Outflow and Emission Model of Pulsar Wind Nebulae with the Back Reaction of Particle Diffusion

Ishizaki, W.; Asano, Katsuaki; Kawaguchi, Kyohei

doi:10.3847/1538-4357/aae389

Cited by 18 publications

(15 citation statements)

References 42 publications

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“…Our methodology is mainly established by Ishizaki et al(2017Ishizaki et al( ,2018 [8,9]. We assume that the PWN is a steady and spherical bubble with a radius r N .…”

Section: Methodsmentioning

confidence: 99%

“…Note that, with regard to DF model, in order to satisfy the consistency between the fluid structure and the distribution function of non-thermal particles, we formulated the effect of the back-reaction of the diffusion process to the fluid motion. However, in the scope of the results presented in this paper, the effect of the back-reaction is almost negligible, so we omit a description of that formulation (see Ishizaki et al(2018) [9] for details). For the fluid structure, the almost same calculation as the KC model [1] is mainly performed.…”

Section: Pos(icrc2019)704mentioning

confidence: 99%

“…In order to clarify the problems of the KC model, we examine both the emission spectrum integrated over the entire nebula and the surface brightness profile of X-rays simultaneously [8]. Furthermore, based on the results, we construct a model with the diffusion process, and the observed entire spectra and surface brightness profiles are simultaneously reproduced for G21.5-0.9 and 3C58 [9]. These are based on the results reported as Ishizaki et al…”

Section: Introductionmentioning

confidence: 96%

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Modeling of Broadband Spectra and Radial Profiles of Emission of Pulsar Wind Nebulae

Ishizaki¹,

Asano²,

Kawaguchi³

2019

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019)

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X-ray emission of a pulsar wind nebula (PWN) is a group of particles with the highest energy among the non-thermal electron-positrons present in the nebula. The standard emission model of PWNe predicts that such high energy particles lose their energy immediately by radiative cooling and that the emission region of X-rays is smaller than those of lower frequencies. However, as 3C 58 and G21.5-0.9, some PWNe have been discovered in which the emission region of X-rays and radio extend to the almost same extent, and it has been pointed out that the conventional model has room for reconsideration. We investigate the validity of the model by simultaneously calculating the emission spectrum integrating over the entire nebula and the radial profile of the X-ray surface brightness. Our detailed analysis reveals that the conventional model cannot explain observational facts of 3C 58 and G21.5-0.9. Furthermore, in order to improve the model, we construct a model of PWNe in consideration of spatial diffusion due to a disturbed magnetic field. We show that entire spectra and X-ray surface brightness profiles are reproduced simultaneously by our new model. The model implies the existence of a large gamma-ray halo which consists of particles diffusely escaped out of the nebula. The halo could spread to a degree that it can be resolved spatially by the Cherenkov Telescope Array.

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“…Our methodology is mainly established by Ishizaki et al(2017Ishizaki et al( ,2018 [8,9]. We assume that the PWN is a steady and spherical bubble with a radius r N .…”

Section: Methodsmentioning

confidence: 99%

Section: Pos(icrc2019)704mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 96%

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Modeling of Broadband Spectra and Radial Profiles of Emission of Pulsar Wind Nebulae

Ishizaki¹,

Asano²,

Kawaguchi³

2019

Proceedings of 36th International Cosmic Ray Conference — PoS(ICRC2019)

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“…Recently, Ishizaki et al () tried to explain both SED and spatial variations measured for 3C 58 by approximately solving fluid equations with diffusion. This model seems to explain the SED (without the possible IR feature), but matches with the spatial variations are rather poor.…”

Section: Observational Properties Of 3c 58 and Previous Modelingmentioning

confidence: 99%

Spectral energy distribution modeling of broadband emission in the pulsar wind nebula 3C 58

Kim

2020

Astron Nachr

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We investigate the broadband emission properties of the pulsar wind nebula (PWN) 3C 58 using a spectral energy distribution (SED) model. We attempt to match simultaneously the broadband SED and spatial variations of X‐ray emission in the PWN. We further use the model to explain a possible far‐IR feature of which a hint was recently suggested in 3C 58: a small bump at ∼1011 GHz in the PLANCK and Herschel bands. While external dust emission may easily explain the observed bump, it may be the internal emission of the source, implying an additional population of particles. Although significance for the bump is not high, here we explore possible origins of the IR bump using the emission model, and find that a population of electrons with GeV energies can explain it. If it is produced in the PWN, it may provide new insights into particle acceleration and flows in PWNe.

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“…To assess if the diffusion scenario is viable the transport of the particles near the termination shock must be studied in detail, which is, however, beyond the scope of this paper (for some studies in this direction, see, e.g. Van Etten & Romani 2011; Porth et al 2016;Ishizaki et al 2018).…”

Section: Origin Of the Cocoon And Particle Transportmentioning

confidence: 99%

H.E.S.S. andSuzakuobservations of the Vela X pulsar wind nebula

Abdalla¹,

Aharonian²,

Benkhali³

et al. 2019

A&A

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Context. Pulsar wind nebulae (PWNe) represent the most prominent population of Galactic very-high-energy gamma-ray sources and are thought to be an efficient source of leptonic cosmic rays. Vela X is a nearby middle-aged PWN, which shows bright X-ray and TeV gamma-ray emission towards an elongated structure called the cocoon. Aims. Since TeV emission is likely inverse-Compton emission of electrons, predominantly from interactions with the cosmic microwave background, while X-ray emission is synchrotron radiation of the same electrons, we aim to derive the properties of the relativistic particles and of magnetic fields with minimal modelling. Methods. We used data from the Suzaku XIS to derive the spectra from three compact regions in Vela X covering distances from 0.3 to 4 pc from the pulsar along the cocoon. We obtained gamma-ray spectra of the same regions from H.E.S.S. observations and fitted a radiative model to the multi-wavelength spectra. Results. The TeV electron spectra and magnetic field strengths are consistent within the uncertainties for the three regions, with energy densities of the order 10−12 erg cm−3. The data indicate the presence of a cutoff in the electron spectrum at energies of ~ 100 TeV and a magnetic field strength of ~6 μG. Constraints on the presence of turbulent magnetic fields are weak. Conclusions. The pressure of TeV electrons and magnetic fields in the cocoon is dynamically negligible, requiring the presence of another dominant pressure component to balance the pulsar wind at the termination shock. Sub-TeV electrons cannot completely account for the missing pressure, which may be provided either by relativistic ions or from mixing of the ejecta with the pulsar wind. The electron spectra are consistent with expectations from transport scenarios dominated either by advection via the reverse shock or by diffusion, but for the latter the role of radiative losses near the termination shock needs to be further investigated in the light of the measured cutoff energies. Constraints on turbulent magnetic fields and the shape of the electron cutoff can be improved by spectral measurements in the energy range ≳ 10 keV.

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Outflow and Emission Model of Pulsar Wind Nebulae with the Back Reaction of Particle Diffusion

Cited by 18 publications

References 42 publications

Modeling of Broadband Spectra and Radial Profiles of Emission of Pulsar Wind Nebulae

Modeling of Broadband Spectra and Radial Profiles of Emission of Pulsar Wind Nebulae

Spectral energy distribution modeling of broadband emission in the pulsar wind nebula 3C 58

H.E.S.S. andSuzakuobservations of the Vela X pulsar wind nebula

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