COMPTEL upper limits for the $^{\sf 56}$Co<i>γ</i>-ray emission from SN1998bu

Georgii, R.; Plüschke, S.; Diehl, R.; Lichti, G.; Schönfelder, V.; Bloemen, H.; Hermsen, W.; Ryan, J. M.; Bennett, K.

doi:10.1051/0004-6361:20021133

Cited by 33 publications

(31 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Comparing these interpretations with Georgii et al (2002), the conclusions are similar, but not identical. Principally, at the larger distance, that work only rejects the high 56 Ni producing models, while at the shorter distance that work rejects all normally luminous models.…”

Section: Cgro Comptel Observv Ations Of Sn 1998bumentioning

confidence: 85%

“…and (À0:6 AE 1:6) ; 10 À5 photons cm À2 s À1 for the 847 and 1238 keV lines (M. D. Leising 2004, private communication). The COMPTEL 2 upper limits are 3:1 ; 10 À5 and 2:3 ; 10 À5 photons cm À2 s À1 , respectively (using the lower of the imaging and spectral analysis results for each line, from Georgii et al 2002).…”

Section: Cgro Comptel Observv Ations Of Sn 1998bumentioning

confidence: 99%

See 1 more Smart Citation

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

Milne

Hungerford

Fryer

et al. 2004

ApJ

View full text Add to dashboard Cite

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:

show abstract

Section: Cgro Comptel Observv Ations Of Sn 1998bumentioning

confidence: 85%

Section: Cgro Comptel Observv Ations Of Sn 1998bumentioning

confidence: 99%

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

Milne

Hungerford

Fryer

et al. 2004

ApJ

View full text Add to dashboard Cite

show abstract

“…For SN 1998bu Based on observations collected at the La Silla and Paranal observatories of the European Southern observatory, Chile in time allocated to proposals 63.H-0527, 63.H-0649. Georgii et al (2002) report upper limits for the amount of 56 Ni manufactured in the explosion from the absence of 56 Co γ-ray emission. Their 2-σ upper limit is 0.35 M of 56 Ni.…”

Section: Introductionmentioning

confidence: 99%

Optical and near infrared observations of SN 1998bu

Spyromilio

Gilmozzi

Sollerman

et al. 2004

A&A

View full text Add to dashboard Cite

Abstract. Infrared and optical spectra of SN 1998bu at an age of one year after explosion are presented. The data show evidence for the radioactive decay of 56 Co to 56 Fe, long assumed to be the powering source for the supernova light curve past maximum light. The spectra provide direct evidence for at least 0.4 solar masses of iron being present in the ejecta of the supernova. The fits to the data also show that the widths of the emission lines increase with time. Photometric measurements in the H-band show that the supernova is not fading during the observation period. This is consistent with theoretical expectations.

show abstract

“…The second event during the CGRO mission was SN1998bu at 17 Mpc. It was much fainter, and no gamma-ray emission could be detected [36].…”

Section: Supernovae Of Type Iamentioning

confidence: 99%

Cosmic Gamma-Ray Spectroscopy

Diehl

2013

Astronomical Review

View full text Add to dashboard Cite

Penetrating gamma-rays require complex instrumentation for astronomical spectroscopy measurements of gamma-rays from cosmic sources. Multiple-interaction detectors in space combined with sophisticated postprocessing of detector events on ground have lead to a spectroscopy performance which is now capable to provide new astrophysical insights. Spectral signatures in the MeV regime originate from transitions in the nuclei of atoms (rather than in their electron shell). Nuclear transitions are stimulated by either radioactive decays or high-energy nuclear collisions such as with cosmic rays. Gamma-ray lines have been detected from radioactive isotopes produced in nuclear burning inside stars and supernovae, and from energetic-particle interactions in solar flares. Radioactive-decay gamma-rays from 56 Ni directly reflect the source of supernova light. 44 Ti is produced in core-collapse supernova interiors, and the paucity of corresponding 44 Ti gamma-ray line sources reflects the variety of dynamical conditions herein. 26 Al and 60 Fe are dispersed in interstellar space from massive-star nucleosynthesis over millions of years. Gamma-rays from their decay are measured in detail by gamma-ray telescopes, astrophysical interpretations reach from massive-star interiors to dynamical processes in the interstellar medium. Nuclear de-excitation gamma-ray lines have been found in solar-flare events, and convey information about energetic-particle production in these events, and their interaction in the solar atmosphere. The annihilation of positrons leads to another type of cosmic gamma-ray source. The characteristic annihilation gamma-rays at 511 keV have been measured long ago in solar flares, and now throughout the interstellar medium of our Milky Way galaxy. But now a puzzle has appeared, as a surprising predominance of the central bulge region was determined. This requires either new positron sources or transport processes not yet known to us. In this paper we discuss instrumentation and data processing for cosmic gamma-ray spectroscopy, and the astrophysical issues and insights from these measurements.

show abstract

COMPTEL upper limits for the $^{\sf 56}$Coγ-ray emission from SN1998bu

Cited by 33 publications

References 32 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

Optical and near infrared observations of SN 1998bu

Cosmic Gamma-Ray Spectroscopy

Contact Info

Product

Resources

About