal ◽  
Gravity Models ◽  
Expansion Of The Universe

On August 8, 2017, LIGO/Virgo detected the merging of two neutron stars 130 million light years away. Just 1.7 seconds later, the Fermi Gamma Ray Space Telescope received an optical signal—a short gamma ray burst (GRB). Thus began a new era of “multimessenger astronomy.” The GRBs are very energetic explosions observed in galaxies. The neutron star merger offers the first evidence that heavy metals such as gold, platinum, and uranium were created by the collision of neutron stars in a “kilonova.” The resulting gravitational waves offer a new way of measuring the Hubble constant, which determines the rate of expansion of the universe. An important result from the neutron star merger is an extremely accurate determination of the speed of gravitational waves; they move at the speed of light. This has significant ramifications for gravitational theory. It falsifies many proposed modified gravity models.

scholarly journals Gravitational waves, neutrino emissions and effects of hyperons in binary neutron star mergers

2012 ◽  
Vol 29 (12) ◽  
pp. 124003 ◽  
Author(s):  
Kenta Kiuchi ◽  
Yuichiro Sekiguchi ◽  
Koutarou Kyutoku ◽  
Masaru Shibata
Keyword(s):  
Neutron Star ◽  
Gravitational Waves ◽  
Binary Neutron Star

scholarly journals Binary Neutron Star (BNS) Merger: What We Learned from Relativistic Ejecta of GW/GRB 170817A

Physics ◽  
2019 ◽  
Vol 1 (2) ◽  
pp. 194-228 ◽  
Author(s):  
Houri Ziaeepour
Keyword(s):  
Neutron Star ◽  
Gravitational Waves ◽  
Gamma Ray ◽  
Lorentz Factor ◽  
Prompt Gamma ◽  
External Shocks ◽  
Binary Neutron Star ◽  
Tidal Forces ◽  
Relativistic Jet ◽  
Short Grbs

Gravitational Waves (GW) from coalescence of a Binary Neutron Star (BNS) and its accompanying short Gamma-Ray Burst (GRB) GW/GRB 170817A confirmed the presumed origin of these puzzling transients and opened up the way for relating properties of short GRBs to those of their progenitor stars and their surroundings. Here we review an extensive analysis of the prompt gamma-ray and late afterglows of this event. We show that a fraction of polar ejecta from the merger had been accelerated to ultra-relativistic speeds. This structured jet had an initial Lorentz factor of about 260 in our direction, which was O ( 10 ∘ ) from the jet’s axis, and was a few orders of magnitude less dense than in typical short GRBs. At the time of arrival to circum-burst material the ultra-relativistic jet had a close to Gaussian profile and a Lorentz factor ≳ 130 in its core. It had retained in some extent its internal collimation and coherence, but had extended laterally to create mildly relativistic lobes—a cocoon. Its external shocks on the far from center inhomogeneous circum-burst material and low density of colliding shells generated slowly rising afterglows, which peaked more than 100 days after the prompt gamma-ray. The circum-burst material was somehow correlated with the merger. As non-relativistic outflows or tidally ejected material during BNS merger could not have been arrived to the location of the external shocks before the relativistic jet, circum-burst material might have contained recently ejected materials from resumption of internal activities, faulting and mass loss due to deformation and breaking of stars crusts by tidal forces during latest stages of their inspiral but well before their merger. By comparing these findings with the results of relativistic Magneto-Hydro-Dynamics (MHD) simulations and observed gravitational waves we conclude that progenitor neutron stars were most probably old, had close masses and highly reduced magnetic fields.

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