Discovery of an unusual hard X-ray source in the region of supernova 1987A

Dotani, Tadayasu; Hayashida, Kentaro; Inoue, Hajime; Itoh, M.; Koyama, K.; Makino, F.; Mitsuda, Kazuhisa; Murakami, T.; Oda, M.; Ogawara, Y.; Takano, Shiro; Tanaka, Yasuo; Yoshida, A.; Makishima, Kazuo; Ohashi, T.; Kawai, N.; Matsuoka, M.; Hōshi, Reiun; Hayakawa, Satio; Kii, T.; Kunieda, H.; Nagase, F.; Tawara, Yuzuru; Hatsukade, Isamu; Kitamoto, Shunji; Miyamoto, S.; Tsunemi, H.; Yamashita, Kazuya; Nakagawa, M.; Yamauchi, M.; Turner, Martin; Pounds, K. A.; Thomas, H. D.; Stewart, G. C.; Cruise, A. M.; Patchett, B. E.; Reading, D. H.

doi:10.1038/330230a0

Cited by 155 publications

(49 citation statements)

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“…In both of these cases, the time delay before the peak of the supernova's gigahertz radio emission is an order of magnitude longer than that observed for the Type II-P supernova 1987A. Along with the detection of prompt radio emission from supernovae 1987A, 1999em, and 2004dj, all three of these sources have also been detected at X-ray wavelengths (Masai et al 1987;Dotani et al 1987;Rodin et al 1987;Pooley et al 2002;. This is often true for corecollapse supernovae (see Fig.…”

Section: Comparison With Sn 1987a and Sn 1999emmentioning

confidence: 72%

Monitoring of the Prompt Radio Emission from the Unusual Supernova SN 2004dj in NGC 2403

Beswick

Muxlow

Argo

et al. 2005

ApJ

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Section: Comparison With Sn 1987a and Sn 1999emmentioning

confidence: 72%

Monitoring of the Prompt Radio Emission from the Unusual Supernova SN 2004dj in NGC 2403

Beswick

Muxlow

Argo

et al. 2005

ApJ

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“…From two to eight weeks after the explosion, however, no significant flux in the 10-30 keV band was observed by Ginga in the direction of 1987A to a crude upper limit of 10 37 ergs s −1 (Dotani et al 1987;Makino 1987). The lack of a detectable Compton echo therefore places severe constraints on the brightness of a possible GRB jet associated with SN 1987A, as only an unusually weak burst of intrinsic energy E ∼ < few×10 47 ergs would be compatible with the assumed circumstellar density profile.…”

Section: A Lateral Grb Jet From Sn 1987a?mentioning

confidence: 96%

Compton Echoes from Gamma‐Ray Bursts

Madau¹,

Blandford²,

Rees³

2000

ApJ

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Recent observations of gamma-ray bursts (GRBs) have provided growing evidence for collimated outflows and emission, and strengthened the connection between GRBs and supernovae. If massive stars are the progenitors of GRBs, the hard photon pulse will propagate in the pre-burst, dense environment. Circumstellar material will Compton scatter the prompt GRB radiation and give rise to a reflection echo. We calculate luminosities, spectra, and light curves of such Compton echoes in a variety of emission geometries and ambient gas distributions, and show that the delayed hard X-ray flash from a pulse propagating into a red supergiant wind could be detectable by Swift out to z ∼ 0.2. Independently of the γ-ray spectrum of the prompt burst, reflection echoes will typically show a high-energy cutoff between m e c 2 /2 and m e c 2 because of Compton downscattering. At fixed burst energy per steradian, the luminosity of the reflected echo is proportional to the beaming solid angle, Ω b , of the prompt pulse, while the number of bright echoes detectable in the sky above a fixed limiting flux increases as Ω 1/2 b , i.e. it is smaller in the case of more collimated jets. The lack of an X-ray echo at ∼ one month delay from the explosion poses severe constraints on the possible existence of a lateral GRB jet in SN 1987A. The late r-band afterglow observed in GRB990123 is fainter than the optical echo expected in a dense red supergiant environment from a isotropic prompt optical flash. Significant MeV delayed emission may be produced through the bulk Compton (or Compton drag) effect resulting from the interaction of the decelerating fireball with the scattered X-ray radiation.

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“…predicted, x-ray emission of dense, core elements, specifically 56 Ni and 56 Co. Also, peak velocities of some of these dense elements were much higher than the velocities predicted by one-dimensional ͑1D͒ simulations. 21 It is possible that these discrepancies are due to extensive mixing within the layers of the star. The mixing that is believed to occur in this core-collapse supernova has motivated many simulations 8,12,[22][23][24] and experiments.…”

Section: Introductionmentioning

confidence: 98%

Three-dimensional blast-wave-driven Rayleigh–Taylor instability and the effects of long-wavelength modes

et al. 2009

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This paper describes experiments exploring the three-dimensional (3D) Rayleigh–Taylor instability at a blast-wave-driven interface. This experiment is well scaled to the He/H interface during the explosion phase of SN1987A. In the experiments, ∼5 kJ of energy from the Omega laser was used to create a planar blast wave in a plastic disk, which is accelerated into a lower-density foam. These circumstances induce the Richtmyer–Meshkov instability and, after the shock passes the interface, the system quickly becomes dominated by the Rayleigh–Taylor instability. The plastic disk has an intentional pattern machined at the plastic/foam interface. This perturbation is 3D with a basic structure of two orthogonal sine waves with a wavelength of 71 μm and an amplitude of 2.5 μm. Additional long-wavelength modes with a wavelength of either 212 or 424 μm are added onto the single-mode pattern. The addition of the long-wavelength modes was motivated by the results of previous experiments where material penetrated unexpectedly to the shock front, perhaps due to an unintended structure. The current experiments and simulations were performed to explore the effects of this unintended structure; however, we were unable to reproduce the previous results.

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Discovery of an unusual hard X-ray source in the region of supernova 1987A

Cited by 155 publications

References 0 publications

Monitoring of the Prompt Radio Emission from the Unusual Supernova SN 2004dj in NGC 2403

Monitoring of the Prompt Radio Emission from the Unusual Supernova SN 2004dj in NGC 2403

Compton Echoes from Gamma‐Ray Bursts

Three-dimensional blast-wave-driven Rayleigh–Taylor instability and the effects of long-wavelength modes

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