Using planetary nebulae to probe the structure of the galactic thin disk
Most planetary nebulae appear to arise from progenitors with mass MPG 1 M. One would therefore expect them to be closely associated with stars locatedwithin the galactic thin disk. This has been confrmed through a series of recentestimates of scale height, which imply values z0(PNe) of order 220 pc....
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| Tipo de documento: | artigo |
| Estado: | Versão publicada |
| Data de publicação: | 2005 |
| País: | México |
| Recursos: | Universidad de Guadalajara |
| Repositório: | Redalyc-UDG |
| OAI Identifier: | oai:redalyc.org:57141205 |
| Acesso em linha: | https://www.redalyc.org/articulo.oa?id=57141205 |
| Access Level: | Acceso aberto |
| Palavra-chave: | Física, Astronomía y Matemáticas ISM: JETS AND OUTFLOWS PLANETARY NEBULAE: GENERAL |
| Resumo: | Most planetary nebulae appear to arise from progenitors with mass MPG 1 M. One would therefore expect them to be closely associated with stars locatedwithin the galactic thin disk. This has been confrmed through a series of recentestimates of scale height, which imply values z0(PNe) of order 220 pc. We shallshow, in the following, that it is also possible to evaluate the variation of z0(PNe)with galactocentric distance R. Although such an analysis is subject to severaluncertainties, including those associated with the distances to these outows, it isnevertheless possible to demonstrate that z0(PNe) increases with increasing R. Thisspatial \aring" is consistent with what is known of various other disk components. |
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