3D MHD modeling of the expanding remnant of SN 1987A: Role of magnetic field and non-thermal radio emission ?

Marco Miceli, Giovanni Peres, Petruk, Guarrasi, Lee, Nagataki, Bocchino, Aloy, Orlando, Giovanni Peres, Ono, Mimica, Miceli, Massimiliano Guarrasi

Risultato della ricerca: Article

Abstract

Aims. We investigate the role played by a pre-supernova (SN) ambient magnetic field in the dynamics of the expanding remnant of SN 1987A, and the origin and evolution of the radio emission from the remnant, in particular during the interaction of the blast wave with the nebula surrounding the SN. Methods. We modeled the evolution of SN 1987A from the breakout of the shock wave at the stellar surface to the expansion of its remnant through the surrounding nebula using three-dimensional magnetohydrodynamic simulations. The model considers the radiative cooling, the deviations from equilibrium of ionization, the deviation from temperature-equilibration between electrons and ions, and a plausible configuration of the pre-SN ambient magnetic field. We explore the strengths of the pre-SN magnetic field ranging between 1 and 100 μG at the inner edge of the nebula and we assume an average field strength at the stellar surface B0 3 kG. From the simulations, we synthesize the thermal X-ray and the non-thermal radio emission and compare the model results with observations. Results. The presence of an ambient magnetic field with strength in the range considered does not change significantly the overall evolution of the remnant. Nevertheless, the magnetic field reduces the erosion and fragmentation of the dense equatorial ring after the impact of the SN blast wave. As a result, the ring survives the passage of the blast, at least during the time covered by the simulations (40 yr). Our model is able to reproduce the morphology and lightcurves of SN 1987A in both X-ray and radio bands. The model reproduces the observed radio emission if the flux originating from the reverse shock is heavily suppressed. In this case, the radio emission originates mostly from the forward shock traveling through the H II region and this may explain why the radio emission seems to be insensitive to the interaction of the blast with the ring. Possible mechanisms for the suppression of emission from the reverse shock are investigated. We find that synchrotron self-absorption and free-free absorption have negligible effects on the emission during the interaction with the nebula. We suggest that the emission from the reverse shock at radio frequencies might be limited by highly magnetized ejecta.
Lingua originaleEnglish
pagine (da-a)A73-
Numero di pagine15
RivistaASTRONOMY & ASTROPHYSICS
Volume622
Stato di pubblicazionePublished - 2019

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supernova 1987A
radio emission
supernovae
blasts
nebulae
radio
magnetic field
shock
magnetic fields
modeling
rings
deviation
magnetohydrodynamic simulation
self absorption
H II regions
interactions
ejecta
erosion
shock waves
field strength

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cita questo

3D MHD modeling of the expanding remnant of SN 1987A: Role of magnetic field and non-thermal radio emission ? / Miceli, Marco; Peres, Giovanni; Petruk; Guarrasi; Lee; Nagataki; Bocchino; Aloy; Orlando; Peres, Giovanni; Ono; Mimica; Miceli; Guarrasi, Massimiliano.

In: ASTRONOMY & ASTROPHYSICS, Vol. 622, 2019, pag. A73-.

Risultato della ricerca: Article

Miceli, M, Peres, G, Petruk, Guarrasi, Lee, Nagataki, Bocchino, Aloy, Orlando, Peres, G, Ono, Mimica, Miceli & Guarrasi, M 2019, '3D MHD modeling of the expanding remnant of SN 1987A: Role of magnetic field and non-thermal radio emission ?', ASTRONOMY & ASTROPHYSICS, vol. 622, pagg. A73-.
Miceli, Marco ; Peres, Giovanni ; Petruk ; Guarrasi ; Lee ; Nagataki ; Bocchino ; Aloy ; Orlando ; Peres, Giovanni ; Ono ; Mimica ; Miceli ; Guarrasi, Massimiliano. / 3D MHD modeling of the expanding remnant of SN 1987A: Role of magnetic field and non-thermal radio emission ?. In: ASTRONOMY & ASTROPHYSICS. 2019 ; Vol. 622. pagg. A73-.
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title = "3D MHD modeling of the expanding remnant of SN 1987A: Role of magnetic field and non-thermal radio emission ?",
abstract = "Aims. We investigate the role played by a pre-supernova (SN) ambient magnetic field in the dynamics of the expanding remnant of SN 1987A, and the origin and evolution of the radio emission from the remnant, in particular during the interaction of the blast wave with the nebula surrounding the SN. Methods. We modeled the evolution of SN 1987A from the breakout of the shock wave at the stellar surface to the expansion of its remnant through the surrounding nebula using three-dimensional magnetohydrodynamic simulations. The model considers the radiative cooling, the deviations from equilibrium of ionization, the deviation from temperature-equilibration between electrons and ions, and a plausible configuration of the pre-SN ambient magnetic field. We explore the strengths of the pre-SN magnetic field ranging between 1 and 100 μG at the inner edge of the nebula and we assume an average field strength at the stellar surface B0 3 kG. From the simulations, we synthesize the thermal X-ray and the non-thermal radio emission and compare the model results with observations. Results. The presence of an ambient magnetic field with strength in the range considered does not change significantly the overall evolution of the remnant. Nevertheless, the magnetic field reduces the erosion and fragmentation of the dense equatorial ring after the impact of the SN blast wave. As a result, the ring survives the passage of the blast, at least during the time covered by the simulations (40 yr). Our model is able to reproduce the morphology and lightcurves of SN 1987A in both X-ray and radio bands. The model reproduces the observed radio emission if the flux originating from the reverse shock is heavily suppressed. In this case, the radio emission originates mostly from the forward shock traveling through the H II region and this may explain why the radio emission seems to be insensitive to the interaction of the blast with the ring. Possible mechanisms for the suppression of emission from the reverse shock are investigated. We find that synchrotron self-absorption and free-free absorption have negligible effects on the emission during the interaction with the nebula. We suggest that the emission from the reverse shock at radio frequencies might be limited by highly magnetized ejecta.",
keywords = "Astronomy and Astrophysics, ISM: supernova remnants, Magnetohydrodynamics (MHD), Space and Planetary Science, X-rays: ISM, radio continuum: ISM, shock waves, supernovae: individual: SN 1987A",
author = "Marco Miceli and Giovanni Peres and Petruk and Guarrasi and Lee and Nagataki and Bocchino and Aloy and Orlando and Giovanni Peres and Ono and Mimica and Miceli and Massimiliano Guarrasi",
year = "2019",
language = "English",
volume = "622",
pages = "A73--",
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}

TY - JOUR

T1 - 3D MHD modeling of the expanding remnant of SN 1987A: Role of magnetic field and non-thermal radio emission ?

AU - Miceli, Marco

AU - Peres, Giovanni

AU - Petruk, null

AU - Guarrasi, null

AU - Lee, null

AU - Nagataki, null

AU - Bocchino, null

AU - Aloy, null

AU - Orlando, null

AU - Peres, Giovanni

AU - Ono, null

AU - Mimica, null

AU - Miceli, null

AU - Guarrasi, Massimiliano

PY - 2019

Y1 - 2019

N2 - Aims. We investigate the role played by a pre-supernova (SN) ambient magnetic field in the dynamics of the expanding remnant of SN 1987A, and the origin and evolution of the radio emission from the remnant, in particular during the interaction of the blast wave with the nebula surrounding the SN. Methods. We modeled the evolution of SN 1987A from the breakout of the shock wave at the stellar surface to the expansion of its remnant through the surrounding nebula using three-dimensional magnetohydrodynamic simulations. The model considers the radiative cooling, the deviations from equilibrium of ionization, the deviation from temperature-equilibration between electrons and ions, and a plausible configuration of the pre-SN ambient magnetic field. We explore the strengths of the pre-SN magnetic field ranging between 1 and 100 μG at the inner edge of the nebula and we assume an average field strength at the stellar surface B0 3 kG. From the simulations, we synthesize the thermal X-ray and the non-thermal radio emission and compare the model results with observations. Results. The presence of an ambient magnetic field with strength in the range considered does not change significantly the overall evolution of the remnant. Nevertheless, the magnetic field reduces the erosion and fragmentation of the dense equatorial ring after the impact of the SN blast wave. As a result, the ring survives the passage of the blast, at least during the time covered by the simulations (40 yr). Our model is able to reproduce the morphology and lightcurves of SN 1987A in both X-ray and radio bands. The model reproduces the observed radio emission if the flux originating from the reverse shock is heavily suppressed. In this case, the radio emission originates mostly from the forward shock traveling through the H II region and this may explain why the radio emission seems to be insensitive to the interaction of the blast with the ring. Possible mechanisms for the suppression of emission from the reverse shock are investigated. We find that synchrotron self-absorption and free-free absorption have negligible effects on the emission during the interaction with the nebula. We suggest that the emission from the reverse shock at radio frequencies might be limited by highly magnetized ejecta.

AB - Aims. We investigate the role played by a pre-supernova (SN) ambient magnetic field in the dynamics of the expanding remnant of SN 1987A, and the origin and evolution of the radio emission from the remnant, in particular during the interaction of the blast wave with the nebula surrounding the SN. Methods. We modeled the evolution of SN 1987A from the breakout of the shock wave at the stellar surface to the expansion of its remnant through the surrounding nebula using three-dimensional magnetohydrodynamic simulations. The model considers the radiative cooling, the deviations from equilibrium of ionization, the deviation from temperature-equilibration between electrons and ions, and a plausible configuration of the pre-SN ambient magnetic field. We explore the strengths of the pre-SN magnetic field ranging between 1 and 100 μG at the inner edge of the nebula and we assume an average field strength at the stellar surface B0 3 kG. From the simulations, we synthesize the thermal X-ray and the non-thermal radio emission and compare the model results with observations. Results. The presence of an ambient magnetic field with strength in the range considered does not change significantly the overall evolution of the remnant. Nevertheless, the magnetic field reduces the erosion and fragmentation of the dense equatorial ring after the impact of the SN blast wave. As a result, the ring survives the passage of the blast, at least during the time covered by the simulations (40 yr). Our model is able to reproduce the morphology and lightcurves of SN 1987A in both X-ray and radio bands. The model reproduces the observed radio emission if the flux originating from the reverse shock is heavily suppressed. In this case, the radio emission originates mostly from the forward shock traveling through the H II region and this may explain why the radio emission seems to be insensitive to the interaction of the blast with the ring. Possible mechanisms for the suppression of emission from the reverse shock are investigated. We find that synchrotron self-absorption and free-free absorption have negligible effects on the emission during the interaction with the nebula. We suggest that the emission from the reverse shock at radio frequencies might be limited by highly magnetized ejecta.

KW - Astronomy and Astrophysics

KW - ISM: supernova remnants

KW - Magnetohydrodynamics (MHD)

KW - Space and Planetary Science

KW - X-rays: ISM

KW - radio continuum: ISM

KW - shock waves

KW - supernovae: individual: SN 1987A

UR - http://hdl.handle.net/10447/342837

UR - https://www.aanda.org/

M3 - Article

VL - 622

SP - A73-

JO - ASTRONOMY & ASTROPHYSICS

JF - ASTRONOMY & ASTROPHYSICS

SN - 0004-6361

ER -