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

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2 Citazioni (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.
Lingua originaleEnglish
pagine (da-a)1156-1176
Numero di pagine21
RivistaMonthly Notices of the Royal Astronomical Society
Volume470
Stato di pubblicazionePublished - 2017

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cita questo

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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; Cosmic rays; ISM: supernova remnants; Radiation mechanisms: non-thermal; Shock waves; Astronomy and Astrophysics; Space and Planetary Science",
author = "Marco Miceli",
year = "2017",
language = "English",
volume = "470",
pages = "1156--1176",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",

}

TY - JOUR

T1 - Radio polarization maps of shell-type SNRs - II. Sedov models with evolution of turbulent magnetic field

AU - Miceli, Marco

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; Cosmic rays; ISM: supernova remnants; Radiation mechanisms: non-thermal; Shock waves; Astronomy and Astrophysics; Space and Planetary Science

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

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

M3 - Article

VL - 470

SP - 1156

EP - 1176

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

ER -