scholarly journals Constraints on long-lived remnants of neutron star binary mergers from late-time radio observations of short duration gamma-ray bursts

2013 ◽  
Vol 437 (2) ◽  
pp. 1821-1827 ◽  
Author(s):  
Brian D. Metzger ◽  
Geoffrey C. Bower
Keyword(s):  
Neutron Star ◽  
Short Duration ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Late Time ◽  
Radio Observations ◽  
Binary Mergers ◽  
Star Binary

Anatomy of a merger

2019 ◽  
pp. 541-580
Author(s):  
Nils Andersson
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Binary System ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Late Time ◽  
Tidal Effects ◽  
Gamma Ray Burst ◽  
Love Numbers ◽  
Star Binary

This chapter discusses the different stages of an inspiralling neutron star binary system, through the formation of a black hole and the possible emergence of a gamma-ray burst. Tidal effects and the information encoded in the so-called Love numbers are explored. The violent dynamics of the merger is considered and models of gamma-ray bursts and the late time kilonova emission are also explored.

Induced gravitational collapse in FeCO Core–Neutron star binaries and Neutron star–Neutron star binary mergers

2015 ◽  
Vol 30 (28n29) ◽  
pp. 1545023
Author(s):  
R. Ruffini ◽  
Y. Aimuratov ◽  
C. L. Bianco ◽  
M. Enderli ◽  
M. Kovacevic ◽  
...  
Keyword(s):  
Neutron Star ◽  
Gravitational Collapse ◽  
Binary Systems ◽  
Recent Progress ◽  
Gamma Ray ◽  
Critical Mass ◽  
Gamma Ray Bursts ◽  
New Paradigm ◽  
Binary Mergers ◽  
Star Binary

We review the recent progress in understanding the nature of gamma-ray bursts (GRBs). The occurrence of GRB is explained by the Induced Gravitational Collapse (IGC) in FeCO Core–Neutron star binaries and Neutron star–Neutron star binary mergers, both processes occur within binary system progenitors. Making use of this most unexpected new paradigm, with the fundamental implications by the neutron star (NS) critical mass, we find that different initial configurations of binary systems lead to different GRB families with specific new physical predictions confirmed by observations.

scholarly journals A Late-time Radio Survey of Short Gamma-ray Bursts at z < 0.5: New Constraints on the Remnants of Neutron-star Mergers

2020 ◽  
Vol 902 (1) ◽  
pp. 82
Author(s):  
Genevieve Schroeder ◽  
Ben Margalit ◽  
Wen-fai Fong ◽  
Brian D. Metzger ◽  
Peter K. G. Williams ◽  
...  
Keyword(s):  
Neutron Star ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Late Time ◽  
Radio Survey

scholarly journals Searching for the radio remnants of short-duration gamma-ray bursts

2020 ◽  
Vol 500 (2) ◽  
pp. 1708-1720
Author(s):  
R Ricci ◽  
E Troja ◽  
G Bruni ◽  
T Matsumoto ◽  
L Piro ◽  
...  
Keyword(s):  
Short Duration ◽  
Gamma Ray ◽  
Thermal Emission ◽  
Surrounding Medium ◽  
Mass Range ◽  
Gamma Ray Bursts ◽  
Late Time ◽  
Central Engine ◽  
Two Samples ◽  
Rule Out

ABSTRACT Neutron star mergers produce a substantial amount of fast-moving ejecta, expanding outwardly for years after the merger. The interaction of these ejecta with the surrounding medium may produce a weak isotropic radio remnant, detectable in relatively nearby events. We use late-time radio observations of short duration gamma-ray bursts (sGRBs) to constrain this model. Two samples of events were studied: four sGRBs that are possibly in the local (&lt;200 Mpc) Universe were selected to constrain the remnant non-thermal emission from the sub-relativistic ejecta, whereas 17 sGRBs at cosmological distances were used to constrain the presence of a proto-magnetar central engine, possibly re-energizing the merger ejecta. We consider the case of GRB 170817A/GW170817 and find that in this case the early radio emission may be quenched by the jet blast-wave. In all cases, for ejecta mass range of ${M}_{\rm {ej}}\lesssim 10^{-2}\, (5\times 10^{-2})\, \mathrm{M}_\odot$, we can rule out very energetic merger ejecta ${E}_{\rm {ej}}\gtrsim 5\times 10^{52}\, (10^{53})\, \rm erg$, thus excluding the presence of a powerful magnetar as a merger remnant.

scholarly journals On the Central Engine of Short Gamma-ray Bursts

2005 ◽  
Vol 192 ◽  
pp. 503-508
Author(s):  
Stephan Rosswog ◽  
Enrico Ramírez-Ruiz
Keyword(s):  
Neutron Star ◽  
Kinetic Energy ◽  
Gamma Ray ◽  
Rotation Axis ◽  
Gamma Ray Bursts ◽  
Relativistic Jets ◽  
Dynamo Action ◽  
Neutron Star Mass ◽  
Central Engine ◽  
Star Binary

SummaryWe assess the ability of neutron star binary coalescence to produce short gamma-ray bursts (GRBs). We find that the neutrino annihilation above the merged remnant will drive bipolar, relativistic jets along the initial binary rotation axis. This outflow can be collimated by the energetic, neutrino-driven baryonic wind that is blown off the remnant. Despite the narrow neutron star mass distribution the apparent luminosities will be spread over a broad range from ~ 1049 to ~ 1052erg s−1, typical jet opening half-angles are around 5 degrees. If the central core of the merger remnant does not collapse immediately convective dynamo action will set in and the available kinetic energy can be transformed into magnetic fields in excess of 1017 G. The corresponding spin-down time scale is ~ 0.2 s, just about the duration of a short GRB.

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.

scholarly journals The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. VIII. A Comparison to Cosmological Short-duration Gamma-Ray Bursts

2017 ◽  
Vol 848 (2) ◽  
pp. L23 ◽  
Author(s):  
W. Fong ◽  
E. Berger ◽  
P. K. Blanchard ◽  
R. Margutti ◽  
P. S. Cowperthwaite ◽  
...  
Keyword(s):  
Neutron Star ◽  
Short Duration ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Binary Neutron Star

scholarly journals Long-Term Evolution of (Short) Gamma-Ray Burst Central Engines

2004 ◽  
Vol 194 ◽  
pp. 132-133
Author(s):  
William H. Lee
Keyword(s):  
Black Holes ◽  
Neutron Star ◽  
Accretion Disks ◽  
Gamma Ray ◽  
Dynamical Evolution ◽  
Gamma Ray Bursts ◽  
Term Evolution ◽  
Star Binary ◽  
Short Grbs

AbstractCosmological gamma ray bursts (GRBs) possibly originate from accretion disks around stellar mass black holes. These could be formed after the merger of a double neutron star or black hole-neutron star binary. The dynamical evolution of the disk is important if one wishes to relate characteristic timescales with the observed duration and variability. We show here the results of such a set of calculations, relevant for short GRBs.

Late‐Time Radio Observations of 68 Type Ibc Supernovae: Strong Constraints on Off‐Axis Gamma‐Ray Bursts

2006 ◽  
Vol 638 (2) ◽  
pp. 930-937 ◽  
Author(s):  
A. M. Soderberg ◽  
E. Nakar ◽  
E. Berger ◽  
S. R. Kulkarni
Keyword(s):  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Late Time ◽  
Radio Observations
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