Radio polarization maps of shell-type SNRs - II. Sedov models with evolution of turbulent magnetic field

Marco Miceli, Petruk, Beshley, Bandiera, Orlando, Miceli

Research output: Contribution to journalArticle

2 Citations (Scopus)

Abstract

Polarized radio emission has been mapped with great detail in several Galactic supernova remnants (SNRs), but has not yet been exploited to the extent it deserves. We have developed a method to model maps of the Stokes parameters for shell-like SNRs during their Sedov evolution phase. At first, three-dimensional structure of an SNR has been computed, by modelling the distribution of the magnetohydrodynamic parameters and of the accelerated particles. The generation and dissipation of the turbulent component of magnetic field everywhere in SNR are also considered taking into account its interaction with accelerated particles. Then, in order to model the emission, we have used a generalization of the classical synchrotron theory, valid for the case in which the magnetic field has ordered and disordered components. Finally, two-dimensional projected maps have been derived, for different orientations of SNR and of interstellar magnetic field with respect to the observer. An important effect to consider is the Faraday rotation of the polarization planes inside the SNR interior. In this paper, we present details of the model, and describe general properties of the images.
Original languageEnglish
Pages (from-to)1156-1176
Number of pages21
JournalMonthly Notices of the Royal Astronomical Society
Volume470
Publication statusPublished - 2017

Fingerprint

supernova remnants
polarization
shell
radio
magnetic field
magnetic fields
general property
magnetohydrodynamics
dissipation
interstellar magnetic fields
radio emission
Faraday effect
modeling
synchrotrons
parameter
particle
interactions

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Radio polarization maps of shell-type SNRs - II. Sedov models with evolution of turbulent magnetic field. / Miceli, Marco; Petruk; Beshley; Bandiera; Orlando; Miceli.

In: Monthly Notices of the Royal Astronomical Society, Vol. 470, 2017, p. 1156-1176.

Research output: Contribution to journalArticle

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title = "Radio polarization maps of shell-type SNRs - II. Sedov models with evolution of turbulent magnetic field",
abstract = "Polarized radio emission has been mapped with great detail in several Galactic supernova remnants (SNRs), but has not yet been exploited to the extent it deserves. We have developed a method to model maps of the Stokes parameters for shell-like SNRs during their Sedov evolution phase. At first, three-dimensional structure of an SNR has been computed, by modelling the distribution of the magnetohydrodynamic parameters and of the accelerated particles. The generation and dissipation of the turbulent component of magnetic field everywhere in SNR are also considered taking into account its interaction with accelerated particles. Then, in order to model the emission, we have used a generalization of the classical synchrotron theory, valid for the case in which the magnetic field has ordered and disordered components. Finally, two-dimensional projected maps have been derived, for different orientations of SNR and of interstellar magnetic field with respect to the observer. An important effect to consider is the Faraday rotation of the polarization planes inside the SNR interior. In this paper, we present details of the model, and describe general properties of the images.",
keywords = "Acceleration of particles, Astronomy and Astrophysics, Cosmic rays, ISM: supernova remnants, Radiation mechanisms: non-thermal, Shock waves, Space and Planetary Science",
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T1 - Radio polarization maps of shell-type SNRs - II. Sedov models with evolution of turbulent magnetic field

AU - Miceli, Marco

AU - Petruk, null

AU - Beshley, null

AU - Bandiera, null

AU - Orlando, null

AU - Miceli, null

PY - 2017

Y1 - 2017

N2 - Polarized radio emission has been mapped with great detail in several Galactic supernova remnants (SNRs), but has not yet been exploited to the extent it deserves. We have developed a method to model maps of the Stokes parameters for shell-like SNRs during their Sedov evolution phase. At first, three-dimensional structure of an SNR has been computed, by modelling the distribution of the magnetohydrodynamic parameters and of the accelerated particles. The generation and dissipation of the turbulent component of magnetic field everywhere in SNR are also considered taking into account its interaction with accelerated particles. Then, in order to model the emission, we have used a generalization of the classical synchrotron theory, valid for the case in which the magnetic field has ordered and disordered components. Finally, two-dimensional projected maps have been derived, for different orientations of SNR and of interstellar magnetic field with respect to the observer. An important effect to consider is the Faraday rotation of the polarization planes inside the SNR interior. In this paper, we present details of the model, and describe general properties of the images.

AB - Polarized radio emission has been mapped with great detail in several Galactic supernova remnants (SNRs), but has not yet been exploited to the extent it deserves. We have developed a method to model maps of the Stokes parameters for shell-like SNRs during their Sedov evolution phase. At first, three-dimensional structure of an SNR has been computed, by modelling the distribution of the magnetohydrodynamic parameters and of the accelerated particles. The generation and dissipation of the turbulent component of magnetic field everywhere in SNR are also considered taking into account its interaction with accelerated particles. Then, in order to model the emission, we have used a generalization of the classical synchrotron theory, valid for the case in which the magnetic field has ordered and disordered components. Finally, two-dimensional projected maps have been derived, for different orientations of SNR and of interstellar magnetic field with respect to the observer. An important effect to consider is the Faraday rotation of the polarization planes inside the SNR interior. In this paper, we present details of the model, and describe general properties of the images.

KW - Acceleration of particles

KW - Astronomy and Astrophysics

KW - Cosmic rays

KW - ISM: supernova remnants

KW - Radiation mechanisms: non-thermal

KW - Shock waves

KW - Space and Planetary Science

UR - http://hdl.handle.net/10447/342219

UR - http://mnras.oxfordjournals.org/

M3 - Article

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SP - 1156

EP - 1176

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

ER -