An imaging observation of SN 1987A at gamma-ray energies

Cook, W. R.; Palmer, D. M.; Prince, Thomas A.; Schindler, S. M.; Starr, C. H.; Stone, E. C.

doi:10.1086/185318

Cited by 46 publications

(16 citation statements)

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“…The daughter products of radioactive elements are usually not in their nuclear ground states, but rapid de-excitation occurs through the emission of γ-ray lines (Table 6.2). The nuclear decay lines of 56 Co at 847 keV and 1238 keV have been detected from SN 1987A by several balloon and satellite experiments (Cook et al, 1988;Mahoney et al, 1988;Sandie et al, 1988;Teegarden et al, 1989, see also Sect. 9.2).…”

Section: Line Emission Associated With Radioactivitymentioning

confidence: 91%

Supernova remnants: the X-ray perspective

Vink

2011

Astron Astrophys Rev

435

323

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Supernova remnants are beautiful astronomical objects that are also of high scientific interest, because they provide insights into supernova explosion mechanisms, and because they are the likely sources of Galactic cosmic rays. X-ray observations are an important means to study these objects. And in particular the advances made in X-ray imaging spectroscopy over the last two decades has greatly increased our knowledge about supernova remnants. It has made it possible to map the products of fresh nucleosynthesis, and resulted in the identification of regions near shock fronts that emit X-ray synchrotron radiation. Since X-ray synchrotron radiation requires 10-100 TeV electrons, which lose their energies rapidly, the study of X-ray synchrotron radiation has revealed those regions where active and rapid particle acceleration is taking place.In this text all the relevant aspects of X-ray emission from supernova remnants are reviewed and put into the context of supernova explosion properties and the physics and evolution of supernova remnants. The first half of this review has a more tutorial style and discusses the basics of supernova remnant physics and X-ray spectroscopy of the hot plasmas they contain. This includes hydrodynamics, shock heating, thermal conduction, radiation processes, non-equilibrium ionization, He-like ion triplet lines, and cosmic ray acceleration. The second half offers a review of the advances made in field of X-ray spectroscopy of supernova remnants during the last 15 year. This period coincides with the availability of X-ray imaging spectrometers. In addition, I discuss the results of high resolution X-ray spectroscopy with the Chandra and XMM-Newton gratings. Although these instruments are not ideal for studying extended sources, they nevertheless provided interesting results for a limited number of remnants. These results provide a glimpse of what may be achieved with future microcalorimeters that will be available on board future X-ray observatories. In discussing the results of the last 15 years I have chosen to discuss a few topics that are of particular interest. These include the properties of Type Ia supernova remnants, which appear to be regularly shaped and have stratified ejecta, in contrast to core collapse supernova remnants, which have patchy ejecta distributions. For core collapse supernova remnants I discuss the spatial distribution of fresh nucleosynthesis products, but also their properties in connection to the neutron stars they contain.For the mature supernova remnants I focus on the prototypal supernova remnants Vela and the Cygnus Loop. And I discuss the interesting class of mixed-morphology remnants. Many of these mature supernova remnants contain still plasma with enhanced ejecta abundances. Over the last five years it has also become clear that many mixed-morphology remnants contain plasma that is overionized. This is in contrast to most other supernova remnants, which contain underionized plasmas.This text ends with a review of X-ray synchrotron radiatio...

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Section: Line Emission Associated With Radioactivitymentioning

confidence: 91%

Supernova remnants: the X-ray perspective

Vink

2011

Astron Astrophys Rev

435

323

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“…However, more 56 Co positrons will escape if the expansion is fast (Cassé et al, 2004;Vink, 2004). This led Cassé et al (2004) to the suggestion that a hypernova in the Galactic center region may be responsible for the 511 keV electronpositron line emission from that region (Kinzer et al, 2001; (Cook et al, 1988;Mahoney et al, 1988;Sandie et al, 1988;Teegarden et al, 1989), and the gammaray spectrometer (GRS) on board the Solar Maximum Mission (SMM) satellite (Matz et al, 1988;Leising and Share, 1990, see Fig. 2).…”

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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“…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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An imaging observation of SN 1987A at gamma-ray energies

Abstract: Cl 1m. Tllt Am

Cited by 46 publications

References 4 publications

Supernova remnants: the X-ray perspective

Supernova remnants: the X-ray perspective

Gamma-ray observations of explosive nucleosynthesis products

Explosive Nucleosynthesis

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