A possible relation between flare activity in super-luminous supernovae and gamma-ray bursts

Yu, Yun-Wei; Li, Shao-Ze

doi:10.1093/mnras/stx1028

Cited by 16 publications

(5 citation statements)

References 66 publications

(84 reference statements)

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“…The meanings of the three terms on the right side of the equation are explained as follows. Firstly, the bolometric luminosity L th of the ejecta thermal emission can be estimated by (Kasen & Bildsten 2010;Yu & Li 2017)…”

Section: The Emission Of a Ts And A Hot Ejectamentioning

confidence: 99%

X-Ray Transients from the Accretion-induced Collapse of White Dwarfs

Chen

2019

ApJL

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The accretion-induced collapse (AIC) of a white dwarf in a binary with a nondegenerate companion can sometimes lead to the formation of a rapidly rotating and highly magnetized neutron star (NS). The spin-down of this NS can drive a powerful pulsar wind (PW) and bring out some detectable multi-wavelength emissions. On the one hand, the PW can evaporate the companion in a few days to form a torus surrounding the NS. Then, due to the blockage of the PW by the torus, a reverse shock can be formed in the wind to generate intense hard X-rays. This emission component disappears in a few weeks' time, after the torus is broken down at its inner boundary and scoured into a very thin disk. On the other hand, the interaction between the PW with an AIC ejecta can lead to a termination shock of the wind, which can produce a long-lasting soft X-ray emission component. In any case, the high-energy emissions from deep inside the system can be detected only after the AIC ejecta becomes transparent for X-rays. Meanwhile, by absorbing the X-rays, the AIC ejecta can be heated effectively and generate a fast-evolving and luminous ultraviolet (UV)/optical transient. Therefore, the predicted hard and soft X-ray emissions, associated by an UV/optical transient, provide a clear observational signature for identifying AIC events in current and future observations (e.g., AT 2018cow).

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Section: The Emission Of a Ts And A Hot Ejectamentioning

confidence: 99%

X-Ray Transients from the Accretion-induced Collapse of White Dwarfs

Chen

2019

ApJL

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“…The increased opacity due to the increased ionization would then cause a delay in the escape of radiation, resulting in a change in the lightcurve decline rate. Finally, the magnetar engine may exhibit flare activity, resulting in intermittent energy injection (Yu & Li 2017).…”

Section: Lightcurve Undulationsmentioning

confidence: 99%

The Type I Superluminous Supernova PS16aqv: Lightcurve Complexity and Deep Limits on Radioactive Ejecta in a Fast Event

Blanchard

Nicholl

Berger

et al. 2018

ApJ

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We present UV/optical photometric and spectroscopic observations of PS16aqv (SN 2016ard), a Type I superluminous supernova (SLSN-I) classified as part of our search for low-z SLSNe. PS16aqv is most similar in timescale and spectroscopic evolution to fast evolving SLSNe-I and reached a peak absolute magnitude of M r ≈ −22.1. The lightcurves exhibit a significant undulation at 30 rest-frame days after peak, with a behavior similar to undulations seen in the slowly fading SLSN-I SN 2015bn. This similarity strengthens the case that fast and slow SLSNe-I form a continuum with a common origin. At ≈ 80 days after peak, the lightcurves exhibit a transition to a slow decline, followed by significant subsequent steepening, indicative of a plateau phase or a second significant undulation. Deep limits at ≈ 280 days after peak imply a tight constraint on the nickel mass, M Ni 0.35 M (lower than for previous SLSNe-I), and indicate that some SLSNe-I do not produce significantly more nickel than normal Type Ic SNe. Using MOSFiT, we model the lightcurve with a magnetar central engine model and find P spin ≈ 0.9 ms, B ≈ 1.5 × 10 14 G, and M ej ≈ 16 M . The implied rapid spin-down time and large reservoir of available energy coupled with the high ejecta mass may account for the fast evolving lightcurve and slow spectroscopic evolution. We also study the location of PS16aqv within its host galaxy and find that it occurred at an offset of 2.46 ± 0.21 kpc from the central, most active star-forming region. We find the host galaxy exhibits low metallicity and spatially varying extinction and star formation rate, with the explosion site of PS16aqv exhibiting lower values than the central region. The complexity seen in the lightcurves of PS16aqv and other events highlights the importance of obtaining well-sampled lightcurves for exploring deviations from a uniform decline.

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“…Recent studies are increasingly favoring the central engine model (e.g., Nicholl et al 2017;Margalit et al 2017) as it has been shown to satisfactorily reproduce the optical light-curves of SLSNe-I with a wide range of properties (e.g., Inserra et al 2013;Chatzopoulos et al 2013;Nicholl et al 2014;Metzger et al 2015;Inserra et al 2017;Nicholl et al 2017b). Magnetar central engines with initial spin periods in the range 1-5 ms and magnetic fields in the range ≈ 10 13 − 10 14 G are the best fit for the optical bolometric emission of several systems (e.g., Dessart et al 2012;Inserra et al 2013;Nicholl et al 2013;Metzger et al 2015;Lunnan et al 2016;Yu & Li 2017).…”

Section: Introductionmentioning

confidence: 98%

Jets in Hydrogen-poor Superluminous Supernovae: Constraints from a Comprehensive Analysis of Radio Observations

Coppejans

Margutti

Guidorzi

et al. 2018

ApJ

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The energy source powering the extreme optical luminosity of hydrogen-stripped Superluminous Supernovae (SLSNe-I) is not known, but recent studies have highlighted the case for a central engine. Radio and/or X-ray observations are best placed to track the fastest ejecta and probe the presence of outflows from a central engine. We compile all the published radio observations of SLSNe-I to date and present three new observations of two new SLSNe-I. None were detected. Through modeling the radio emission, we constrain the sub-parsec environments and possible outflows in SLSNe-I. In this sample we rule out on-axis collimated relativistic jets of the kind detected in Gamma-Ray Bursts (GRBs). We constrain off-axis jets with opening angles of 5 • (30 • ) to energies of E k < 4 × 10 50 erg (E k < 10 50 erg) in environments shaped by progenitors with mass-loss rates oḟ M < 10 −4 M yr −1 (Ṁ < 10 −5 M yr −1 ) for all off-axis angles, assuming fiducial values e = 0.1 and B = 0.01. The deepest limits rule out emission of the kind seen in faint un-collimated GRBs (with the exception of GRB 060218), and from relativistic supernovae. Finally, for the closest SLSN-I SN 2017egm we constrained the energy of an uncollimated non-relativistic outflow like those observed in normal SNe to E k 10 48 erg. Subject headings: supernovae: specific (PS1-10bzj,

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A possible relation between flare activity in super-luminous supernovae and gamma-ray bursts

Cited by 16 publications

References 66 publications

X-Ray Transients from the Accretion-induced Collapse of White Dwarfs

X-Ray Transients from the Accretion-induced Collapse of White Dwarfs

The Type I Superluminous Supernova PS16aqv: Lightcurve Complexity and Deep Limits on Radioactive Ejecta in a Fast Event

Jets in Hydrogen-poor Superluminous Supernovae: Constraints from a Comprehensive Analysis of Radio Observations

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