Smooth Optical Self-similar Emission of Gamma-Ray Bursts

Липунов, В. М.; Simakov, S. G.; Gorbovskoy, E.; Vlasenko, D.

doi:10.3847/1538-4357/aa7e77

Cited by 20 publications

(11 citation statements)

References 48 publications

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“…MASTER global robotic net (Lipunov et al 2010(Lipunov et al , 2019a(Lipunov et al , 2022Kornilov et al 2012 ) of Lomonosov Moscow State University was developed to investigate high-energy astrophysics events, in particular, to disco v er optical counterpart of gamma-ray bursts, gra vitational wa v e ev ents, high-energy neutrino, FRB and other events (Aartsen et al 2017 ;Abbott et al 2016 ;Buckley et al 2018 ;Lipunov et al 2016aLipunov et al , b , 2018aLipunov et al , b , c , 2019aLipunov et al , b , 2020Lipunov et al , 2022. In addition to the targeted transient search, MASTER detects new optical transients during routine sky survey, in particular orphan afterglow and GRB afterglows at the earliest stage (Gorbovsk o y et al 2016 ;Lipunov et al 2016bLipunov et al , 2017aLipunov et al , b , c , d , 2018bLipunov et al , c , 2021Lipunov et al , 2022Troja et al 2017 ;Sadovnichy et al 2018 ;Laskar et al 2019 ;Zimnukhov et al 2019 ;Ershova et al 2020 ;Jordana-Mitjans et al 2020 ). MASTER consists of nine fully robotic ground-based telescopes distributed all o v er the Earth with identical scientific equipment, which provides capability to continuously observe targets in a single photometric system.…”

Section: Master Photometrymentioning

confidence: 99%

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Orphan optical flare as SOSS emission afterglow, localization in time

Липунов

Корнилов

Zhirkov

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We report on MASTER optical observations of an afterglow-like optical and X-ray transient AT2021lfa/ZTF21aayokph. We detected the initial steady brightening of the transient at 7σ confidence level. This allowed us to use smooth optical self-similar emission of GRBs model to constrain the explosion time to better than 14 min as well as to estimate its initial Lorentz factor Γ0 = 20 ± 10. Taking into consideration the low Γ0 and non-detection in gamma-rays, we classify this transient as the first failed GRB afterglow.

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Section: Master Photometrymentioning

confidence: 99%

“…To approximate the light curve of AT2021lfa, we used the smooth optical self-similar emission model (SOSS) for GRB afterglows (Lipunov et al 2017a ). The SOSS light curve is described by the following relation:…”

Section: Light-cur V E Fittingmentioning

confidence: 99%

Orphan optical flare as SOSS emission afterglow, localization in time

Липунов

Корнилов

Zhirkov

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…MASTER Global Robotic Net was developed to study the key tasks of modern extreme energy astrophysics: to discover optical counterparts of gamma-ray bursts and to discover polarization of GRB prompt optical emission [24][25][26][27][28][29] ; to independently localize the sources of gravitational wave, detected by LIGO/Virgo 12,13 , to investigate high energy neutrino sources 30 , fast radio bursts sources [31][32][33][34] and other extreme processes in Universe. MASTER conducted optical observations that reveal strong evidence for high energy neutrino progenitor 30 .…”

Section: Monitoringmentioning

confidence: 99%

First Prompt Optical Observations of Nearest Fast Radio Burst new New Astromomical Method

Липунов

Корнилов

Gorbovskoy

et al. 2020

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With the discovery of gamma ray bursts1,2, it became clear that our Universe flickers with superfast catastrophic events, sometimes lasting for a thousandths of a second. These ultra-fast transients - the peculiar one-day butterflies of the Universe - shine so brightly that they are noticed even on the other end of the Universe and, moreover, by very small telescopes. But in the radio range, the sky remained silent until the beginning of the 21st century. Only in 2007, radio astronomers analyzing archival observations of the Parkes Radio Telescope first encountered fast transients 3,4 . About a hundred such sources have already been discovered. We report the first optical observation of the closest radio burster FRB 180916.J0158+655-8 synchronously with a radio burst. In total, we obtained about 155,093 images at MASTER Global Robotic Net9*. In the course of our observations, we found a new method for detecting objects deep below the noise level. In addition, using the new method, we found the excess of photons in the FRB direction at a level of 23 m associated with the emission of the host galaxy.

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“…It is widely accepted that the optical peak followed by the normal decay phase is described by the standard synchrotron emission from forward shock (FS) or reverse shock (RS), or a superposition of both components evolving in a uniform-density medium (Sari, Piran, & Narayan 1998;Kobayashi and Zhang 2003;Fraĳa et al 2016;Becerra et al 2019c,b). The monotonic rise and decay in the GRB 191016A light curve, has been previously observed in the afterglow of a small sample of GRBs by Lipunov et al (2017) and is usually attributed to a single forward shock wave. However, the universal scaling function proposed to describe GRBs afterglow behaviour based on this assumption requires a rising temporal index 𝛼 = 2, whereas the statistical results presented by Liang et al (2010) show that the rising index is mostly between 1 and 2 for the majority of GRBs where the onset of the optical afterglow is clearly detected.…”

Section: The Bright Peak Followed By the Normal Decaymentioning

confidence: 56%

GRB 191016A: The onset of the forward shock and evidence of late energy injection

Pereyra,

Fraija,

Watson

et al. 2021

Preprint

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We present optical and near-infrared photometric observations of GRB 191016 with the COATLI, DDOTI and RATIR groundbased telescopes over the first three nights. We present the temporal evolution of the optical afterglow and describe 5 different stages that were not completely characterized in previous works, mainly due to scarcity of data points to accurately fit the different components of the optical emission. After the end of the prompt gamma-ray emission, we observed the afterglow rise slowly in the optical and near-infrared (NIR) wavelengths and peak at around 𝑇 + 1450 s in all filters. This was followed by an early decay, a clear plateau from 𝑇 + 5000 s to 𝑇 + 11000 s, and then a regular late decay. We also present evidence of the jet break at later times, with a temporal index in good agreement with the temporal slope obtained from X-ray observations. Although many of the features observed in the optical light curves of GRBs are usually well explained by a reverse shock (RS) or forward shock (FS), the shallowness of the optical rise and enhanced peak emission in the GRB191016A afterglow is not well-fitted by only a FS or a RS. We propose a theoretical model which considers both of these components and combines an evolving FS with a later embedded RS and a subsequent late energy injection from the central engine activity. We use this model to successfully explain the temporal evolution of the light curves and discuss its implications on the fireball properties.

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Smooth Optical Self-similar Emission of Gamma-Ray Bursts

Cited by 20 publications

References 48 publications

Orphan optical flare as SOSS emission afterglow, localization in time

Orphan optical flare as SOSS emission afterglow, localization in time

First Prompt Optical Observations of Nearest Fast Radio Burst new New Astromomical Method

GRB 191016A: The onset of the forward shock and evidence of late energy injection

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