Observations of gamma-ray line profiles from SN 1987A

Tueller, J.; Barthelmy, S. D.; Gehrels, N.; Teegarden, B. J.; Leventhal, M.; MacCallum, C. J.

doi:10.1086/185675

Cited by 87 publications

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“…However, the high spectral resolution observations of SN 1987A showed that the 847 keV and 1238 keV lines were broadened by ∼ 3000km s −1 (FWHM) and redshifted by ∼ 400km s −1 (Sandie et al, 1988;Teegarden et al, 1989;Tueller et al, 1990). This discrepancy is still not understood, but it clearly points to an asymmetric explosion.…”

Section: Gamma-ray Lines From Supernovaementioning

confidence: 99%

Gamma-ray observations of explosive nucleosynthesis products

Vink

2005

Advances in Space Research

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In this review I discuss the various γ-ray emission lines that can be expected and, in some cases have been observed, from radioactive explosive nucleosynthesis products. The most important γ-ray lines result from the decay chains of 56 Ni, 57 Ni, and 44 Ti. 56 Ni is the prime explosive nucleosynthesis product of Type Ia supernovae, and its decay determines to a large extent the Type Ia light curves.56 Ni is also a product of core-collapse supernovae, and in fact, γ-ray line emission from its daughter product, 56 Co, has been detected from SN1987A by several instruments. The early occurrence of this emission was surprising and indicates that some fraction of 56 Ni, which is synthesized in the innermost supernova layers, must have mixed with the outermost supernova ejecta.Special attention is given to the γ-ray line emission of the decay chain of 44 Ti ( 44 Ti→ 44 Sc→ 44 Ca), which is accompanied by line emission at 68 keV, 78 keV, and 1157 keV. As the decay time of 44 Ti is ∼ 86 yr, one expects this line emission from young supernova remnants. Although the 44 Ti yield (typically 10 −5 − 10 −4 M⊙) is not very high, its production is very sensitive to the energetics and asymmetries of the supernova explosion, and to the mass cut, which defines the mass of the stellar remnant. This makes 44 Ti an ideal tool to study the inner layers of the supernova explosion. This is of particular interest in light of observational evidence for asymmetric supernova explosions.The γ-ray line emission from 44 Ti has so far only been detected from the supernova remnant Cas A. I discuss these detections, which were made by COMPTEL (the 1157 keV line) and BeppoSAX (the 68 keV and 78 keV lines), which, combined, give a flux of (2.6 ± 0.4 ± 0.5) × 10 −5 ph cm −2 s −1 per line, suggesting a 44 Ti yield of (1.5 ± 1.0) × 10 −4 M⊙. Moreover, I present some preliminary results of Cas A observations by INTEGRAL, which so far has yielded a 3σ detection of the 68 keV line with the ISGRI instrument with a flux that is consistent with the BeppoSAX detections. Future observations by INTEGRAL-ISGRI will be able to constrain the continuum flux above 90 keV, as the uncertainty about the continuum shape, is the main source of systematic error for the 68 keV and 78 keV line flux measurements. Moreover, with the INTEGRAL-SPI instrument it will be possible to measure or constrain the line broadening of the 1157 keV line. A preliminary analysis of the available data indicates that narrow line emission (i.e. ∆v < 1000 km s −1 ) can be almost excluded at the 2σ level, for an assumed line flux of 1.9 × 10 −5 ph cm −2 s −1 .

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Section: Gamma-ray Lines From Supernovaementioning

confidence: 99%

Gamma-ray observations of explosive nucleosynthesis products

Vink

2005

Advances in Space Research

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“…Radioactive 56C0 from the explosively burned oxygen layer was observed much sooner after the explosion 1) Supported by the NASA ESS HPCC Program under Grant Number NAGS-2652 than predicted by spherically symmetric explosion models, implying that the 56C0 had been mixed well into the outer layers. Doppler broadening of the 'Co implied velocities in excess of 3000 gamma-ray and optical lines from km/s [32,31,22], whereas modeling to date predicts maximum velocities of< 2000 km/s. Also, the 'Bochum event' [29,17,8] showed spectroscopic features suggesting enhanced heating of the envelope, presumably due to mixing from the radioactive core.…”

Section: Introductionmentioning

confidence: 99%

Supernova-relevant hydrodynamic instability experiments on the Nova laser

Kane¹,

Arnett²,

Remington³

et al. 1997

The 13th International Conference on Laser Interactions and Related Plasma Phenomena

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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: 70%

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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Observations of gamma-ray line profiles from SN 1987A

Cited by 87 publications

References 0 publications

Gamma-ray observations of explosive nucleosynthesis products

Gamma-ray observations of explosive nucleosynthesis products

Supernova-relevant hydrodynamic instability experiments on the Nova laser

Gamma-ray Line Astronomy

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