Nuclear γ ray lines in the supernova SN 1987a

AbstractThe changing total luminosity of SN 1987A between 2 and 1200 days after core collapse is illustrated and discussed. From about four weeks after outburst the supernova light curve was dominated by the release of radioactive decay energy; the major contributor being 0.078M⊙ of 56Co. Recently an additional contribution probably from the decay of 57Co and 44Ti appears to be manifesting itself in the light curve. A gradually increasing fraction of the radioactive decay energy has probably been emitted at X- and γ-ray wavelengths; the fluxes are low and no recent measurements have been published. Most of the remaining radioactive decay energy appears to be emitted in the IR and is very difficult to measure. Other factors influencing the interpretation of the recent light curve are the uncertain contribution from long-lived radioactive isotopes and light-echoes. It is therefore premature to make any definitive statements on the contribution from the neutron star, although it is probably less than a few times 1037 erg s−1.

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ULTRA HIGH ENERGY γ-FLUX FROM SUPERNOVA 1987a

Modern Physics Letters A ◽

10.1142/s0217732387001014 ◽

1987 ◽

Vol 02 (11) ◽

pp. 801-804 ◽

Cited By ~ 2

Author(s):

HUMITAKA SATO

Keyword(s):

Southern Hemisphere ◽

Event Rate ◽

Detection System ◽

High Energy ◽

Ultra High Energy ◽

Sn 1987A ◽

Supernova 1987A ◽

Γ Ray ◽

One Year

High energy γ-ray from the SN 1987a in LMC will be observable by such a detection system as used for Cyg X-3, if it is installed in the southern hemisphere. The γ-ray flux will rise and decline in about one year and the maximum event rate could be 104 times larger than Cyg X-3 in some model.

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High Energy γ-ray Observations of SN 1987A

Publications of the Astronomical Society of Australia ◽

10.1017/s1323358000022682 ◽

1988 ◽

Vol 7 (4) ◽

pp. 486-489

Author(s):

R.K. Sood ◽

J.A. Thomas ◽

L. Waldron ◽

R.K. Manchanda ◽

G.K. Rochester ◽

...

Keyword(s):

High Energy ◽

Balloon Flight ◽

X Ray ◽

Preliminary Results ◽

Sn 1987A ◽

Γ Ray

AbstractSN 1987A has been observed with a combined high energy γ-ray (50-500 MeV) and hard X-ray (15-150 keV) payload during a balloon flight on 5 April 1988 from Alice Springs, Australia. The γ-ray observations, along with our earlier ones on 19 April 1987 are the only such observations of the supernova to date. The γ-ray detector characteristics are described. The preliminary results of the recent flight and their implications in terms of the known supernova parameters are discussed.

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Limits of neutrino stability from the γ-ray flux measured in coincidence with neutrinos from SN 1987a

Physics Letters B ◽

10.1016/0370-2693(88)90175-x ◽

1988 ◽

Vol 200 (4) ◽

pp. 580-582 ◽

Cited By ~ 29

Author(s):

F. von Feilitzsch ◽

L. Oberauer

Keyword(s):

Sn 1987A ◽

Γ Ray

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High-energy Emission from Supernovae and Remnants

Symposium - International Astronomical Union ◽

10.1017/s0074180900162874 ◽

2000 ◽

Vol 195 ◽

pp. 135-142

Author(s):

R. A. Chevalier

Keyword(s):

Supernova Remnants ◽

High Energy ◽

Molecular Gas ◽

X Ray ◽

Sn 1987A ◽

Energy Emission ◽

Energetic Radiation ◽

Γ Ray ◽

Composition Structure ◽

High Energy Emission

An early burst of energetic radiation is expected from a supernova at the time of shock breakout. This emission has not been directly observed but has been inferred from the photoionization around SN 1987A. X-ray emission has been detected from core-collapse supernovae in the days to years after the explosion as they interact with their circumstellar winds. Young Galactic supernova remnants provide the possibility of determining the composition structure of the ejecta through X-ray spectroscopy. An exciting finding for older remnants is that a number of remnants that appear to be interacting with molecular gas may be sources of high-energy γ-ray emission. The clumpy structure of molecular clouds has implications for the structure expected in high-energy emission. Finally, the field of γ-ray-line spectroscopy is beginning to yield results relevant to the explosive nucleosynthesis of radionuclides in supernovae.

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SMM γ-Ray Observations of SN 1987A

Supernovae ◽

10.1007/978-1-4612-2988-9_36 ◽

1991 ◽

pp. 261-268

Author(s):

Mark D. Leising ◽

Gerald H. Share

Keyword(s):

Sn 1987A ◽

Γ Ray

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Distance to SN 1987A and the LMC

Symposium - International Astronomical Union ◽

10.1017/s0074180900118959 ◽

1999 ◽

Vol 190 ◽

pp. 549-554

Author(s):

Nino Panagia

Keyword(s):

Angular Size ◽

Large Magellanic Cloud ◽

Magellanic Cloud ◽

Light Curves ◽

Distance Modulus ◽

Absolute Size ◽

Sn 1987A

Using the new reductions of the IUE light curves by Sonneborn et al. (1997) and an extensive set of HST images of SN 1987A we have repeated and improved Panagia et al. (1991) analysis to obtain a better determination of the distance to the supernova. In this way we have derived an absolute size of the ringRabs= (6.23 ± 0.08) x 1017cm and an angular sizeR″ = 808 ± 17 mas, which give a distance to the supernovad(SN1987A) = 51.4 ± 1.2 kpc and a distance modulusm–M(SN1987A) = 18.55 ± 0.05. Allowing for a displacement of SN 1987A position relative to the LMC center, the distance to the barycenter of the Large Magellanic Cloud is also estimated to bed(LMC) = 52.0±1.3 kpc, which corresponds to a distance modulus ofm–M(LMC) = 18.58±0.05.

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