Multi-dimensional simulations of the expanding supernova remnant of SN 1987A

Abstract

The expanding remnant from SN 1987A is an excellent laboratory for investigating the physics of supernovae explosions. There are still a large number of outstanding questions, such the reason for the asymmetric radio morphology, the structure of the pre-supernova environment, and the efficiency of particle acceleration at the supernova shock. We explore these questions using three-dimensional simulations of the expanding remnant between days 820 and 10,000 after the supernova. We combine a hydrodynamical simulation with semi-analytic treatments of diffusive shock acceleration and magnetic field amplification to derive radio emission as part of an inverse problem. Simulations show that an asymmetric explosion, combined with magnetic field amplification at the expanding shock, is able to replicate the persistent one-sided radio morphology of the remnant. We use an asymmetric Truelove & McKee progenitor with an envelope mass of $10 M_{\sun}$ and an energy of $1.5\times 10^{44}J$. A termination shock in the progenitor's stellar wind at a distance of $0\farcs43-0\farcs51$ provides a good fit to the turn on of radio emission around day 1200. For the H\textsc{ii} region, a minimum distance of $0\farcs63\pm0\farcs01$ and maximum particle number density of $(7.11\pm 1.78)\times 10^7$ m${}^{-3}$ produces a good fit to the evolving average radius and velocity of the expanding shocks from day 2000 to day 7000 after explosion. The model predicts a noticeable reduction, and possibly a temporary reversal, in the asymmetric radio morphology of the remnant after day 7000, when the forward shock left the eastern lobe of the equatorial ring.

31 pages, 19 figures

References in corpus (9)

• Interactions of a Light Hypersonic Jet with a Non-Uniform Interstellar Medium
• High-resolution radio observations of SNR 1987A at high frequencies
• Fourier Modeling of the Radio Torus Surrounding Supernova 1987A
• Cosmic ray acceleration at perpendicular shocks in supernova remnants
• Expected gamma-ray emission of supernova remnant SN 1987A
• Magnetic field in supernova remnant SN 1987A
• Reverse and Forward Shock X-ray Emission in an Evolutionary Model of Supernova Remnants undergoing Efficient Diffusive Shock Acceleration
• Fifteen Years of High-Resolution Radio Imaging of Supernova 1987A
• SN Shock Evolution in the Circumstellar Medium surrounding SN 1987A

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• Reverberation of pulsar wind nebulae (II): Anatomy of the "thin-shell'' evolution
• Sensitivity of the Cherenkov Telescope Array to TeV photon emission from the Large Magellanic Cloud
• Latest Evolution of the X-Ray Remnant of SN 1987A: Beyond the Inner Ring
• Revisiting the evolution of nonradiative supernova remnants: A hydrodynamical-informed parameterization of the shock positions
• First 3D Morpho-Kinematic model of Supernova Remnants. The case of VRO 42.05.01 (G 166.0+4.3)
• How do supernova remnants cool? -- I. Morphology, optical emission lines, and shocks
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• Polarized radio emission unveils the structure of the pre-supernova circumstellar magnetic field and the radio emission in SN1987A
• Linking gamma-ray spectra of supernova remnants to the cosmic ray injection properties in the aftermath of supernovae
• The Radio Remnant of Supernova 1987A - A Broader View
• The Bright Supernova 1996cr in the Circinus Galaxy Imaged with VLBI: Shell Structure with Complex Evolution