Detectability of the gravitational wave signal from a close neutron star binary with mass transfer

1992 ◽  
Vol 394 ◽  
pp. 586 ◽  
Author(s):  
Piotr Jaranowski ◽  
Andrzej Krolak
Keyword(s):  
Mass Transfer ◽  
Neutron Star ◽  
Gravitational Wave ◽  
Wave Signal ◽  
Star Binary

Opening the window

2019 ◽  
pp. 1-22
Author(s):  
Nils Andersson
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Gravitational Wave ◽  
Binary Event ◽  
Star Binary

This chapter provides a brief survey of gravitational-wave astronomy, including the recent recent breakthrough detection. It sets the stage for the rest of the book via simple back-of-the-envelope estimates for different sets of sources. The chapter also describes the first detection of a black hole merger (GW150914) as well as the first observed neutron star binary event (GW170817) and introduces some of the ideas required to understand these breakthroughs.

Black Hole-Neutron Star Binary Merger Calculations: GRB Progenitors and the Stability of Mass Transfer

2006 ◽  
Author(s):  
Joshua A. Faber ◽  
Thomas W. Baumgarte ◽  
Stuart L. Shapiro ◽  
Keisuke Taniguchi ◽  
Frederic A. Rasio
Keyword(s):  
Mass Transfer ◽  
Black Hole ◽  
Neutron Star ◽  
Star Binary ◽  
The Stability

scholarly journals Masses of double neutron star mergers

2020 ◽  
Vol 639 ◽  
pp. A123 ◽  
Author(s):  
Matthias U. Kruckow
Keyword(s):  
Neutron Star ◽  
Gravitational Wave ◽  
Milky Way ◽  
Radio Pulsar ◽  
Population Synthesis ◽  
Radio Pulsars ◽  
Wave Observation ◽  
Binary Evolution ◽  
Star Binary

Aims. I aim to explain the mass discrepancy between the observed double neutron-star binary population by radio pulsar observations and gravitational-wave observation. Methods. I performed binary population synthesis calculations and compared their results with the radio and the gravitational-wave observations simultaneously. Results. Simulations of binary evolution were used to link different observations of double neutron star binaries with each other. I investigated the progenitor of GW190425 in more detail. A distribution of masses and merger times of the possible progenitors is presented. Conclusions. A mass discrepancy between the radio pulsars in the Milky Way with another neutron star companion and the inferred masses from gravitational-wave observations of those kind of merging systems is naturally found in binary evolution.

scholarly journals m=1instability and gravitational wave signal in binary neutron star mergers

2016 ◽  
Vol 94 (4) ◽  
Author(s):  
Luis Lehner ◽  
Steven L. Liebling ◽  
Carlos Palenzuela ◽  
Patrick M. Motl
Keyword(s):  
Neutron Star ◽  
Gravitational Wave ◽  
Wave Signal ◽  
Binary Neutron Star

scholarly journals On gravitational-wave echoes from neutron-star binary coalescences

2018 ◽  
Vol 35 (15) ◽  
pp. 15LT01 ◽  
Author(s):  
Paolo Pani ◽  
Valeria Ferrari
Keyword(s):  
Neutron Star ◽  
Gravitational Wave ◽  
Star Binary

scholarly journals Search of S3 LIGO data for gravitational wave signals from spinning black hole and neutron star binary inspirals

2008 ◽  
Vol 78 (4) ◽  
Author(s):  
B. Abbott ◽  
R. Abbott ◽  
R. Adhikari ◽  
J. Agresti ◽  
P. Ajith ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Gravitational Wave ◽  
Star Binary

scholarly journals Reverse shocks in the relativistic outflows of gravitational wave-detected neutron star binary mergers

2019 ◽  
Vol 489 (2) ◽  
pp. 1820-1827 ◽  
Author(s):  
Gavin P Lamb ◽  
Shiho Kobayashi
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Gravitational Wave ◽  
Strong Magnetic Field ◽  
Gamma Ray ◽  
Reverse Shock ◽  
Central Engine ◽  
Forward Shock ◽  
Binary Mergers ◽  
Star Binary

ABSTRACT The afterglows to gamma-ray bursts (GRBs) are due to synchrotron emission from shocks generated as an ultrarelativistic outflow decelerates. A forward and a reverse shock will form, however, where emission from the forward shock is well studied as a potential counterpart to gravitational wave-detected neutron star mergers the reverse shock has been neglected. Here, we show how the reverse shock contributes to the afterglow from an off-axis and structured outflow. The off-axis reverse shock will appear as a brightening feature in the rising afterglow at radio frequencies. For bursts at ∼100 Mpc, the system should be inclined ≲20° for the reverse shock to be observable at ∼0.1–10 d post-merger. For structured outflows, enhancement of the reverse shock emission by a strong magnetic field within the outflow is required for the emission to dominate the afterglow at early times. Early radio photometry of the afterglow could reveal the presence of a strong magnetic field associated with the central engine.

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