Aspect angle for interstellar magnetic field in SN 1006

Petruk, O.; Dubner, G.; Castelletti, G.; Bocchino, F.; Iakubovskyi, Dmytro; Kirsch, Marcus; Miceli, M.; Orlando, S.; Telezhinsky, I.

doi:10.1111/j.1365-2966.2008.14251.x

Cited by 44 publications

(90 citation statements)

References 14 publications

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“…A strong axisymmetric background ISM magnetic field (not included in our simulations) has also been suggested to be responsible for the bilateral character of some Galactic supernova remnants (Gaensler 1998). It would indeed make their shape more elongated as long as the field is strong enough (Rozyczka & Tenorio-Tagle 1995) and produce X-ray and/or radio synchrotron emission from the opposed arcs (Velázquez et al 2004;Petruk et al 2009;Schneiter et al 2010).…”

Section: Bilateral Supernova Remnantsmentioning

confidence: 99%

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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After the death of a runaway massive star, its supernova shock wave interacts with the bow shocks produced by its defunct progenitor, and may lose energy, momentum, and its spherical symmetry before expanding into the local interstellar medium (ISM). We investigate whether the initial mass and space velocity of these progenitors can be associated with asymmetric supernova remnants. We run hydrodynamical models of supernovae exploding in the pre-shaped medium of moving Galactic core-collapse progenitors. We find that bow shocks that accumulate more than about 1.5 M ⊙ generate asymmetric remnants. The shock wave first collides with these bow shocks 160 − 750 yr after the supernova, and the collision lasts until 830 − 4900 yr. The shock wave is then located 1.35 − 5 pc from the center of the explosion, and it expands freely into the ISM, whereas in the opposite direction it is channelled into the region of undisturbed wind material. This applies to an initially 20 M ⊙ progenitor moving with velocity 20 km s −1 and to our initially 40 M ⊙ progenitor. These remnants generate mixing of ISM gas, stellar wind and supernova ejecta that is particularly important upstream from the center of the explosion. Their lightcurves are dominated by emission from optically-thin cooling and by X-ray emission of the shocked ISM gas. We find that these remnants are likely to be observed in the [OIII] λ 5007 spectral line emission or in the soft energy-band of X-rays. Finally, we discuss our results in the context of observed Galactic supernova remnants such as 3C391 and the Cygnus Loop.

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Section: Bilateral Supernova Remnantsmentioning

confidence: 99%

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Meyer¹,

Langer²,

Mackey³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…Recently, Petruk et al (2009b) have further investigated this problem, and showed that in the framework of a simple model of SN1006 in terms of a point-like explosion occurring in a uniform density and uniform magnetic field medium, there is no way to reconcile the quasi-parallel scenario and the SN1006 morphology as observed in the radio band. The same conclusion was reached more recently by Schneiter et al (2010).…”

Section: Introductionmentioning

confidence: 99%

Constraints on the local interstellar magnetic field from non-thermal emission of SN1006

Bocchino

Orlando²,

Miceli³

et al. 2011

A&A

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Context. The synchrotron radio morphology of bilateral supernova remnants depends on the mechanisms of particle acceleration and on the viewing geometry. However, unlike X-ray and γ-ray morphologies, the radio emission does not depend on the cut-off region of the parent electron population, making it a simpler and more straightforward tool to investigate the physics of cosmic ray production in supernova remnants (SNRs). Aims. We will use the radio morphology to derive tight constraints on the direction of the local magnetic field and its gradient, and on the obliquity dependence of the electron injection efficiency. Methods. We perform a set of 3D MHD simulations describing the expansion of a spherical SNR through a magnetized medium with a non-uniform magnetic field. From the simulations, we derive non-thermal radio maps and compare them with observations of the SN1006 remnant. Results. We find that the radio morphology of SN1006 at 1 GHz is best-fitted by a model with quasi-parallel injection efficiency, a magnetic field aspect angle of 38 • ± 4 • with the line of sight, and a gradient of the field strength toward the galactic plane, higher then the expected variations of the large scale field of the Galaxy. Conclusions. We conclude that the radio limbs of SN1006 are polar caps that do not lie in the plane of sky. The study of the synchrotron radio emission of SNRs is of crucial importance to derive information on the galactic magnetic field in the vicinity of the remnants, and to gather more hints on the actual injection efficiency scenario.

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“…The presence (or absence) of the Xray emission in the precursor gives hints on the particle acceleration properties (Long et al 2003;Morlino et al 2010;Winkler et al 2014). The azimuthal variation of the radio brightness depends on the obliquity dependence of the injection efficiency (Fulbright & Reynolds 1990;Petruk et al 2009a) while the X-ray azimuthal profile might help in determining whether the maximum particle momentum is timeor loss-limited (Petruk et al 2011a). High spatial resolution observations may reveal the distance between the shock and the contact discontinuity (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…In particular, they allow for determination of the 3-dimensional orientation of ISMF and even its gradient around SN 1006 (Petruk et al 2009a;Bocchino et al 2011) or, by analyzing a sample of SNRs, to reveal properties of the Galactic MF (West et al 2016). By modeling the surface brightness maps, it was shown that a certain class of SNRs, namely the thermal X-ray composites (or mixed-morphology SNRs, i.e.…”

Section: Introductionmentioning

confidence: 99%

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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Aspect angle for interstellar magnetic field in SN 1006

Cited by 44 publications

References 14 publications

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Asymmetric supernova remnants generated by Galactic, massive runaway stars

Constraints on the local interstellar magnetic field from non-thermal emission of SN1006

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

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