Origin of spectral bands in the Crab pulsar radio emission
Fuente:
arXiv
Salvato in:
| Autore principale: | |
|---|---|
| Natura: | Preprint |
| Pubblicazione: |
2024
|
| Soggetti: | |
| Accesso online: | |
| Tags: |
Aggiungi Tag
Nessun Tag, puoi essere il primo ad aggiungerne!!
|
| _version_ | 1866915417899925504 |
|---|---|
| author | Medvedev, Mikhail V. |
| author_facet | Medvedev, Mikhail V. |
| contents | The model explaining the spectral "zebra" pattern of the high-frequency interpulse (HFIP) of the Crab pulsar radio emission is proposed. The observed emission bands are diffraction fringes in the spectral domain. The pulsar's own plasma-filled magnetosphere plays a role of a frequency-dependent "diffraction screen". The observed features such as the proportional band spacing, high polarization, constant position angle, and others are explained. The model allows one to perform "tomography" of the pulsar magnetosphere. Indeed, we have obtained the plasma density profile directly from observations, without assuming a particular magnetosphere. Our model is testable and several predictions are made. The two "high-frequency components" observed at the same frequencies as the HFIP are proposed to be related to HFIP. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_12992 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Origin of spectral bands in the Crab pulsar radio emission Medvedev, Mikhail V. High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics Plasma Physics The model explaining the spectral "zebra" pattern of the high-frequency interpulse (HFIP) of the Crab pulsar radio emission is proposed. The observed emission bands are diffraction fringes in the spectral domain. The pulsar's own plasma-filled magnetosphere plays a role of a frequency-dependent "diffraction screen". The observed features such as the proportional band spacing, high polarization, constant position angle, and others are explained. The model allows one to perform "tomography" of the pulsar magnetosphere. Indeed, we have obtained the plasma density profile directly from observations, without assuming a particular magnetosphere. Our model is testable and several predictions are made. The two "high-frequency components" observed at the same frequencies as the HFIP are proposed to be related to HFIP. |
| title | Origin of spectral bands in the Crab pulsar radio emission |
| topic | High Energy Astrophysical Phenomena Astrophysics of Galaxies Solar and Stellar Astrophysics Plasma Physics |
| url | https://arxiv.org/abs/2410.12992 |