Exploring the non-thermal physics behind the pulsar wind nebula PSR J2030+4415 through radio observations
PSR J2030+4415 is a gamma-ray pulsar with an X-ray pulsar wind nebula elongated North-South. The system shows a prominent X-ray filament oriented at an angle of 130° to the nebula axis. To improve our understanding of the non-thermal processes occurring in the pulsar wind nebula, we attempt to deter...
| Autores: | , , , , , , |
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| Tipo de documento: | artigo |
| Estado: | Versão publicada |
| Data de publicação: | 2025 |
| País: | España |
| Recursos: | Varias* (Consorci de Biblioteques Universitáries de Catalunya, Centre de Serveis Científics i Acadèmics de Catalunya) |
| Repositório: | Recercat. Dipósit de la Recerca de Catalunya |
| OAI Identifier: | oai:recercat.cat:2445/221067 |
| Acesso em linha: | https://hdl.handle.net/2445/221067 |
| Access Level: | Acceso aberto |
| Palavra-chave: | Púlsars Observacions astronòmiques Pulsars Astronomical observations |
| Resumo: | PSR J2030+4415 is a gamma-ray pulsar with an X-ray pulsar wind nebula elongated North-South. The system shows a prominent X-ray filament oriented at an angle of 130° to the nebula axis. To improve our understanding of the non-thermal processes occurring in the pulsar wind nebula, we attempt to determine the possible existence of a radio counterpart, study its morphology and obtain restrictive upper limits of the pulsar and filament emission at radio wavelengths. We have performed observations of the pulsar PSR J2030+4415 and its surroundings with the upgraded Giant Metrewave Radio Telescope (uGMRT) at two frequency bands, and put the results in context with findings at other wavelengths. We have obtained radio images at 736 and 1274 MHz revealing a structure trailing the pulsar, with a morphology overlapping the X-ray nebula. This radio structure is the radio counterpart of the X-ray PWN. The derived spectral index along this structure shows spatial variation. There are no hints of the pulsar and the filament at any of the explored radio frequencies but we have obtained restrictive upper limits. A physical scenario that combines the radio and the X-ray observations, and consistent with IR data, of the nebula and the filament is presented. We propose that particle acceleration occurs in the nebula tail due to the presence of a re-collimation shock, and the highest energy particles gradually escape from it through energy-dependent diffusion. We also find a lower limit in the energy of the particles escaping along the X-ray filament of $\sim$~GeV. |
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