Spatially radiative properties of 3C 58 and G21.5−0.9

Lu, Fang-Wu; Gao, Q.; Zhu, Bo-Tao; Zhang, Li

doi:10.1093/mnras/stx2223

Cited by 10 publications

(24 citation statements)

References 51 publications

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“…Similar to our work, Lu et al (2017a) models young PWNe (< 10 kyr) that have not been influenced by the returning reverse shock. Their code solves a radially-dependent transport equation similar to ours, but coupled to a photon conservation equation, and additionally includes the effects of particle injection due to photon-photon pair production as well as synchrotron-self-absorption that decreases the number of escaping photons.…”

Section: Comparison To Other Spatial Modelssupporting

confidence: 82%

“…Examples of this methodology are afforded by Porth et al (2016), who used a Nelder-Mead minimisation method coupled to a χ 2 test statistic to find optimal parameters for their transport code when applying their model to three PWNe (fitting SB profiles and X-ray photon spectral index profiles). Similarly, Lu et al (2017a) applied their model to PWN 3C 58, PWN G21.5−0.9 and PWN MSH 15−52, using a χ 2 method to first fit the SED and then predict the spatial behaviour of each source based on the best-fit parameters found using only the SED. Since we are not only fitting a single data set, we calculate the χ 2 value for each of the subsets and then minimise the sum to find the best possible fit (as shown by the red lines in the figures below).…”

Section: Methods For Finding Best Fitsmentioning

confidence: 99%

“…There are also a few differences in our modelling approaches. Lu et al (2017a) invoke the definition of the outer boundary of the PWN as derived by Bucciantini et al (2004) using their spherically-symmetric relativistic MHD PWN model. We, on the other hand, define an escaping boundary radius far beyond the expected PWN radius and allow the particles to freely expand from their initial injection site at the termination shock and escape at this distant boundary.…”

Section: Comparison To Other Spatial Modelsmentioning

confidence: 99%

“…We tested this method in van Rensburg et al (2018) and found that our results were not impacted greatly by the difference in approach. Finally, Lu et al (2017a) use a time-dependent diffusion coefficient, while our coefficient is independent of time. Lastly, they fix the bulk flow normalisation V0(σ) while we leave this as a free parameter.…”

Section: Comparison To Other Spatial Modelsmentioning

confidence: 99%

“…Also, they assume a time-independent diffusion coefficient which is dependent on radius but independent of energy, contrary to our assumption of energy dependence. Porth et al (2016) lastly considered only the X-ray band, while Lu et al (2017b) also considered the radio and TeV energy bands.…”

Section: Comparison To Other Spatial Modelsmentioning

confidence: 99%

See 4 more Smart Citations

Exploiting morphological data from Pulsar Wind Nebulae via a spatiotemporal leptonic transport code

Rensburg

Venter

Seyffert

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The next era of ground-based Cherenkov telescope development will see a great increase in both quantity and quality of γ-ray morphological data. This initiated the development of a spatio-temporal leptonic transport code to model pulsar wind nebulae. We present results from this code that predicts the evolution of the leptonic particle spectrum and radiation at different radii in a spherically-symmetric source. We simultaneously fit the overall broadband spectral energy distribution, the surface brightness profile and the X-ray photon index vs. radius for PWN 3C 58, PWN G21.5−0.9 and PWN G0.9+0.1. Such concurrent fitting of disparate data sets is non-trivial and we thus investigate the utility of different goodness-of-fit statistics, specifically the traditional χ 2 test statistic and a newly developed scaled-flux-normalised test statistic to obtain best-fit parameters. We find reasonable fits to the spatial and spectral data of all three sources, but note some remaining degeneracies that will have to be broken by future observations.

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Section: Comparison To Other Spatial Modelssupporting

confidence: 82%

Section: Methods For Finding Best Fitsmentioning

confidence: 99%

Section: Comparison To Other Spatial Modelsmentioning

confidence: 99%

Section: Comparison To Other Spatial Modelsmentioning

confidence: 99%

Section: Comparison To Other Spatial Modelsmentioning

confidence: 99%

See 3 more Smart Citations

Exploiting morphological data from Pulsar Wind Nebulae via a spatiotemporal leptonic transport code

Rensburg

Venter

Seyffert

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Generation of cosmic rays in pulsar wind nebulae

Sinitsyna

2022

Astron Nachr

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The overall observations of plerions from radio to the very high energy gamma-rays could provide information about the evolution of pulsar wind nebulae (PWN) from the young Crab-like stage to the older plerion stages. Geminga is a nearby (250 pc) and middle-aged pulsar of ∼ 3.4 × 10 5 years. The Geminga pulsar wind nebula was detected in X-rays, and the detailed studies reveal the morphological and spectral variability, which may raise a high energy emission.The extended MeV-TeV emission from Geminga in SHALON, Milagro, HAWC observations, and Fermi-LAT detection and upper limits could arise from the PWN associated with the Geminga SNR. 3C58 is similar to the Crab Nebula (explosion of the 1054 year) on many parameters, but these two objects differ significantly in luminosity and size at X-rays and radio-emission. The 3C 58 estimated age varies from ∼ 800 to (5 − 7) × 10 3 years. MeV-GeV gamma-ray emission from the nebula has been detected by Fermi-LAT. The γ-ray source associated with the 3C 58 was detected above 800 GeV for the first time by SHALON in observations of 2011 year and systematically studied since then.The overall spectral energy distribution and information about the extension of PWN from radio to GeV-TeV energies can contribute to particle transport models and also to the understanding of the mechanisms of PWN expanding, which is, in turn, can shed light on the age of 3C 58 and the history of progenitor SN explosion.

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High energy spatially radiative properties of Vela X pulsar wind nebula

Gao

Zhu

et al. 2019

A&A

Self Cite

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Context. Vela X is a middle-aged pulsar wind nebula (PWN) that has been detected in radio, X-ray, and γ-ray bands. The observations indicate that that photon index and flux density of the inner regions of the nebula have obvious changes as the radial distance increases in the X-ray band, and the surface brightness has been discovered to decrease with the increase of radial distance in γ-ray band. Aims. The multi-band photon emission and high energy spatially radiative properties of Vela X are investigated in the framework of a spatially dependent particle transport model. Methods. Electron distribution inside the PWN was described by a spatially dependent particle transport equation and the evolution of the non-thermal photon was described as a photon conservation equation under the assumption of a spherically symmetric system with dynamical evolution. In this model, the dynamical and particle evolution equations were simultaneously solved, and the γ-ray attenuation by the supernova remnant (SNR) photon fields in the PWN were taken into account. Results. The observed spectral energy distributions of Vela X, including X-ray spectra of the inner regions and γ-ray spectra observed at GeV and TeV bands, are well reproduced. The radial variations of the photon index in X-ray band and the surface brightness in the TeV energy range as well as the γ-ray spectra of the inner region and ring extension can also be well reproduced in the framework of our model. The spatial variations of photon indices at GeV and TeV bands are predicted and show that the photon index in GeV band increases with the increase of radial distance while there is only a slight change in the TeV band. Moreover, the modelling results reveal that the γ-ray attenuation by the SNR photon fields is important for modifying very high energy γ-ray spectrum of Vela X.

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Spatially radiative properties of 3C 58 and G21.5−0.9

Cited by 10 publications

References 51 publications

Exploiting morphological data from Pulsar Wind Nebulae via a spatiotemporal leptonic transport code

Exploiting morphological data from Pulsar Wind Nebulae via a spatiotemporal leptonic transport code

Generation of cosmic rays in pulsar wind nebulae

High energy spatially radiative properties of Vela X pulsar wind nebula

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