Circumstellar Matter in the Accretion Model of Cosmic X-Ray Sources

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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The X-Ray Spectrum of Supernova SN1993J

Symposium - International Astronomical Union ◽

10.1017/s0074180900114950 ◽

1998 ◽

Vol 188 ◽

pp. 245-246

Author(s):

Shin'ichiro Uno ◽

Kazuhisa Mitsuda ◽

Tadayuki Takahashi ◽

Hajime Inoue ◽

Fumiyoshi Makino ◽

...

Keyword(s):

Early Detection ◽

Radio Emission ◽

Shock Front ◽

Circumstellar Matter ◽

High Density ◽

X Ray ◽

Unique Object

SN1993J is very unique object which was discovered in the nearby Sb galaxy M81 (NGC 3031) on March 28. The first detection of the radio emission was at 22.5 GHz by the VLA only 5 days after the optical outburst. Subsequently X-ray emission was detected by ROSAT and ASCA at 6 days and 8 days after the explosion respectively. These emissions are expected when the SN shock front sweeps out the circumstellar matter (CSM). The early detection of radio and X-ray emission implies the existence of high-density CSM in the vicinity of the supernova(e.g.).

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A tale of two shocks in SN 2004dj

Proceedings of the International Astronomical Union ◽

10.1017/s1743921313009319 ◽

2013 ◽

Vol 9 (S296) ◽

pp. 108-111

Author(s):

Alak Ray ◽

Sayan Chakraborti ◽

Naveen Yadav ◽

Randall Smith ◽

Poonam Chandra ◽

...

Keyword(s):

Thermal Emission ◽

Mass Loss Rate ◽

Circumstellar Matter ◽

Published Data ◽

Reverse Shock ◽

X Ray ◽

Inverse Compton Scattering ◽

Field Amplification ◽

Forward Shock ◽

Red Supergiants

AbstractType IIP SNe constitute a major fraction of all core-collapse supernovae and arise from massive stars that end their lives close to Red Supergiants. The blastwave from the SN interacting with the progenitor's circumstellar matter produces a hot region bounded by a forward and a reverse shock from which most of the X-ray emission originates. Analysis of archival Chandra observations of SN 2004dj, one of the nearest supernovae since SN 1987A, together with published data from radio and optical bands determines the pre-explosion mass-loss rate, blastwave speed, electron acceleration and magnetic field amplification efficiencies. X-ray emission arises from both inverse Compton scattering by non-thermal electrons accelerated in the forward shock and from thermal emission from the supernova ejecta hit by the reverse shock. Determination of the properties of the radiating plasma based on the separation of thermal and non-thermal radiation differentiates different types of supernovae and their environments.

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