An attempt to determine the magnetic field configuration in the planetary nebula K 3-35 with ALMA
We examined dust polarization within the planetary nebula (PN) K 3-35 using the Atacama Large Millimeter/Submillimeter Array (ALMA). This investigation aimed to identify and trace the magnetic field within the PN, as it potentially plays a crucial role in shaping this bipolar nebula. Our findings in...
| Autores: | , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2025 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/391441 |
| Acceso en línea: | http://hdl.handle.net/10261/391441 |
| Access Level: | acceso abierto |
| Palabra clave: | Magnetic fields Polarization Stars: AGB and post-AGB ISM: jets and outflows ISM: planetary nebula: individual: K 3-35 |
| Sumario: | We examined dust polarization within the planetary nebula (PN) K 3-35 using the Atacama Large Millimeter/Submillimeter Array (ALMA). This investigation aimed to identify and trace the magnetic field within the PN, as it potentially plays a crucial role in shaping this bipolar nebula. Our findings include a marginal detection of the polarized region and low fractional polarization (peaking at 1.4 per cent). Assuming a certain level of validity, we observed well-organized dust grains aligned along the equatorial plane of the PN, indicating a magnetic field alignment with the outflows. The limited detection of polarization at submillimeter wavelengths in this PN and others may be attributed to a pronounced optical depth. However, our analysis of K 3-35 with the code dusty does not seem to support this idea. We also modelled the Spectral Energy Distribution (SED) of K3-35, and our best-fitting models included a mixture of silicates and amorphous carbon. The grains of amorphous carbon are less susceptible to alignment with the magnetic field, which could, at least partially, explain the observed low polarization. The models presented in this article should be considered preliminary, and a more advanced approach is needed for a more complete interpretation of the results. © 2025 The Author(s). |
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