Multicolour modelling of SN 2013dx associated with GRB 130702A★

Volnova, A.; Pruzhinskaya, M.; Pozanenko, A.; Блинников, С. И.; Minaev, P. Yu.; Бурхонов, О.; Chernenko, A.; Ehgamberdiev, S. A.; Inasaridze, R.; Jelínek, M.; Хорунжев, Г. А.; Klunko, E.; Krugly, Yu. N.; Mazaeva, E.; Rumyantsev, V.; Volvach, A. E.

doi:10.1093/mnras/stw3297

Cited by 34 publications

(13 citation statements)

References 69 publications

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“…The different properties of these transient events may be related to different parameters of the underlying magnetars (Metzger et al 2015;Yu et al 2017). Kovacevic et al 2014;(10)Ferrero et al 2006;(11)Campana et al 2006;(12)Mirabal et al 2006;(13) Xu et al2008;(14)Li 2008;(15) Soderberg et al 2008;(16)Jin et al 2013;(17)Olivares E et al 2015;(18)Berger et al 2011;(19)Vergani et al 2011;(20) Bufano et al 2012;(21)Fan et al 2011;(22) Larsson et al 2015;(23) Greiner et al 2015;(24) Kann et al 2016;(25) Kann et al 2017;(26) Zhang et al 2012;(27) Melandri et al 2012;(28) Schulze et al 2014;(29) (30) Xu et al2013;(31) Vestrand et al 2014;(32) Ackermann et al 2014;(33) Maselli et al 2014;(34)Singer et al 2013;(35)D'Elia et al 2015;(36) Volnova et al 2017;(37) Cano et al 2015;(38)…”

Section: Conclusion and Discussionunclassified

Gamma-Ray Burst/Supernova Associations: Energy Partition and the Case of a Magnetar Central Engine

Lü

Lin

Zhang

et al. 2018

ApJ

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The favored progenitor model for Gamma-ray Bursts (GRBs) with Supernova (SN) association is the core collapse of massive stars. One possible outcome of such a collapse is a rapidly spinning, strongly magnetized neutron star ("magnetar"). We systematically analyze the multi-wavelength data of GRB/SN associations detected by several instruments before 2017 June. Twenty GRB/SN systems have been confirmed via direct spectroscopic evidence or a clear light curve bump, as well as some spectroscopic evidence resembling a GRB-SN. We derive/collect the basic physical parameters of the GRBs and SNe, and look for correlations among these parameters. We find that the peak brightness, 56 Ni mass, and explosion energy of SNe associated with GRBs are statistically higher than other Type Ib/c SNe. A statistically significant relation between the peak energy of GRBs and the peak brightness of their associated SNe is confirmed. No significant correlations are found between the GRB energies (either isotropic or beaming-corrected) and the supernova energy. We investigate the energy partition within these systems and find that the beaming-corrected GRB energy of most systems is smaller than the SN energy, with less than 30% of the total energy distributed in the relativistic jet. The total energy of the systems is typically smaller than the maximum available energy of a millisecond magnetar (2 × 10 52 erg), especially if aspherical SN explosions are considered. The data are consistent with-though not proof of-the hypothesis that most, but not all, GRB/SN systems are powered by millisecond magnetars.

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Section: Conclusion and Discussionunclassified

Gamma-Ray Burst/Supernova Associations: Energy Partition and the Case of a Magnetar Central Engine

Lü

Lin

Zhang

et al. 2018

ApJ

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“…At very early times, there are the extremely bright flashes of GRBs 080319B (Racusin et al 2008;Bloom et al 2009) and 130427A (Vestrand et al 2014), but also very faint light curves, like those of XRF 050416A (Kann et al 2010) and GRB 120714B as presented in this paper. Afterglows of SN-associated GRBs can also be very bright at late times, such as the exceptional case of GRB 030329 (e.g., Lipkin et al 2004;Kann et al 2006), and the similarly nearby GRB 130702A (Singer et al 2013(Singer et al , 2015Toy et al 2016;Volnova et al 2017). This is not unexpected, as there are strong biases involved.…”

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confidence: 99%

Four GRB supernovae at redshifts between 0.4 and 0.8

Klose

Schmidl

Канн

et al. 2019

A&A

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Twenty years ago, GRB 980425/SN 1998bw revealed that long Gamma-Ray Bursts (GRBs) are physically associated with broad-lined type Ic supernovae. Since then more than 1000 long GRBs have been localized to high angular precision, but only in ∼ 50 cases the underlying supernova (SN) component was identified. Using the multi-channel imager GROND (Gamma-Ray Burst Optical Near-Infrared Detector) at ESO/La Silla, during the last ten years we have devoted a substantial amount of observing time to reveal and to study SN components in long-GRB afterglows.Here we report on four more GRB-SNe (associated with GRBs 071112C, 111228A, 120714B, and 130831A) which were discovered and/or followed-up with GROND and whose redshifts lie between z = 0.4 and 0.8. We study their afterglow light curves, follow the associated SN bumps over several weeks, and characterize their host galaxies. Using SN 1998bw as a template, the derived SN explosion parameters are fully consistent with the corresponding properties of the so-far known GRB-SN ensemble, with no evidence for an evolution of their properties as a function of redshift. In two cases (GRB 120714B/SN 2012eb at z = 0.398 and GRB 130831A/SN 2013fu at z = 0.479) additional Very Large Telescope (VLT) spectroscopy of the associated SNe revealed a photospheric expansion velocity at maximum light of about 40 000 and 20 000 km s −1 , respectively. For GRB 120714B, which was an intermediate-luminosity burst, we find additional evidence for a blackbody component in the light of the optical transient at early times, similar to what has been detected in some GRB-SNe at lower redshifts.

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“…We modeled numerically the multicolor light curves using the one-dimensional radiation hydrodynamical code STELLA, previously widely implemented for the modeling of typical non-GRB SNe. Figure 4 shows the combined multicolor light curve of the event, the physical parameters obtained and the modeling process are described in (Volnova et al 2018(Volnova et al , 2017.…”

Section: Resultsmentioning

confidence: 99%

“…Nearby long GRBs exhibit in the light curve the feature of the supernova (SN) of Type Ic which confirms the core-collapse nature of these events (Hjorth & Bloom 2012). The observations of SNe allows estimating main physical properties of the progenitor and the ejection (e.g., Volnova et al 2017). Short GRBs show the kilonova (Li & Paczyński 1998, Metzger et al 2010, Tanvir et al 2013) feature originating from the merging compact system of binary neutron stars (e.g., Abbott et al 2017, Abbott et al 2020).…”

Section: Introductionmentioning

confidence: 99%

IKI GRB-FuN: observations of GRBs with small-aperture telescopes

Volnova

Pozanenko

Mazaeva

et al. 2021

An. Acad. Bras. Ciênc.

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Gamma-ray bursts (GRBs) are the most energetic and mysterious events in the Universe, which are observed in all ranges of electromagnetic spectrum. Most valuable results about physics of GRB are obtained by optical observations. GRBs are initially detected in gamma-rays with poor localization accuracy, and an optical counterpart should be found. The faster the counterpart is found, the more it can give to physics. This first phase, as a rule, corresponds to an early afterglow. The next phases of the observations are multicolor photometry, polarimetry, spectroscopy, and few days later the search for a supernova or kilonova associated with the GRB, and finally, observations of the host galaxy. To manage the problem of fast optical observations, telescopes with a small aperture are suitable. They can have a large field of view, which is necessary to cover initial localizations of GRBs. The sensitivity of the telescope+detector may be sufficient to record statistically significant light curve with fine time resolution. We describe one of the networks of telescopes with a small aperture IKI-GRB FuN, and present the results of early optical observation of GRB sources, and discuss the design requirements of the optical observations for effective GRB research in the next decade.

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Multicolour modelling of SN 2013dx associated with GRB 130702A★

Cited by 34 publications

References 69 publications

Gamma-Ray Burst/Supernova Associations: Energy Partition and the Case of a Magnetar Central Engine

Gamma-Ray Burst/Supernova Associations: Energy Partition and the Case of a Magnetar Central Engine

Four GRB supernovae at redshifts between 0.4 and 0.8

IKI GRB-FuN: observations of GRBs with small-aperture telescopes

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