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 The binary progenitors of short and long GRBs and their gravitational-wave emission

2018 ◽  
Vol 168 ◽  
pp. 01006
Author(s):  
J. A. Rueda ◽  
R. Ruffini ◽  
J. F. Rodriguez ◽  
M. Muccino ◽  
Y. Aimuratov ◽  
...  
Keyword(s):  
Neutron Star ◽  
Gravitational Wave ◽  
Gamma Ray ◽  
Critical Mass ◽  
Compact Object ◽  
Annual Number ◽  
Black Hole Binaries ◽  
Nuclear Equation Of State ◽  
Long Duration ◽  
Wave Emission

We have sub-classified short and long-duration gamma-ray bursts (GRBs) into seven families according to the binary nature of their progenitors. Short GRBs are produced in mergers of neutron-star binaries (NS-NS) or neutron star-black hole binaries (NS-BH). Long GRBs are produced via the induced gravitational collapse (IGC) scenario occurring in a tight binary system composed of a carbon-oxygen core (COcore) and a NS companion. The COcore explodes as type Ic supernova (SN) leading to a hypercritical accretion process onto the NS: if the accretion is sufficiently high the NS reaches the critical mass and collapses forming a BH, otherwise a massive NS is formed. Therefore long GRBs can lead either to NS-BH or to NS-NS binaries depending on the entity of the accretion. We discuss for the above compact-object binaries: 1) the role of the NS structure and the nuclear equation of state; 2) the occurrence rates obtained from X and gamma-rays observations; 3) the predicted annual number of detections by the Advanced LIGO interferometer of their gravitational-wave emission.

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 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 Analysis of broad-lined Type Ic supernovae from the (intermediate) Palomar Transient Factory

2019 ◽  
Vol 621 ◽  
pp. A71 ◽  
Author(s):  
F. Taddia ◽  
J. Sollerman ◽  
C. Fremling ◽  
C. Barbarino ◽  
E. Karamehmetoglu ◽  
...  
Keyword(s):  
Binary Systems ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Light Curves ◽  
Close Binary ◽  
Host Galaxy ◽  
Scaling Relations ◽  
Homogeneous Sample ◽  
Long Duration ◽  
Absolute Magnitudes

We study 34 Type Ic supernovae that have broad spectral features (SNe Ic-BL). This is the only SN type found in association with long-duration gamma-ray bursts (GRBs). We obtained our photometric data with the Palomar Transient Factory (PTF) and its continuation, the intermediate PTF (iPTF). This is the first large, homogeneous sample of SNe Ic-BL from an untargeted survey. Furthermore, given the high observational cadence of iPTF, most of these SNe Ic-BL were discovered soon after explosion. We present K-corrected Bgriz light curves of these SNe, obtained through photometry on template-subtracted images. We analyzed the shape of the r-band light curves, finding a correlation between the decline parameter Δm15 and the rise parameter Δm−10. We studied the SN colors and, based on g − r, we estimated the host-galaxy extinction for each event. Peak r-band absolute magnitudes have an average of −18.6 ± 0.5 mag. We fit each r-band light curve with that of SN 1998bw (scaled and stretched) to derive the explosion epochs. We computed the bolometric light curves using bolometric corrections, r-band data, and g − r colors. Expansion velocities from Fe II were obtained by fitting spectral templates of SNe Ic. Bolometric light curves and velocities at peak were fitted using the semianalytic Arnett model to estimate ejecta mass Mej, explosion energy EK and 56Ni mass M(56Ni) for each SN. We find average values of Mej = 4 ± 3 M⊙, EK = (7 ± 6)×1051 erg, and M(56Ni)=0.31  ±  0.16 M⊙. The parameter distributions were compared to those presented in the literature and are overall in agreement with them. We also estimated the degree of 56Ni mixing using scaling relations derived from hydrodynamical models and we find that all the SNe are strongly mixed. The derived explosion parameters imply that at least 21% of the progenitors of SNe Ic-BL are compatible with massive (> 28 M⊙), possibly single stars, whereas at least 64% might come from less massive stars in close binary systems.

scholarly journals Neutron star binaries and long-duration gamma-ray bursts

2006 ◽  
Vol 372 (3) ◽  
pp. 1351-1356 ◽  
Author(s):  
A. J. Levan ◽  
M. B. Davies ◽  
A. R. King
Keyword(s):  
Neutron Star ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Long Duration

scholarly journals The role of magnetic field geometry in the evolution of neutron star merger accretion discs

2019 ◽  
Vol 490 (4) ◽  
pp. 4811-4825 ◽  
Author(s):  
I M Christie ◽  
A Lalakos ◽  
A Tchekhovskoy ◽  
R Fernández ◽  
F Foucart ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Neutron Star ◽  
Large Scale ◽  
Gamma Ray ◽  
Long Duration ◽  
Field Geometry ◽  
General Relativistic ◽  
R Process ◽  
Magnetohydrodynamic Simulations

ABSTRACT Neutron star mergers are unique laboratories of accretion, ejection, and r-process nucleosynthesis. We used 3D general relativistic magnetohydrodynamic simulations to study the role of the post-merger magnetic geometry in the evolution of merger remnant discs around stationary Kerr black holes. Our simulations fully capture mass accretion, ejection, and jet production, owing to their exceptionally long duration exceeding 4 s. Poloidal post-merger magnetic field configurations produce jets with energies Ejet ∼ (4–30) × 1050 erg, isotropic equivalent energies Eiso ∼ (4–20) × 1052 erg, opening angles θjet ∼ 6–13°, and durations tj ≲ 1 s. Accompanying the production of jets is the ejection of $f_\mathrm{ej}\sim 30\!-\!40{{\ \rm per\ cent}}$ of the post-merger disc mass, continuing out to times &gt;1 s. We discover that a more natural, purely toroidal post-merger magnetic field geometry generates large-scale poloidal magnetic flux of alternating polarity and striped jets. The first stripe, of $E_\mathrm{jet}\simeq 2\times 10^{48}\, \mathrm{erg}$, Eiso ∼ 1051 erg, θjet ∼ 3.5–5°, and tj ∼ 0.1 s, is followed by ≳4 s of striped jet activity with $f_\mathrm{ej}\simeq 27{{\ \rm per\ cent}}$. The dissipation of such stripes could power the short-duration gamma-ray burst (sGRB) prompt emission. Our simulated jet energies and durations span the range of sGRBs. We find that although the blue kilonova component is initially hidden from view by the red component, it expands faster, outruns the red component, and becomes visible to off-axis observers. In comparison to GW 170817/GRB 170817A, our simulations underpredict the mass of the blue relative to red component by a factor of few. Including the dynamical ejecta and neutrino absorption may reduce this tension.

scholarly journals Evolution of Progenitor Stars of Type Ibc Supernovae and Long Gamma-Ray Bursts

2007 ◽  
Vol 3 (S250) ◽  
pp. 231-236
Author(s):  
Sung-Chul Yoon ◽  
Norbert Langer ◽  
Matteo Cantiello ◽  
Stan E. Woosley ◽  
Gary A. Glatzmaier
Keyword(s):  
Binary Stars ◽  
Binary Systems ◽  
Massive Star ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Evolutionary Models ◽  
Single Star ◽  
Solar Metallicity ◽  
Progenitor Stars

AbstractWe discuss how rotation and binary interactions may be related to the diversity of type Ibc supernovae and long gamma-ray bursts. After presenting recent evolutionary models of massive single and binary stars including rotation, the Tayler-Spruit dynamo and binary interactions, we argue that the nature of SNe Ibc progenitors from binary systems may not significantly differ from that of single star progenitors in terms of rotation, and that most long GRB progenitors may be produced via the quasi-chemically homogeneous evolution at sub-solar metallicity. We also briefly discuss the possible role of magnetic fields generated in the convective core of a massive star for the transport of angular momentum, which is potentially important for future stellar evolution models of supernova and GRB progenitors.

Gamma-ray burst models

2007 ◽  
Vol 365 (1854) ◽  
pp. 1277-1280 ◽  
Author(s):  
Andrew King
Keyword(s):  
Black Hole ◽  
Star Formation ◽  
Neutron Star ◽  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Close Binaries ◽  
Host Galaxy ◽  
Star Forming ◽  
Star Forming Regions ◽  
Long Duration

I consider various possibilities for making gamma-ray bursts, particularly from close binaries. In addition to the much-studied neutron star+neutron star and black hole+neutron star cases usually considered good candidates for short-duration bursts, there are also other possibilities. In particular, neutron star+massive white dwarf has several desirable features. These systems are likely to produce long-duration gamma-ray bursts (GRBs), in some cases definitely without an accompanying supernova, as observed recently. This class of burst would have a strong correlation with star formation and occur close to the host galaxy. However, rare members of the class need not be near star-forming regions and could have any type of host galaxy. Thus, a long-duration burst far from any star-forming region would also be a signature of this class. Estimates based on the existence of a known progenitor suggest that this type of GRB may be quite common, in agreement with the fact that the absence of a supernova can only be established in nearby bursts.

scholarly journals One Dimensional Hydrodynamics of Asteroid-Neutron Star Collisions

1980 ◽  
Vol 58 ◽  
pp. 591-594
Author(s):  
Michael J. Newman ◽  
Arthur N. Cox
Keyword(s):  
Neutron Star ◽  
Solid Body ◽  
Gamma Ray ◽  
Compact Object ◽  
Gamma Ray Bursts ◽  
Radiation Diffusion ◽  
Gamma Ray Burst ◽  
One Dimensional

It has been suggested by several authors (e.g., Harwit and Salpeter, 1973) that the observed cosmic gamma-ray bursts might be produced by the collision of comet or asteroid-sized bodies with a compact object. Colgate and Petschek (1980) have discussed the tidal breakup of a solid body approaching a neutron star in central impact, with particular application to the cosmic gamma-ray burst of March 5, 1979. In this work we present the results of simplified one-dimensional hydrodynamic-radiation diffusion calculations of such an occurence.

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