Preface

Petruk, W.

doi:10.1016/b978-044450077-9/50000-6

Cited by 8 publications

(11 citation statements)

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“…There are known solutions of the system (1). Namely, Sedov (1959) found the analytical solutions for L = 0 and B = 0 (for approximations of the Sedov solutions see Petruk 2000). Analytical description of MF in Sedov SNRs (L = 0, B = 0) are given by Karlikov & Korobeinikov (1960); Korobeinikov (1964).…”

Section: The Code and Problem Setupmentioning

confidence: 99%

Post-adiabatic supernova remnants in an interstellar magnetic field: parallel and perpendicular shocks

Petruk¹,

Kuzyo²,

Beshley³

2015

Mon. Not. R. Astron. Soc.

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Gamma-rays from hadronic collisions are expected from supernova remnants (SNRs) located near molecular clouds. The temperature on the shock interacting with the dense environment quickly reaches 10 5 K. The radiative losses of plasma become essential in the evolution of SNRs. They decrease the thermal pressure and essentially increase the density behind the shock. The presence of ambient magnetic field may considerably alter the behavior of the post-adiabatic SNRs comparing to hydrodynamic scenario. In the present paper, the magneto-hydrodynamic simulations of radiative shocks in magnetic field are performed. High plasma compression due to the radiative losses results also in the prominent increase of the strength of the tangential component of magnetic field behind the shock and the decrease of the parallel one. If the strength of the tangential field before the shock is higher than about 3 µG it prevents formation of the very dense thin shell. The higher the strength of the tangential magnetic field the larger the thickness and the lower the maximum density in the radiative shell. Parallel magnetic field does not affect the distribution of the hydrodynamic parameters behind the shock. There are almost independent channels of energy transformations: radiative losses are due to the thermal energy, the magnetic energy increases by reducing the kinetic energy. The large density and high strength of the perpendicular magnetic field in the radiative shells of SNRs should result in considerable increase of the hadronic gamma-ray flux comparing to the leptonic one.

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Section: The Code and Problem Setupmentioning

confidence: 99%

Post-adiabatic supernova remnants in an interstellar magnetic field: parallel and perpendicular shocks

Petruk¹,

Kuzyo²,

Beshley³

2015

Mon. Not. R. Astron. Soc.

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“…Let us consider an adiabatic SNR in uniform ISM and uniform ISMF. Hydrodynamics of the remnant is given by the self-similar Sedov (1959) solutions; in practice, we use their quite accurate approximations in Lagrangian coordinates (Section 4 in Petruk 2000). Magnetic field is described following Reynolds (1998); we do not consider amplification of the ambient field (though its role is discussed in Section 4).…”

Section: General Descriptionmentioning

confidence: 99%

Hadronic γ-ray images of Sedov supernova remnants

Beshley

Petruk

2011

Monthly Notices of the Royal Astronomical Society

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A number of modern experiments in high‐energy astrophysics produce images of supernova remnants (SNRs) in the TeV and GeV γ‐rays. Either relativistic electrons (due to the inverse‐Compton scattering) or protons (due to the pion decays) may be responsible for this emission. In particular, the broad‐band spectra of SNRs may be explained in both leptonic and hadronic scenarios. Another kind of observational data, namely, images of SNRs, is an important part of experimental information. We present a method to model γ‐ray images of Sedov SNRs in uniform media and magnetic field due to hadronic emission. These γ‐rays are assumed to appear as a consequence of meson decays produced in inelastic collisions of accelerated protons with thermal protons downstream of the shock – a model would be relevant for SNRs without firm confirmations of the shock–cloud interaction, as e.g. SN 1006. Distribution of surface brightness of the shell‐like SNR is synthesized numerically for a number of configurations. An approximate analytical formula for azimuthal and radial variation of hadronic γ‐ray brightness close to the shock is derived. The properties of images as well as the main factors determining the surface brightness distribution are determined. Some conclusions that would be relevant to SN 1006 are discussed.

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“…1 Accurate approximations of the Sedov solution have been proposed for calculations, either in the Eulerian coordinate r (Cox & Franko 1981) or in the Lagrangian coordinate a (Sect. 4.5 in Petruk 2000). 2 The model assumes that the MF is a composition of an ordered (B) and a disordered (δB) component.…”

Section: Magnetohydrodynamics and Relativistic Electrons In Sedov Snrsmentioning

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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Preface

Cited by 8 publications

References 0 publications

Post-adiabatic supernova remnants in an interstellar magnetic field: parallel and perpendicular shocks

Post-adiabatic supernova remnants in an interstellar magnetic field: parallel and perpendicular shocks

Hadronic γ-ray images of Sedov supernova remnants

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

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