Jet or shock breakout? The low-luminosity GRB 060218

Irwin, Christopher M.; Chevalier, Roger A.

doi:10.1093/mnras/stw1058

Cited by 54 publications

(67 citation statements)

References 95 publications

(316 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…SN 2006aj, a SN Ic-BL associated with an X-ray flash (e.g., Sollerman et al 2006), also showed a double peak. The early maximum was interpreted as being due to the presence of an extended envelope formed by a dense wind (Campana et al 2006;Waxman et al 2007;Irwin & Chevalier 2016). Similar to SN 2006aj, the GRB-SN 2010bh also exhibited an early peak (Cano et al 2011).…”

Section: Introductionmentioning

confidence: 97%

iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor

Taddia

Fremling

Sollerman

et al. 2016

A&A

View full text Add to dashboard Cite

Context. Type Ic supernovae (SNe Ic) arise from the core-collapse of H-(and He-) poor stars, which could either be single Wolf-Rayet (WR) stars or lower-mass stars stripped of their envelope by a companion. Their light curves are radioactively powered and usually show a fast rise to peak (∼10−15 d), without any early (in the first few days) emission bumps (with the exception of broad-lined SNe Ic) as sometimes seen for other types of stripped-envelope SNe (e.g., Type IIb SN 1993J and Type Ib SN 2008D). Aims. We have studied iPTF15dtg, a spectroscopically normal SN Ic with an early excess in the optical light curves followed by a long (∼30 d) rise to the main peak. It is the first spectroscopically-normal double-peaked SN Ic to be observed. Our aim is to determine the properties of this explosion and of its progenitor star. Methods. Optical photometry and spectroscopy of iPTF15dtg was obtained with multiple telescopes. The resulting light curves and spectral sequence are analyzed and modeled with hydrodynamical and analytical models, with particular focus on the early emission. Results. iPTF15dtg is a slow rising SN Ic, similar to SN 2011bm. Hydrodynamical modeling of the bolometric properties reveals a large ejecta mass (∼10 M ) and strong 56 Ni mixing. The luminous early emission can be reproduced if we account for the presence of an extended ( 500 R ), low-mass ( 0.045 M ) envelope around the progenitor star. Alternative scenarios for the early peak, such as the interaction with a companion, a shock-breakout (SBO) cooling tail from the progenitor surface, or a magnetar-driven SBO are not favored. Conclusions. The large ejecta mass and the presence of H-and He-free extended material around the star suggest that the progenitor of iPTF15dtg was a massive ( 35 M ) WR star that experienced strong mass loss.

show abstract

Section: Introductionmentioning

confidence: 97%

iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor

Taddia

Fremling

Sollerman

et al. 2016

A&A

View full text Add to dashboard Cite

show abstract

“…These dots are denoted in black filled circles. Squares and stars denote the data collected by Irwin & Chevalier (2016) and Levan et al (2014), respectively. The arrows denote the GRBs with the lower limit of jet luminosity (due to the lack of detection of a jet break).…”

Section: Modelmentioning

confidence: 99%

Black Hole Hyperaccretion Inflow–Outflow Model. I. Long and Ultra-long Gamma-Ray Bursts

Liu

Song

Zhang

et al. 2017

ApJ

View full text Add to dashboard Cite

Long-duration gamma-ray bursts (LGRBs) and ultra-LGRBs (ULGRBs) originate from collapsars, in the center of which a newborn rotating stellar-mass black hole (BH) surrounded by a massive accretion disk may form. In the scenario of BH hyperaccretion inflow-outflow model and BlandfordZnajek (BZ) mechanism to trigger gamma-ray bursts (GRBs), the real accretion rate to power a BZ jet is far lower than the mass supply rate from the progenitor star. The characteristics of the progenitor stars can be constrained by GRB luminosity observations, and the results exceed usual expectations.LGRBs lasting from several seconds to tens of seconds in the rest frame may originate from solar-metallicity (Z ∼ 1 Z ⊙ , where Z and Z ⊙ are the metallicities of progenitor stars and the Sun), massive (M 34 M ⊙ , where M and M ⊙ are the masses of progenitor stars and the Sun) stars or some zero-metallicity (Z ∼ 0) stars. A fraction of low-metallicity (Z 10 −2 Z ⊙ ) stars, including Population III stars, can produce ULGRBs such as GRB 111209A. The fraction of LGRBs lasting less than tens of seconds in the rest frame is more than 40%, which cannot conform to the fraction of the demanded type of progenitor star. It possibly implies that the activity timescale of central engine may be much longer than the observed timescale of prompt emission phase, as indicated by X-ray late-time activities. Alternatively, LGRBs and ULGRBs may be powered by a millisecond magnetar central engine.

show abstract

“…It is desirable to consider also the case of much lower jet luminosities and longer engine timescales, to test out the Irwin & Chevalier (2016) model discussed in Chapter 2. However, this comes with a few technical challenges.…”

Section: Jet Injectionmentioning

confidence: 99%

“…For example, if the operating time of the jet is sufficiently long to escape the progenitor star, but not the extended envelope, the envelope can suffocate the jet leading to a quasi-spherical, mildly relativistic "choked jet" explosion that produces a transient in γ-rays and X-rays when it breaks out (Nakar 2015). On the other hand, if the jet's luminosity is low and its duration is long, it can be collimated by the extended envelope; in this case a weak GRB is produced after the jet drills through the envelope, and later interaction of the SN with the remaining envelope material powers an early optical signal (Irwin & Chevalier 2016). Both of these interpretations have been put forward to explain the peculiarly long and faint GRB 060218 and its associated SN 2006aj (Nakar 2015;Irwin & Chevalier 2016).…”

Section: Introductionmentioning

confidence: 99%

“…On the other hand, if the jet's luminosity is low and its duration is long, it can be collimated by the extended envelope; in this case a weak GRB is produced after the jet drills through the envelope, and later interaction of the SN with the remaining envelope material powers an early optical signal (Irwin & Chevalier 2016). Both of these interpretations have been put forward to explain the peculiarly long and faint GRB 060218 and its associated SN 2006aj (Nakar 2015;Irwin & Chevalier 2016). …”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Long-Duration, Low-Luminosity Gamma-Ray Bursts: Towards a Comprehensive Model of the Weakest Engine-Driven Explosions

Irwin¹

View full text Add to dashboard Cite

Long-duration, low-luminosity gamma-ray bursts (LLGRBs) are a peculiar subclass of gamma-ray bursts (GRBs) that are up to 5 orders of magnitude less luminous than typical bursts. The observation of Type Ic supernovae (SNe) accompanying LLGRBs supports the notion that, like typical GRBs, they are powered by the gravitational collapse of a massive star's core, but beyond this little is known about their origin, and the differences between the progenitors of LLGRBs and GRBs are unclear.In this dissertation, I present analytical and numerical modeling that aims to improve our understanding of the physical conditions leading to LLGRBs.We consider first the unusual GRB 060218, a well-studied event that is prototypical of the long-duration LLGRB class. We present a model for this burst that can account for the prompt X-ray emission lasting for ∼ 3000 s, the early optical peak lasting for hours, and the X-ray and radio afterglow lasting for several days.The basic ingredients of the model are a long-lived jet (t j ∼ 3000 s) with an unusually low luminosity (L j ∼ 10 47 erg s −1 ), a progenitor star surrounded by an extended (∼ 10 13 cm), optically thick, low-mass (∼ 10 −2 M ) envelope, and a modest amount of dust (A V ∼ 0.1) in the interstellar environment.We fit the observed thermal component of the prompt X-ray emission with a simple photospheric model, and then calculate the nonthermal emission due to inverseCompton (IC) scattering of thermal photons from the external shocks of the jet. We find that this model can fit the observed nonthermal emission, if the conditions are such that the reverse shock dominates the emission. We show that the low-power jet can successfully traverse the progenitor star and extended envelope, and that it can also produce the observed radio emission via external shock synchrotron emission at late times. In the meantime, fast ejecta from the associated SN 2006aj shock the iii extended envelope, which emits a burst of optical emission as it expands and cools, consistent with the early optical peak. We interpret the anomalous X-ray afterglow in GRB 060218 as a light echo from dust situated ∼ 30 pc from the burst. Our results suggest that LLGRB progenitors are shrouded in dense circumstellar envelopes, and that they require both a jet and a supernova. Support for this view comes fromNakar (2015), who considered a different model for LLGRBs involving choked jets, but arrived at the same main conclusions.Motivated by these results, we also perform numerical simulations of jets with standard GRB properties in stars with extended envelopes. We present analytical calculations that predict whether or not the jet escapes successfully from the envelope, and apply them to interpret the numerical results. We find that the jet-driven outflow is more well-confined by the envelope than previous analytical results suggested, leading to a flow that is far from spherically symmetric when it breaks out of the envelope. This is generally true for a wide range of physical parameters. Even though the outf...

show abstract

Jet or shock breakout? The low-luminosity GRB 060218

Cited by 54 publications

References 95 publications

iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor

iPTF15dtg: a double-peaked Type Ic supernova from a massive progenitor

Black Hole Hyperaccretion Inflow–Outflow Model. I. Long and Ultra-long Gamma-Ray Bursts

Long-Duration, Low-Luminosity Gamma-Ray Bursts: Towards a Comprehensive Model of the Weakest Engine-Driven Explosions

Contact Info

Product

Resources

About