The unusual γ-ray burst GRB 101225A from a helium star/neutron star merger at redshift 0.33

Thöne, C. C.; Postigo, A. de Ugarte; Fryer, Chris L.; Page, K. L.; Gorosabel, J.; Aloy, M. Á.; Perley, D.; Kouveliotou, C.; Janka, Hans-Thomas; Mimica, P.; Racusin, J. L.; Krimm, H. A.; Cummings, J. R.; Oates, S. R.; Holland, S. T.; Siegel, M. H.; Pasquale, M. de; Сонбас, Э.; Im, Myungshin; Park, W.-K.; Канн, Д. А.; Guziy, S.; García, L. Hernández; Llorente, A.; Bundy, Kevin; Choi, Changsu; Jeong, Hyeonju; Korhonen, H.; Kubánek, P.; Lim, Juhee; Москвитин, А. С.; Muñoz-Darias, T.; Pak, Soojong; Parrish, Ian J.

doi:10.1038/nature10611

Cited by 124 publications

(89 citation statements)

References 20 publications

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“…The helium-merger model, for example, predicts a massive shell very close to the exploding star. The first possible evidence of such a progenitor may be the recent "Christmas" burst (Thöne et al 2011). With detailed models, we may be able to place velocity and mass constraints on these shells.…”

Section: Discussionmentioning

confidence: 99%

Gamma-Ray Bursts in Circumstellar Shells: A Possible Explanation for Flares

Mesler

Whalen

Lloyd-Ronning

et al. 2012

ApJ

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It is now generally accepted that long-duration gamma-ray bursts (GRBs) are due to the collapse of massive rotating stars. The precise collapse process itself, however, is not yet fully understood. Strong winds, outbursts, and intense ionizing UV radiation from single stars or strongly interacting binaries are expected to destroy the molecular cloud cores that give birth to them and create highly complex circumburst environments for the explosion. Such environments might imprint features on GRB light curves that uniquely identify the nature of the progenitor and its collapse. We have performed numerical simulations of realistic environments for a variety of long-duration GRB progenitors with ZEUS-MP and have developed an analytical method for calculating GRB light curves in these profiles. Though a full, three-dimensional, relativistic magnetohydrodynamical computational model is required to precisely describe the light curve from a GRB in complex environments, our method can provide a qualitative understanding of these phenomena. We find that, in the context of the standard afterglow model, massive shells around GRBs produce strong signatures in their light curves, and that this can distinguish them from those occurring in uniform media or steady winds. These features can constrain the mass of the shell and the properties of the wind before and after the ejection. Moreover, the interaction of the GRB with the circumburst shell is seen to produce features that are consistent with observed X-ray flares that are often attributed to delayed energy injection by the central engine. Our algorithm for computing light curves is also applicable to GRBs in a variety of environments such as those in high-redshift cosmological halos or protogalaxies, both of which will soon be targets of future surveys such as the Joint Astrophysics Nascent Satellite or Lobster.

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Section: Discussionmentioning

confidence: 99%

Gamma-Ray Bursts in Circumstellar Shells: A Possible Explanation for Flares

Mesler

Whalen

Lloyd-Ronning

et al. 2012

ApJ

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“…However, this burst is known to be peculiar, being its optical emission dominated by a supernova component and not the afterglow (Campana et al 2006;Soderberg et al 2006; see also Thöne et al 2011). GRB 050509B an extremely faint short burst, most probably hosted by a giant elliptical galaxy at z = 0.22 (Hjorth et al 2005;Gehrels et al 2005;Castro-Tirado et al 2005) is the following dimmest limit.…”

Section: Redshift Distribution and Luminositiesmentioning

confidence: 99%

Pre-ALMA observations of GRBs in the mm/submm range

Postigo

Lundgren

Martín

et al. 2012

A&A

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Context. Gamma-ray bursts (GRBs) generate an afterglow emission that can be detected from radio to X-rays during days, or even weeks after the initial explosion. The peak of this emission crosses the millimeter and submillimeter range during the first hours to days, making their study in this range crucial for constraining the models. Observations have been limited until now due to the low sensitivity of the observatories in this range. This situation will be greatly improved with the start of scientific operations of the Atacama Large Millimeter/submillimeter Array (ALMA). Aims. In this work we do a statistical analysis of the complete sample of mm/submm observations of GRB afterglows obtained before the beginning of scientific operations at ALMA. Methods. We present observations of 11 GRB afterglows obtained from the Atacama Pathfinder Experiment (APEX) and the SubMillimeter Array (SMA), as well as the first detection of a GRB with ALMA, still in the commissioning phase, and put them into context with a catalogue of all the observations that have been published until now in the spectral range that is covered by ALMA.Results. The catalogue of mm/submm observations collected here is the largest to date and is composed of 102 GRBs, of which 88 have afterglow observations, whereas the rest are host galaxy searches. With our programmes, we contributed with data of 11 GRBs and the discovery of 2 submm counterparts. In total, the full sample, including data from the literature, has 22 afterglow detections with redshifts ranging from 0.168 to 8.2. GRBs have been detected in mm/submm wavelengths with peak luminosities spanning 2.5 orders of magnitude, the most luminous reaching 10 33 erg s −1 Hz −1 . We observe a correlation between the X-ray brightness at 0.5 days and the mm/submm peak brightness. Finally we give a rough estimate of the distribution of peak flux densities of GRB afterglows, based on the current mm/submm sample. Conclusions. Observations in the mm/submm bands have been shown to be crucial for our understanding of the physics of GRBs, but have until now been limited by the sensitivity of the observatories. With the start of the operations at ALMA, the sensitivity has improved by more than an order of magnitude, opening a new era in the study of GRB afterglows and their host galaxies. Our estimates predict that, once completed, ALMA will detect up to ∼98% of the afterglows if observed during the passage of the peak synchrotron emission.

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“…Stripping the envelope and spinning-up the core can be achieved by several channels involving CEE (for a review of this and of alternative possibilities, see Fryer et al 2007; also Podsiadlowski et al 2010). One notable recently observed GRB has been explained using a specific CEE-based model (see Thöne et al 2011; for the underlying model see, e.g., Fryer and Woosley 1998).…”

Section: A Crucial Astrophysical Processmentioning

confidence: 99%

Common envelope evolution: where we stand and how we can move forward

Іванова

Justham

Chen

et al. 2013

Astron Astrophys Rev

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587

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This work aims to present our current best physical understanding of common-envelope evolution (CEE). We highlight areas of consensus and disagree- ment, and stress ideas which should point the way forward for progress in this important but long-standing and largely unconquered problem. Unusually for CEE-related work, we mostly try to avoid relying on results from population synthesis or observations, in order to avoid potentially being misled by previous misunderstandings. As far as possible we debate all the relevant issues starting from physics alone, all the way from the evolution of the binary system immediately before CEE begins to the processes which might occur just after the ejection of the envelope. In particular, we include extensive discussion about the energy sources and sinks operating in CEE, and hence examine the foundations of the standard energy formalism. Special attention is also given to comparing the results of hydrodynamic simulations from different groups and to discussing the potential effect of initial conditions on the differences in the outcomes. We compare current numerical techniques for the problem of CEE and also whether more appropriate tools could and should be produced (including new formulations of computational hydrodynamics, and attempts to include 3D processes within 1D codes). Finally we explore new ways to link CEE with observations. We compare previous simulations of CEE to the recent outburst from V1309 Sco, and discuss to what extent post-common-envelope binaries and nebulae can provide information, e.g. from binary eccentricities, which is not currently being fully exploited.

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The unusual γ-ray burst GRB 101225A from a helium star/neutron star merger at redshift 0.33

Cited by 124 publications

References 20 publications

Gamma-Ray Bursts in Circumstellar Shells: A Possible Explanation for Flares

Gamma-Ray Bursts in Circumstellar Shells: A Possible Explanation for Flares

Pre-ALMA observations of GRBs in the mm/submm range

Common envelope evolution: where we stand and how we can move forward

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