Luminous supernovae associated with ultra-long gamma-ray bursts from hydrogen-free progenitors extended by pulsational pair-instability

We show that the luminous supernovae associated with ultra-long gamma-ray bursts can be related to the slow cooling from the explosions of hydrogen-free progenitors that are extended by pulsational pair-instability. We have recently shown that some rapidly-rotating hydrogen-free gamma-ray burst progenitors that experience pulsational pair-instability can keep an extended structure caused by pulsational pair-instability until the core collapse. These types of progenitors have large radii exceeding 10 R⊙ and they sometimes reach beyond 1000 R⊙ at the time of the core collapse. They are, therefore, promising progenitors of ultra-long gamma-ray bursts. Here, we perform light-curve modeling of the explosions of one extended hydrogen-free progenitor with a radius of 1962 R⊙. The progenitor mass is 50 M⊙ and 5 M⊙ exists in the extended envelope. We use the one-dimensional radiation hydrodynamics code STELLA in which the explosions are initiated artificially by setting given explosion energy and 56Ni mass. Thanks to the large progenitor radius, the ejecta experience slow cooling after the shock breakout and they become rapidly evolving (≲10 days), luminous (≳1043 erg s−1) supernovae in the optical even without energy input from the 56Ni nuclear decay when the explosion energy is more than 1052 erg. The 56Ni decay energy input can affect the light curves after the optical light-curve peak and make the light-curve decay slowly when the 56Ni mass is around 1 M⊙. They also have a fast photospheric velocity above 10 000 km s−1 and a hot photospheric temperature above 10 000 K at around the peak luminosity. We find that the rapid rise and luminous peak found in the optical light curve of SN 2011kl, which is associated with the ultra-long gamma-ray burst GRB 111209A, can be explained as the cooling phase of the extended progenitor. The subsequent slow light-curve decline can be related to the 56Ni decay energy input. The ultra-long gamma-ray burst progenitors we proposed recently can explain both the ultra-long gamma-ray burst duration and the accompanying supernova properties. When the gamma-ray burst jet is off-axis or choked, the luminous supernovae could be observed as fast blue optical transients without accompanying gamma-ray bursts.

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GAMMA-RAY BURST JETS: COMPOSITION AND CONFIGURATION

International Journal of Modern Physics A ◽

10.1142/s0217751x05025991 ◽

2005 ◽

Vol 20 (14) ◽

pp. 3151-3153

Author(s):

BING ZHANG

Keyword(s):

Gamma Ray ◽

Massive Stars ◽

Gamma Ray Bursts ◽

Geometric Configuration ◽

Relativistic Jets ◽

Gamma Ray Burst ◽

The Core ◽

Physical Composition ◽

Core Questions ◽

Near Future

Long Gamma-ray bursts (GRBs) are believed to be originated from relativistic jets launched during the core collapses of some massive stars. The two core questions in the contemporary GRB science are the physical composition and the geometric configuration of the jets. Here I review the recent theoretical progress in both directions, and discuss how Swift may address both questions in the near future.

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Gamma-ray burst optical light-curve zoo: comparison with X-ray observations

Astronomy and Astrophysics ◽

10.1051/0004-6361/201321221 ◽

2013 ◽

Vol 557 ◽

pp. A12 ◽

Cited By ~ 26

Author(s):

E. Zaninoni ◽

M. G. Bernardini ◽

R. Margutti ◽

S. Oates ◽

G. Chincarini

Keyword(s):

Light Curve ◽

Gamma Ray ◽

Gamma Ray Burst ◽

X Ray ◽

Optical Light Curve

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PTF11rka: an interacting supernova at the crossroads of stripped-envelope and H-poor superluminous stellar core collapses

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/staa2191 ◽

2020 ◽

Vol 497 (3) ◽

pp. 3542-3556

Author(s):

E Pian ◽

P A Mazzali ◽

T J Moriya ◽

A Rubin ◽

A Gal-Yam ◽

...

Keyword(s):

Kinetic Energy ◽

Light Curve ◽

Lower Energy ◽

Rest Frame ◽

Main Sequence ◽

Gamma Ray ◽

Core Collapse ◽

Curve Shape ◽

Maximum Brightness ◽

The Core

ABSTRACT The hydrogen-poor supernova (SN) PTF11rka (z = 0.0744), reported by the Palomar Transient Factory, was observed with various telescopes starting a few days after the estimated explosion time of 2011 December 5 UT and up to 432 rest-frame days thereafter. The rising part of the light curve was monitored only in the RPTF filter band, and maximum in this band was reached ∼30 rest-frame days after the estimated explosion time. The light curve and spectra of PTF11rka are consistent with the core-collapse explosion of a ∼10 M⊙ carbon–oxygen core evolved from a progenitor of main-sequence mass 25–40 M⊙, that liberated a kinetic energy Ek≈4 × 1051 erg, expelled ∼8 M⊙ of ejecta, and synthesized ∼0.5 M⊙ of 56Ni. The photospheric spectra of PTF11rka are characterized by narrow absorption lines that point to suppression of the highest ejecta velocities (≳ 15 000 km s−1). This would be expected if the ejecta impacted a dense, clumpy circumstellar medium. This in turn caused them to lose a fraction of their energy (∼5 × 1050 erg), less than 2 per cent of which was converted into radiation that sustained the light curve before maximum brightness. This is reminiscent of the superluminous SN 2007bi, the light-curve shape and spectra of which are very similar to those of PTF11rka, although the latter is a factor of 10 less luminous and evolves faster in time. PTF11rka is in fact more similar to gamma-ray burst SNe in luminosity, although it has a lower energy and a lower Ek/Mej ratio.

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The core collapse supernovae, gamma-ray bursts and SN 1987A

SN 1987A, Quark Phase Transition in Compact Objects and Multimessenger Astronomy. Proceedings of The International Conference. ◽

10.26119/sao.2020.1.52359 ◽

2018 ◽

Author(s):

Vladimir V. Sokolov ◽

Alberto J. Castro-Tirado ◽

Tatyana N. Sokolova

Keyword(s):

Gamma Ray ◽

Gamma Ray Bursts ◽

Core Collapse ◽

The Core ◽

Sn 1987A

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Plerion model of the X-ray plateau in short gamma-ray bursts

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1648 ◽

2019 ◽

Vol 487 (4) ◽

pp. 5010-5018 ◽

Cited By ~ 3

Author(s):

L C Strang ◽

A Melatos

Keyword(s):

Light Curve ◽

Supernova Remnants ◽

Gamma Ray ◽

Electron Energy Spectrum ◽

Gamma Ray Bursts ◽

Time Dependent ◽

Core Collapse ◽

X Ray ◽

Surface Magnetic Field ◽

Core Collapse Supernova

Abstract Many short gamma-ray bursts (sGRBs) exhibit a prolonged plateau in the X-ray light curve following the main burst. It is shown that an X-ray plateau at the observed luminosity emerges naturally from a plerion-like model of the sGRB remnant, in which the magnetized, relativistic wind of a millisecond magnetar injects shock-accelerated electrons into a cavity confined by the sGRB blast wave. A geometry-dependent fraction of the plerionic radiation is also intercepted and reprocessed by the optically thick merger ejecta. The relative contributions of the plerion and ejecta to the composite X-ray light curve are estimated approximately with the aid of established ejecta models. The plerionic component of the electron energy spectrum is evolved under the action of time-dependent, power-law injection and adiabatic and synchrotron cooling in order to calculate the X-ray light curve analytically. The model yields an anticorrelation between the luminosity and duration of the plateau as well as a sudden cut-off in the X-ray flux, if the decelerating magnetar collapses to form a black hole. Both features are broadly consistent with the data and can be related to the surface magnetic field of the magnetar and its angular velocity at birth. The analogy with core-collapse supernova remnants is discussed briefly.

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Population III Gamma-Ray Burst

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312013099 ◽

2011 ◽

Vol 7 (S279) ◽

pp. 301-304 ◽

Cited By ~ 1

Author(s):

Kunihito Ioka ◽

Yudai Suwa ◽

Hiroki Nagakura ◽

Rafael S. de Souza ◽

Naoki Yoshida

Keyword(s):

Mass Loss ◽

First Generation ◽

Gamma Ray ◽

Gamma Ray Bursts ◽

Gamma Ray Burst ◽

X Ray ◽

The Core ◽

Long Duration ◽

The Future ◽

Bright Phase

AbstractGamma-ray bursts (GRBs) are unique probes of the first generation (Pop III) stars. We show that a relativistic gamma-ray burst (GRB) jet can potentially pierce the envelope of a very massive Pop III star even if the Pop III star has a supergiant hydrogen envelope without mass loss, thanks to the long-lived powerful accretion of the envelope itself. While the Pop III GRB is estimated to be energetic (Eγ,iso ~ 1055 erg), the supergiant envelope hides the initial bright phase in the cocoon component, leading to a GRB with a long duration ~1000 (1 + z) s and an ordinary isotropic luminosity ~ 1052 erg s−1 (~ 10−9 erg cm−2 s−1 at redshift z ~ 20), although these quantities are found to be sensitive to the core and envelope mass. We also show that Pop III.2 GRBs (which are primordial but affected by radiation from other stars) occur >100 times more frequently than Pop III.1 GRBs, and thus should be suitable targets for future X-ray and radio missions. The radio transient surveys are already constraining the Pop III GRB rate and promising in the future.

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PHYSICS OF SUPERNOVAE

International Journal of Modern Physics A ◽

10.1142/s0217751x05029630 ◽

2005 ◽

Vol 20 (29) ◽

pp. 6597-6611 ◽

Cited By ~ 16

Author(s):

D. K. NADYOZHIN ◽

V. S. IMSHENNIK

Keyword(s):

Shock Wave ◽

Gamma Ray ◽

Gamma Ray Bursts ◽

Core Collapse ◽

Temporal Behavior ◽

The Core ◽

Global Properties ◽

Thermonuclear Burning ◽

Different Types ◽

Type Ia

The origin of cosmic rays (CR) is supposed to be closely connected with supernovae (SNe) which create the conditions favorable for various mechanisms of the CR acceleration to operate effectively. First, modern ideas about the physics of the SN explosion are briefly discussed: the explosive thermonuclear burning in degenerate white dwarfs resulting in Type Ia SNe and the gravitational collapse of stellar cores giving rise to other types of SNe (Ib, Ic, IIL, IIP). Next, we survey some global properties of the SNe of different types: the total explosion energy distribution of various components (kinetic energy of the hydrodynamic flow, electromagnetic radiation, temporal behavior of the neutrino emission and individual energies of different neutrino flavors). Then, we discuss in the possibility of direct hydrodynamic acceleration by the shock wave breakout and the properties of the SN shocks in the circumstellar medium. Then the properties of the neutrino radiation from the core-collapse SNe and a possibility to incorporate both the LSD Mont Blanc neutrino event and that recorded by the K II and IMB detectors into a single scenario are described in detail. Finally, the issues of the neutrino nucleosynthesis and of the connection between supernova and gamma-ray bursts are discussed.

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Inhomogeneities in the light curves of gamma-ray bursts afterglow

International Journal of Modern Physics D ◽

10.1142/s0218271818440121 ◽

2018 ◽

Vol 27 (10) ◽

pp. 1844012

Author(s):

Elena Mazaeva ◽

Alexei Pozanenko ◽

Pavel Minaev

Keyword(s):

Light Curve ◽

Power Law ◽

Gamma Ray ◽

Gamma Ray Bursts ◽

Light Curves ◽

Peak Time ◽

Gamma Ray Burst ◽

X Ray

We discuss the inhomogeneous behavior of gamma-ray burst afterglow light curves in optic. We use well-sampled light curves based on mostly our own observations to find and identify deviations (inhomogeneities) from broken power law. By the inhomogeneous behavior we mean flashes, bumps, slow deviations from power law (wiggles) in a light curve. In particular we report parameters of broken power law, describe phenomenology, compare optical light curves with X-ray ones and classify the inhomogeneities. We show that the duration of the inhomogeneities correlates with their peak time relative to gamma-ray burst (GRB) trigger and the correlation is the same for all types of inhomogeneities.

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