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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| Acceso en línea: | http://hdl.handle.net/20.500.12110/paper_22144048_v1-2_n_p31_Torres |
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todo:paper_22144048_v1-2_n_p31_Torres2023-10-03T16:40:38Z Time-dependent modeling of TeV-detected, young pulsar wind nebulae Torres, D.F. Cillis, A. Martín, J. de Oña Wilhelmi, E. 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. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar 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 Torres, D.F. Cillis, A. Martín, J. de Oña Wilhelmi, E. 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. |
| format |
JOUR |
| author |
Torres, D.F. Cillis, A. Martín, J. de Oña Wilhelmi, E. |
| author_facet |
Torres, D.F. Cillis, A. Martín, J. de Oña Wilhelmi, E. |
| author_sort |
Torres, D.F. |
| 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 |
| url |
http://hdl.handle.net/20.500.12110/paper_22144048_v1-2_n_p31_Torres |
| work_keys_str_mv |
AT torresdf timedependentmodelingoftevdetectedyoungpulsarwindnebulae AT cillisa timedependentmodelingoftevdetectedyoungpulsarwindnebulae AT martinj timedependentmodelingoftevdetectedyoungpulsarwindnebulae AT deonawilhelmie timedependentmodelingoftevdetectedyoungpulsarwindnebulae |
| _version_ |
1807322663184498688 |