Magnetic Fields in Supernova Remnants

Dickel, John R.; Milne, D. K.

doi:10.1071/ph760435

Cited by 69 publications

(78 citation statements)

References 1 publication

(2 reference statements)

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“…1) shows a similar dipole-shaped magnetic field configuration as earlier noted by Kundu & Velusamy (1969) and Dickel & Milne (1976). The radial configuration of the magnetic fields observed at λ6 cm seems to be intrinsic.…”

Section: G1891+30 (Ic 443)supporting

confidence: 62%

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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Context.Observations of large supernova remnants (SNRs) at high frequencies are rare, but provide valuable information about their physical properties. Aims. The total intensity and polarization properties of 16 large SNRs in the Galactic plane are investigated based on observations of the Urumqi λ6 cm polarization survey of the Galactic plane with an angular resolution of 9. 5. Methods. We extracted total intensity and linear polarization maps of large SNRs from the Urumqi λ6 cm survey, obtained their integrated flux densities, and derived the radio spectra by using these flux densities together with previously published flux densities at various frequencies. In particular, Effelsberg λ11 cm and λ21 cm survey data were used to calculate integrated flux densities. The λ6 cm polarization data also delineate the magnetic field structures of the SNRs. Results. We present the first total intensity maps at λ6 cm for SNRs G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06) and the first polarization measurements at λ6 cm for SNRs G82.2+5.3 (W63), G106.3+2.7, G114.3+0.3, G116.5+1.1, G166.0+4.3 (VRO 42.05.01), G205.5+0.5 (Monoceros Nebula), and G206.9+2.3 (PKS 0646+06). Most of the newly derived integrated radio spectra are consistent with previous results. The new flux densities obtained from the Urumqi λ6 cm, Effelsberg λ11 cm and λ21 cm surveys are crucial to determine the spectra of SNR G65.1+0.6, G69.0+2.7 (CTB 80), G93.7−0.2, and G114.3+0.3. We find that G192.8−1.1 (PKS 0607+17) consists of background sources, H ii regions, and extended diffuse emission of thermal nature, and conclude that G192.8−1.1 is not a SNR.

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Section: G1891+30 (Ic 443)supporting

confidence: 62%

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Gao

Han

Reich

et al. 2011

A&A

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“…There are observational evidences (Dickel & Milne 1976;Dubner & Giacani 2015) that patterns of polarization maps of the young SNRs demonstrate predominantly radial orientation of the projected MF directions while maps of the older SNRs have mostly tangential orientation. Our simulations suggest that, in order to restore this effect numerically, the model has to go beyond the 'point-explosion' approach and beyond the adiabatic stage, in order to treat the ejecta-ISM interactions in the young SNRs and the influence of the radiative losses of the shocked plasma on the magnetic field.…”

Section: Discussionmentioning

confidence: 99%

“…Orlando et al 2012) are not accounted for; ii) the radiative losses of the shocked plasma (efficient after the Sedov stage) increase the tangential component of MF in old SNRs . Future simulations have to be extended to the SNR ages be- fore and after the adiabatic phase in order to reconsider the idea of Dickel & Milne (1976) which seems to be confirmed by recent observations (Dubner & Giacani 2015).…”

Section: Models With the Partially Disordered Magnetic Fieldmentioning

confidence: 99%

“…The larger the parameter βn the stronger the effect of the internal Faraday rotation. Dickel & Milne (1976) have suggested that a change of the 'inferred MF' directions from the radial to the mostly tangential one could be the evolutional trend from young Π and Πmax are respectively: 0.488, 0.602, 0.691 (a), 0.007, 0.428, 0.642 (b), 0.001, 0.331, 0.579 (c), 0.000, 0.187, 0.317 (d).…”

Section: Models With the Partially Disordered Magnetic Fieldmentioning

confidence: 99%

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

Petruk

Bandiera

Beshley

et al. 2017

Monthly Notices of the Royal Astronomical Society

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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, 3-dimensional structure of a SNR has been computed, by modeling 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, 2-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.

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“…It is known that observations of polarized radio synchrotron emissions from some young supernova remnants (SNRs) show radially oriented distributions of magnetic field [3][4][5]13]. If we suppose isotropic turbulence, which is often assumed, the synchrotron emissions are unpolarized due to isotropic distribution of the magnetic field.…”

Section: Introductionmentioning

confidence: 99%

Synthetic Observation of Turbulent Supernova Remnants

Shimoda¹,

Inoue

Ohira³

et al. 2014

Proceedings of the 12th Asia Pacific Physics Conference (APPC12)

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It is known that observations of polarized radio synchrotron emissions from young supernova remnants show radially oriented distributions of magnetic field. By using synthetic polarization observations of the results of three-dimensional magnetohydrodynamics simulations, we find that the radially oriented distribution of magnetic field can be reproduced by turbulent dynamo mechanism induced by the Richtmyer-Meshkov instability. In the simulation, we consider propagation of a supernova blast wave shock in realistic inhomogeneous interstellar medium. Interaction between the density inhomogeneity and the shock wave induces the so-called Richtmyer-Meshkov instability that generates shear of radial-component velocity in the downstream of the blast wave. In such medium, magnetic field lines are stretched by the shear motion that leads to amplification of radial-component magnetic field. Thus, the downstream magnetic field is oriented parallel to the shock normal. We conclude that the observed polarized synchrotron emission is successfully explained by the dynamo effect induced by the Richtmyer-Meshkov instability.

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Magnetic Fields in Supernova Remnants

Abstract: Parkes 2·7 and 5·0 GHz polarization maps have been combined to obtain distributions of magnetic field, Faraday rotation and depolarization for 20 supernova remnants.

Cited by 69 publications

References 1 publication

A Sino-Germanλ6 cm polarization survey of the Galactic plane

A Sino-Germanλ6 cm polarization survey of the Galactic plane

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

Synthetic Observation of Turbulent Supernova Remnants

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