OPEN SLIT ECHELLE SPECTROSCOPY OF PLANETARY NEBULA M 1-9
Optical spectroscopy of the entire planetary nebula M 1-9, reveals pronounced density variations, a temperature distribution where Te(N+) is larger than Te(O+2) and abundances indicating that it is a halo planetary nebulae, an association supported by it is very large radial velocity and distance to...
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2012 |
| País: | México |
| Institución: | Universidad Nacional Autónoma de México |
| Repositorio: | Redalyc-UNAM |
| OAI Identifier: | oai:redalyc.org:57124423011 |
| Acceso en línea: | https://www.redalyc.org/articulo.oa?id=57124423011 |
| Access Level: | acceso abierto |
| Palabra clave: | Física, Astronomía y Matemáticas 9) ISM: abundances planetary nebulae: general ISM: individual objects (M 1 |
| Sumario: | Optical spectroscopy of the entire planetary nebula M 1-9, reveals pronounced density variations, a temperature distribution where Te(N+) is larger than Te(O+2) and abundances indicating that it is a halo planetary nebulae, an association supported by it is very large radial velocity and distance to the galactic plane. The ionized mass is between 0.1 and 0.4 M☉. A uniform density photoionization model (Cloudy, version 10.00) reproduced most of the spectrum, but the intensity of [O III] 4363 °A is much larger than observed. In this model, nebular abundances are smaller than those derived using standard techniques and the stellar temperature and luminosity are 84900ºK and 1025 L☉, which implies that the progenitor probably was a =1 M☉ zero-age main sequence star. |
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