Oriented Scintillation Spectrometer Experiment observations of Co-57 in SN 1987A

Kurfess, J. D.; Johnson, W. N.; Kinzer, R. L.; Kroeger, R. A.; Strickman, M. S.; Grove, J. E.; Leising, M. D.; Clayton, Donald D.; Grabelsky, D. A.; Purcell, W. R.; Ulmer, M. P.; Cameron, R. A.; Jung, G. V.

doi:10.1086/186626

Cited by 119 publications

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“…Together with the 56 Ni mass of 0.069 M and the 57 Ni mass of ∼3.3 × 10 −3 M (Fransson & Kozma 1993;Varani et al 1990;Kurfess et al 1992), the determination of the 44 Ti mass should put considerable constraints on supernova explosion models. Our result of 1.5 +0.5 −0.5 × 10 −4 M agrees with the result of (1−2) × 10 −4 M found in C97, although that result was based on an analysis of [Fe II] lines, whose identifications are different in our model on several instances, and on the [O I] λλ6300, 6364 doublet, whose emission is highly sensitive to uncertain charge transfer reactions, and which is also contaminated by Fe I lines.…”

Section: Discussionmentioning

confidence: 98%

The⁴⁴Ti-powered spectrum of SN 1987A

Jerkstrand

Fransson

Kozma

2011

A&A

171

249

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SN 1987A provides a unique opportunity to study the evolution of a supernova from explosion into very late phases. Owing to the rich chemical structure, the multitude of physical processes involved and extensive radiative transfer effects, detailed modeling is needed to interpret the emission from this and other supernovae. In this paper, we analyze the late-time (about eight years) Hubble Space Telescope spectrum of the SN 1987A ejecta, where 44 Ti is the dominant power source. Based on an explosion model for a 19 M progenitor, we compute a model spectrum by calculating the degradation of positrons and gamma-rays from the radioactive decays, solving the equations governing temperature, ionization balance and NLTE level populations, and treating the radiative transfer with a Monte Carlo technique. We obtain a UV/optical/NIR model spectrum that reproduces most of the lines in the observed spectrum with good accuracy. We find non-local radiative transfer in atomic lines to be an important process also at this late stage of the supernova, with ∼30% of the emerging flux in the optical and NIR coming from scattering/fluorescence. We investigate the question of where the positrons deposit their energy, and favor the scenario where they are locally trapped in the Fe/He clumps by a magnetic field. Energy deposition into these largely neutral Fe/He clumps makes Fe I lines prominent in the emerging spectrum. With the best available estimates for the dust extinction, we determine the amount of 44 Ti produced in the explosion to be 1.5 +0.5 −0.5 × 10 −4 M .

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Section: Discussionmentioning

confidence: 98%

The⁴⁴Ti-powered spectrum of SN 1987A

Jerkstrand

Fransson

Kozma

2011

A&A

171

249

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“…• Characteristic Ni decay gamma-rays have been observed from SN1987A [ 48,30,23], directly confirming supernova production of fresh isotopes up to iron group nuclei.…”

Section: Introductionmentioning

confidence: 69%

Gamma-ray Line Astronomy

Diehl

2005

Nuclear Physics A

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Gamma-ray lines from radioactive isotopes, ejected into interstellar space by cosmic nucleosynthesis events, are observed with new space telescopes. The Compton Observatory had provided a sky survey for the isotopes 56 Co, 22 Na, 44 Ti, and 26 Al, detecting supernova radioactivity and the diffuse glow of long-lived radioactivity from massive stars in the Galaxy. High-resolution spectroscopy is now being exploited with Ge detectors: Since 2002, with ESA's INTEGRAL satellite and the RHESSI solar imager two spacebased Ge-gamma-ray telescopes are in operation, measuring Doppler broadenings and line shape details of cosmic gamma-ray lines. First year's results include a detection and line shape measurement of annihilation emission, and 26 Al emission from the inner Galaxy and from the Cygnus region.60 Fe gamma-ray intensity is surprisingly low; it may have been detected by RHESSI at 10% of the 26 Al brightness, yet is not seen by INTEGRAL. 44 Ti emission from Cas A and SN1987A is being studied; no other candidate young supernova remnants have been found through 44 Ti. 22 Na from novae still is not seen.

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“…The detection of the 122 keV supernova line from SN1987a) was reported by OSSE (Kurfess et al 1992). Neutrons interacting with Ni nuclei inside the shield will produce the 122 and 136 keV lines through the 58 Ni(n, 2n) 57 Ni(β + ) 57 Co reaction.…”

Section: The Problemmentioning

confidence: 92%

Neutron-induced nuclear reactions and degradation in germanium detectors

Leleux

Albernhe

Borrel

et al. 2003

A&A

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Abstract. We have measured cross sections of neutron-induced nuclear reactions leading to the delayed production of γ-ray lines similar to the ones of astrophysical interest. Conclusions were drawn concerning the expected background in the 26 Al 1809 keV line and the 7 Be 478 keV line in SPI. The neutron-induced degradation of Ge detectors was studied vs. the neutron energy, the neutron fluence and the detector temperature. Performance recovery of the detectors was studied for different annealing temperatures. Optimum temperature and times for annealing were determined.

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Oriented Scintillation Spectrometer Experiment observations of Co-57 in SN 1987A

Cited by 119 publications

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The⁴⁴Ti-powered spectrum of SN 1987A

The⁴⁴Ti-powered spectrum of SN 1987A

Gamma-ray Line Astronomy

Neutron-induced nuclear reactions and degradation in germanium detectors

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Oriented Scintillation Spectrometer Experiment observations of Co-57 in SN 1987A

Cited by 119 publications

References 0 publications

The44Ti-powered spectrum of SN 1987A

The44Ti-powered spectrum of SN 1987A

Gamma-ray Line Astronomy

Neutron-induced nuclear reactions and degradation in germanium detectors

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The⁴⁴Ti-powered spectrum of SN 1987A

The⁴⁴Ti-powered spectrum of SN 1987A