Time-dependent modeling of TeV-detected, young pulsar wind nebulae

The increasing sensitivity of instruments at X-ray and TeV energies has revealed a large number of nebulae associated with bright pulsars. Despite this large data set, the observed pulsar wind nebulae (PWNe) do not show a uniform behavior and the main parameters driving features like luminosity, mag...

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Detalles Bibliográficos
Publicado: 2014
Materias:
Pulsars: general
Radiation mechanisms: non-thermal
Acceso en línea:https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_22144048_v1-2_n_p31_Torres
http://hdl.handle.net/20.500.12110/paper_22144048_v1-2_n_p31_Torres
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
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spelling paper:paper_22144048_v1-2_n_p31_Torres2023-06-08T16:35:20Z Time-dependent modeling of TeV-detected, young pulsar wind nebulae Pulsars: general Radiation mechanisms: non-thermal The increasing sensitivity of instruments at X-ray and TeV energies has revealed a large number of nebulae associated with bright pulsars. Despite this large data set, the observed pulsar wind nebulae (PWNe) do not show a uniform behavior and the main parameters driving features like luminosity, magnetization, and others are still not fully understood. To evaluate the possible existence of common evolutive trends and to link the characteristics of the nebula emission with those of the powering pulsar, we selected a sub-set of 10 TeV detections which are likely ascribed to young PWNe and model the spectral energy distribution with a time-dependent description of the nebulae's electron population. In 9 of these cases, a detailed PWNe model, using up-to-date multiwavelength information, is presented. The best-fit parameters of these nebulae are discussed, together with the pulsar characteristics. We conclude that TeV PWNe are particle-dominated objects with large multiplicities, in general far from magnetic equipartition, and that relatively large photon field enhancements are required to explain the high level of Comptonized photons observed. We do not find significant correlations between the efficiencies of emission at different frequencies and the magnetization. The injection parameters do not appear to be particularly correlated with the pulsar properties either. We find that a normalized comparison of the SEDs (e.g., with the corresponding spin-down flux) at the same age significantly reduces the spectral distributions dispersion. © 2014 Elsevier B.V. 2014 https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_22144048_v1-2_n_p31_Torres http://hdl.handle.net/20.500.12110/paper_22144048_v1-2_n_p31_Torres
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Pulsars: general
Radiation mechanisms: non-thermal
spellingShingle Pulsars: general
Radiation mechanisms: non-thermal
Time-dependent modeling of TeV-detected, young pulsar wind nebulae
topic_facet Pulsars: general
Radiation mechanisms: non-thermal
description The increasing sensitivity of instruments at X-ray and TeV energies has revealed a large number of nebulae associated with bright pulsars. Despite this large data set, the observed pulsar wind nebulae (PWNe) do not show a uniform behavior and the main parameters driving features like luminosity, magnetization, and others are still not fully understood. To evaluate the possible existence of common evolutive trends and to link the characteristics of the nebula emission with those of the powering pulsar, we selected a sub-set of 10 TeV detections which are likely ascribed to young PWNe and model the spectral energy distribution with a time-dependent description of the nebulae's electron population. In 9 of these cases, a detailed PWNe model, using up-to-date multiwavelength information, is presented. The best-fit parameters of these nebulae are discussed, together with the pulsar characteristics. We conclude that TeV PWNe are particle-dominated objects with large multiplicities, in general far from magnetic equipartition, and that relatively large photon field enhancements are required to explain the high level of Comptonized photons observed. We do not find significant correlations between the efficiencies of emission at different frequencies and the magnetization. The injection parameters do not appear to be particularly correlated with the pulsar properties either. We find that a normalized comparison of the SEDs (e.g., with the corresponding spin-down flux) at the same age significantly reduces the spectral distributions dispersion. © 2014 Elsevier B.V.
title Time-dependent modeling of TeV-detected, young pulsar wind nebulae
title_short Time-dependent modeling of TeV-detected, young pulsar wind nebulae
title_full Time-dependent modeling of TeV-detected, young pulsar wind nebulae
title_fullStr Time-dependent modeling of TeV-detected, young pulsar wind nebulae
title_full_unstemmed Time-dependent modeling of TeV-detected, young pulsar wind nebulae
title_sort time-dependent modeling of tev-detected, young pulsar wind nebulae
publishDate 2014
url https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_22144048_v1-2_n_p31_Torres
http://hdl.handle.net/20.500.12110/paper_22144048_v1-2_n_p31_Torres
_version_ 1768546606452310016

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