Gamma-ray observations of SN 1987A from Antarctica

Rester, A.C.; Coldwell, R. L.; Dunnam, F.E.; Eichhorn, G.; Trombka, J. I.; Starr, R.; Lasche, G. P.

doi:10.1086/185487

Cited by 31 publications

(11 citation statements)

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“…3 In fact, although the probability to detect prompt emission is predicted to be far higher for thermonuclear SNe than for core-collapse SNe, the two strongest detections have been from an SN of the latter type. SN 1987A was detected at 847 and 1238 keV (from 56 Co decays) by the Solar Maximum Mission (SMM ) instrument (Matz & Share 1990) and with balloon-borne instruments (Mahoney et al 1988;Rester et al 1989;Teegarden et al 1989;Tueller et al 1990;Kazaryan et al 1990;Ait-Ouamer et al 1990) and at 122 keV (from 57 Co decays) by the Compton Gamma Ray Observatory (CGRO) OSSE instrument (Kurfess et al 1992).…”

Section: Introductionmentioning

confidence: 99%

Unified One‐Dimensional Simulations of Gamma‐Ray Line Emission from Type Ia Supernovae

Milne

Hungerford

Fryer

et al. 2004

ApJ

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The light curves of Type Ia supernovae (SNe Ia) are powered by gamma rays emitted by the decay of radioactive elements such as 56 Ni and its decay products. These gamma rays are downscattered, absorbed, and eventually reprocessed into the optical emission that makes up the bulk of all SN observations. Detection of the gamma rays that escape the expanding star provide the only direct means to study this power source for SN Ia light curves. Unfortunately, disagreements between calculations for the gamma-ray lines have made it difficult to interpret any gamma-ray observations. Here we present a detailed comparison of the major gamma-ray line transport codes for a series of one-dimensional SN Ia models. Discrepancies in past results were due to errors in the codes, and the corrected versions of the seven different codes yield very similar results. This convergence of the simulation results allows us to infer more reliable information from the current set of gamma-ray observations of SNe Ia. The observations of SN 1986G, SN 1991T, and SN 1998bu are consistent with explosion models based on their classification:

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Section: Introductionmentioning

confidence: 99%

Unified One‐Dimensional Simulations of Gamma‐Ray Line Emission from Type Ia Supernovae

Milne

Hungerford

Fryer

et al. 2004

ApJ

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“…The principles can best be understood in terms of a perfectly coaxial detector having a uniform density of p-donors. The electric field then has three components: (1) that which is due to the positive high voltage, V, connected to the outer conductor, /~1 (F) =-V/r.ln(r2/rl)/?, which is that of a cylindrical capacitor, (2) …”

Section: Introduction +mentioning

confidence: 99%

“…The terminal drift velocities of electrons and holes were formulated empirically by RAUDORF and PEHL 5 as follows: (2) [1+(e/e0) ] where, for germanium at 80K, Eo=210.5V/cm, J3=1.36, and go=0.0042 cm2/V/100ns for holes, and Eo=275 V/cm, J3= 1.32, and go=0.0036 cm2/V/100 ns for electrons.…”

Section: Introduction +mentioning

confidence: 99%

Using pulse shape discrimination to sort individual energy deposition events in a germanium crystal

Aalseth

Avignone

Brodzinski

et al. 1998

J Radioanal Nucl Chem

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A fast digital oscilloscope based pulse shape discrimination (PSD) system has been tested with intrinsic germanium detectors large enough to allow ionizing events which generate localized electron-hole pairs at a single site to be segregated from those depositing energy at several different sites in the crystal. Drift velocities of the electrons and holes result in pulses several hundred nanoseconds long. Since the electric field varies by almost a factor of 10 between the outer and inner surfaces, collection of electrons and holes can frequently be distinguished, and pulses due to multi-site events can be distinguished from single site events.

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“…Gamma-ray lines from 56 Co decay, at 847 and 1238 keV, were detected in SN 1987A with the GRS instrument of the SMM satellite (Matz et al 1988) and confirmed by several ballon-borne instruments (i.e., Teegarden et al 1989, Mahoney et al 1988, Sandie et al 1988, Cook et al 1988, Rester et al 1989. One surprising fact was the appearence of these lines only 200 days after the explosion (Matz et al, 1988), much earlier than expected.…”

Section: Observational Cluesmentioning

confidence: 71%

Explosive Nucleosynthesis

Hernanz¹

2011

Encyclopedia of Astrobiology

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Many radioactive nuclei relevant for gamma-ray astrophysics are synthesized during explosive events, such as classical novae and supernovae. A review of recent results of explosive nucleosynthesis in these scenarios will be presented, with a special emphasis on the ensuing gamma-ray emission from individual nova and supernova explosions. The influence of the dynamic properties of the ejecta on the gamma-ray emission features, as well as the still remaining uncertainties in nova and supernova modelling will also be reviewed.

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Gamma-ray observations of SN 1987A from Antarctica

Cited by 31 publications

References 0 publications

Unified One‐Dimensional Simulations of Gamma‐Ray Line Emission from Type Ia Supernovae

Unified One‐Dimensional Simulations of Gamma‐Ray Line Emission from Type Ia Supernovae

Using pulse shape discrimination to sort individual energy deposition events in a germanium crystal

Explosive Nucleosynthesis

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