Interaction of Supernova Ejecta with Circumstellar Matter and X-Ray Emission: SN 1987A & SN 1993J

The X-ray spectrum observed by Ginga is characterized by a component below 10keV which decreases with increasing photon energy, and a component above 10keV which is nearly flat. This unusual X-ray spectrum may be understood as follows; X-rays below 10keV is likely to be due to thermal emission coming from the shock-heated ejecta, and X-rays above 10keV to be due to γ-ray degradation inside the ejecta. If thermal emission due to the collision of the ejecta with circumstellar matter (CSM) is responsible for X-rays below 10keV, the epoch of the collision can be estimated to be ∼ 0.2yr after the explosion if ∼ 0.5yr is the time when the X-ray flux at ∼ 10keV reaches its maximum. The X-ray light curve then requires the inner radius of CSM to be ∼ 1×1016cm for an expansion velocity, Vex ≃2×109cm s−1.

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Interaction of supernova ejecta with circumstellar matter and X-ray emission: SN 1987A & SN 1993J

International Astronomical Union Colloquium ◽

10.1017/s0252921100008162 ◽

1996 ◽

Vol 145 ◽

pp. 317-322

Author(s):

T. Suzuki ◽

K. Nomoto ◽

T. Shigeyama ◽

S. Kumagai

Keyword(s):

Circumstellar Matter ◽

Light Curves ◽

X Rays ◽

X Ray ◽

Sn 1987A

We perform hydrodynamical calculations of the collision between the supernova ejecta and circumstellar matter for SN 1987A and SN 1993J. For SN 1987A we predict light curves of X-ray emissions from the shocked ring. For SN 1993J, thermal X-rays from the shocked circumstellar matter can consistently account for the observations with ROSAT, ASCA, and OSSE.

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X-rays and γ-rays from Supernova 1987a

International Astronomical Union Colloquium ◽

10.1017/s0252921100094148 ◽

1988 ◽

Vol 108 ◽

pp. 394-398

Author(s):

P. Sutherland ◽

Y. Xu ◽

R. McCray ◽

R. Ross

Keyword(s):

Circumstellar Matter ◽

Radioactive Material ◽

Strong Line ◽

X Rays ◽

X Ray ◽

Monte Carlo Calculations ◽

Sn 1987A ◽

Unique Event ◽

Supernova 1987A ◽

Γ Rays

SummaryThe observation of X-rays and γ-rays from SN 1987a can provide important constraints on parameters for models of this unique event. We present the results of detailed Monte Carlo calculations of the fluxes to be expected in several X-ray bands and for the strong line at 847 keV associated with the decay of 56Co. Our calculations use Model 10H of Woosley, Pinto, and Ensman(1988), with 0.075M⊙ of radioactive material. If it is assumed that there is no mixing of this material with the layers above, then the X-ray fluxes do not become detectable as early as the observations made by the Ginga team in August, 1987. If these observations correspond to X-rays arising from γ-rays Compton scattered down in energy in the supernova ejecta, rather than the interaction of the ejecta with circumstellar matter, then they can only be explained by mixing outward of radioactive material or an envelope with some combination of less mass or greater kinetic energy per unit mass.

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X-Ray Observation of SN 1987A from GINGA

Supernovae ◽

10.1007/978-1-4612-2988-9_37 ◽

1991 ◽

pp. 269-277 ◽

Cited By ~ 2

Author(s):

Yasuo Tanaka

Keyword(s):

X Ray ◽

Sn 1987A

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Supernovae and the Cosmic Distance Scale

International Astronomical Union Colloquium ◽

10.1017/s0252921100007879 ◽

1996 ◽

Vol 145 ◽

pp. 19-28

Author(s):

Robert P. Kirshner

Keyword(s):

Absolute Magnitude ◽

Circumstellar Matter ◽

Large Magellanic Cloud ◽

Distance Scale ◽

Sn 1987A ◽

Apparent Homogeneity ◽

Independent Test ◽

Age Of The Universe ◽

The Universe ◽

Geometric Measurement

Knowledge of the size and age of the Universe depends on understanding supernovae. The direct geometric measurement of the circumstellar ring of SN 1987A using IUE spectra and HST images provides an independent test of the Cepheid distance scale to the Large Magellanic Cloud. Understanding the details of the mass distribution in the circumstellar matter is important to improving the precision of this distance. Type la supernovae have a narrow distribution in absolute magnitude, and new Cepheid distances to IC 4182 (the site of SN 1937C) and to NGC 5253 (the site of SN 1972E) obtained with HST by Sandage and his collaborators allow that absolute magnitude to be calibrated. Comparison with more distant SNIa gives H0 = 56 ± 8 km s-1 Mpc-1. Recent work in supernova spectroscopy and photometry shows that the apparent homogeneity of SNIa is not quite what it seems, and a deeper understanding of these variations is needed to use the SNIa to best advantage. The Expanding Photosphere Method (EPM) allows direct measurement to each Type II supernova that has adequate photometry and spectroscopy. There are now 18 such objects. The sample of EPM distances from 4.5 Mpc to 180 Mpc indicates H0 = 73±6 (statistical) ±7 (systematic) km s-1 Mpc-1. Better understanding of supernova atmospheres can reduce the systematic error in this approach, which is completely independent of all other astronomical distances.

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X-ray enhancement of SN 1987A due to interaction with its ringlike nebula

The Astrophysical Journal ◽

10.1086/173940 ◽

1994 ◽

Vol 424 ◽

pp. 924 ◽

Cited By ~ 13

Author(s):

Kuniaki Masai ◽

Ken'ichi Nomoto

Keyword(s):

X Ray ◽

Sn 1987A

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The effects of mixing of the ejecta on the hard X-ray emissions from SN 1987A

The Astrophysical Journal ◽

10.1086/185128 ◽

1988 ◽

Vol 327 ◽

pp. L5 ◽

Cited By ~ 29

Author(s):

Toshikazu Ebisuzaki ◽

Noriaki Shibazaki

Keyword(s):

X Ray ◽

Sn 1987A

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Monitoring the Evolution of the X‐Ray Remnant of SN 1987A

The Astrophysical Journal ◽

10.1086/338492 ◽

2002 ◽

Vol 567 (1) ◽

pp. 314-322 ◽

Cited By ~ 53

Author(s):

Sangwook Park ◽

David N. Burrows ◽

Gordon P. Garmire ◽

John A. Nousek ◽

Richard McCray ◽

...

Keyword(s):

X Ray ◽

Sn 1987A

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Non-Equilibrium Thermal X-Ray Emission in the Early Phase of Supernova Remnant

Highlights of Astronomy ◽

10.1017/s1539299600007814 ◽

1989 ◽

Vol 8 ◽

pp. 217-221

Author(s):

Hitoshi Hanami ◽

Tatsuo Yoshida

Keyword(s):

Early Phase ◽

Supernova Remnant ◽

Circumstellar Matter ◽

Temperature Model ◽

X Ray ◽

Two Temperature ◽

Non Equilibrium

AbstractThe X-ray emission from the interaction of the ejecta with circumstellar matter (CSM) for SN1987A is investigated. The electron and the ion temperatures seem to be in non-equilibrium in the early phase of a SN remnant. We have studied the two-temperature model in the early phase of SNR and discuss the X-ray emission from SN1987A and its CSM.

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Radio and X-ray Emission from Newly Born Remnants

Symposium - International Astronomical Union ◽

10.1017/s0074180900033854 ◽

1983 ◽

Vol 101 ◽

pp. 177-182

Author(s):

Marco Salvati

Keyword(s):

Circumstellar Matter ◽

Light Curves ◽

X Ray

Radio and X-ray observations of SN 1979c and SN 1980k offer a unique opportunity of monitoring the transition from supernovae to remnants. By means of the two-frequency radio light curves, we test the hypothesis that these objects are surrounded by circumstellar matter, originated in a pre supernova wind, and derive the relevant parameters. Then we use the absorption-corrected light curves to test the various proposed models. SN 1980 k appears to be powered by a canonical shock, while SN 1979c is a good plerion candidate. An optical pulsar could still be detected at its location.

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