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 The binary systems associated with short and long gamma-ray bursts and their detectability

2017 ◽  
Vol 26 (09) ◽  
pp. 1730016 ◽  
Author(s):  
Jorge A. Rueda ◽  
Y. Aimuratov ◽  
U. Barres de Almeida ◽  
L. Becerra ◽  
C. L. Bianco ◽  
...  
Keyword(s):  
Neutron Star ◽  
Gravitational Collapse ◽  
Binary Systems ◽  
Gamma Ray ◽  
Critical Mass ◽  
Compact Object ◽  
Gamma Ray Bursts ◽  
Black Hole Binaries ◽  
Long Duration

Short and long-duration gamma-ray bursts (GRBs) have been recently sub-classified into seven families according to the binary nature of their progenitors. For short GRBs, mergers of neutron star binaries (NS–NS) or neutron star-black hole binaries (NS-BH) are proposed. For long GRBs, the induced gravitational collapse (IGC) paradigm proposes a tight binary system composed of a carbon–oxygen core (CO[Formula: see text]) and a NS companion. The explosion of the CO[Formula: see text] as supernova (SN) triggers a hypercritical accretion process onto the NS companion which might reach the critical mass for the gravitational collapse to a BH. Thus, this process can lead either to a NS-BH or to NS–NS depending on whether or not the accretion is sufficient to induce the collapse of the NS into a BH. We shall discuss for the above compact object binaries: (1) the role of the NS structure and the equation-of-state on their final fate; (2) their occurrence rates as inferred from the X and gamma-ray observations; (3) the expected number of detections of their gravitational wave (GW) emission by the Advanced LIGO interferometer.

scholarly journals On the Induced Gravitational Collapse

2018 ◽  
Vol 168 ◽  
pp. 02005
Author(s):  
Laura M. Becerra ◽  
Carlo Bianco ◽  
Chris Fryer ◽  
Jorge Rueda ◽  
Remo Ruffini
Keyword(s):  
Black Hole ◽  
Neutron Star ◽  
Gravitational Collapse ◽  
Binary Systems ◽  
Gamma Ray ◽  
Critical Mass ◽  
Supernova Explosion ◽  
Isotropic Energy ◽  
X Ray ◽  
Binary Separations

The induced gravitational collapse (IGC) paradigm has been applied to explain the long gamma ray burst (GRB) associated with type Ic supernova, and recently the Xray flashes (XRFs). The progenitor is a binary systems of a carbon-oxygen core (CO) and a neutron star (NS). The CO core collapses and undergoes a supernova explosion which triggers the hypercritical accretion onto the NS companion (up to 10-2 M⊙s-1). For the binary driven hypernova (BdHNe), the binary system is enough bound, the NS reach its critical mass, and collapse to a black hole (BH) with a GRB emission characterized by an isotropic energy Eiso > 1052 erg. Otherwise, for binary systems with larger binary separations, the hypercritical accretion onto the NS is not sufficient to induced its gravitational collapse, a X-ray flash is produced with Eiso < 1052 erg. We’re going to focus in identify the binary parameters that limits the BdHNe systems with the XRFs systems.

scholarly journals BLACK HOLES, SUPERNOVAE AND GAMMA RAY BURSTS

2013 ◽  
Vol 22 (11) ◽  
pp. 1360009 ◽  
Author(s):  
REMO RUFFINI
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Neutron Star ◽  
Binary System ◽  
Recent Progress ◽  
Gamma Ray ◽  
Critical Mass ◽  
Gamma Ray Bursts ◽  
The Relationship ◽  
Short Grbs

We review recent progress in our understanding of the nature of Gamma Ray Bursts (GRBs) and in particular, of the relationship between short GRBs and long GRBs. The first example of a short GRB is described. The coincidental occurrence of a GRB with a supernova (SN) is explained within the induced gravitational collapse (IGC) paradigm, following the sequence: (1) an initial binary system consists of a compact carbon–oxygen (CO) core star and a neutron star (NS); (2) the CO core explodes as a SN, and part of the SN ejecta accretes onto the NS which reaches its critical mass and collapses to a black hole (BH) giving rise to a GRB; (3) a new NS is generated by the SN as a remnant. The observational consequences of this scenario are outlined.

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.

PULSAR SEARCHING AND TIMING

2013 ◽  
Vol 22 (01) ◽  
pp. 1341007 ◽  
Author(s):  
R. N. MANCHESTER
Keyword(s):  
Neutron Star ◽  
Binary Systems ◽  
Gamma Ray ◽  
Direct Detection ◽  
Theory Of Relativity ◽  
Pulsar Timing ◽  
Combining Data ◽  
Period Derivative ◽  
Star Binary ◽  
Pulsar Timing Array

More than 2000 pulsars are now known. These pulsars may be divided into a number of different classes according to their period, period derivative, binary properties, emission characteristics and so on. Some important classes have relatively few members, e.g. double-neutron-star binary systems, and so continued searches for currently unknown pulsars are important. Such searches are being undertaken at various observatories around the world. Somewhat unexpectedly, the Fermi Gamma-ray Observatory, has proved to be an efficient pulsar detector, especially for millisecond pulsars (MSPs). The great stability of pulsar periods, especially for MSPs, leads to a number of important applications of pulsar timing. The detection and study of relativistic orbit perturbations in double-neutron-star systems has proved to be a powerful tool with measurements of the original binary pulsar, PSR B1913+16, and more recently the double pulsar, PSR J0737-3039A/B, showing that Einstein's general theory of relativity accurately describes these gravitational interactions. Direct detection of gravitational waves using pulsar timing is close to being achieved with the development of pulsar timing arrays (PTAs) in Europe, North America and Australia. Combining data from these PTAs to form the International Pulsar Timing Array (IPTA) will lead to improved significance of such a detection. Ultimately, detailed study of gravitational-wave sources will be possible using future large radio telescopes such as FAST and the SKA.

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 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.

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