1) La descarga del recurso depende de la página de origen
2) Para poder descargar el recurso, es necesario ser usuario registrado en Universia


Opción 1: Descargar recurso

Detalles del recurso

Descripción

We have observed atomic fine-structure lines in the far-infrared (FIR) from 12 oxygen-rich evolved stars. The sample is composed of mostly proto-planetary nebulae (PPNe) and some planetary nebulae (PNe) and asymptotic giant branch (AGB) stars. ISO LWS and SWS observations of [O i], [C ii], [N ii], [Si i], [Si ii], [S i], [Fe i], and [Fe ii] lines were obtained. Taking into account also the sample presented by Fong et al. (Paper I) of carbon-rich evolved stars, we find that PPNe emit in these low-excitation atomic transitions only when the central star is hotter than ∼10 000 K. This result suggests that such lines predominantly arise from photodissociation regions (PDRs), and not from shocked regions. The line widths determined from our Fabry-Perot data also suggest that the FIR lines arise from relatively quiescent PDR gas, as opposed to shocked gas. Our results are in reasonable agreement with predictions from PDR emission models, allowing the estimation of the density of the emitting layers by comparison with the model results. On the other hand, the comparison with predictions of the emission from J-type and C-type shocked regions suggests that detected lines do not come from shocks. The [C ii] line flux has been used to measure the mass of the low-excitation atomic component in PPNe, since this transition has been found to be a useful model-independent probe to estimate the total mass of these PDRs. The derivation of the mass formula and assumptions made are also discussed.

Pertenece a

Caltech Authors  

Autor(es)

Castro -  Carrizo, A. -  Bujarrabal, V. -  Fong, D. -  Meixner, M. -  Tielens, A. G. G. M. -  Latter, W. B. -  Barlow, M. J. - 

Id.: 70994525

Versión: 1.0

Estado: Final

Tipo:  application/pdf - 

Tipo de recurso: Article  -  PeerReviewed  - 

Tipo de Interactividad: Expositivo

Nivel de Interactividad: muy bajo

Audiencia: Estudiante  -  Profesor  -  Autor  - 

Estructura: Atomic

Coste: no

Copyright: sí

Formatos:  application/pdf - 

Requerimientos técnicos:  Browser: Any - 

Relación: [References] http://resolver.caltech.edu/CaltechAUTHORS:20180213-161335427
[References] https://authors.library.caltech.edu/84818/

Fecha de contribución: 15-feb-2018

Contacto:

Localización:
* Castro-Carrizo, A. and Bujarrabal, V. and Fong, D. and Meixner, M. and Tielens, A. G. G. M. and Latter, W. B. and Barlow, M. J. (2001) Low-excitation atomic gas around evolved stars. II. ISO observations of O-rich nebulae. Astronomy and Astrophysics, 367 (2). pp. 674-693. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20180213-161335427

Otros recursos de la mismacolección

  1. Non-Reciprocity in Structures With Nonlinear Internal Hierarchy and Asymmetry Acoustic reciprocity is a property of linear, time invariant systems in which the locations of the s...
  2. Collusion through communication in auctions We study the extent to which communication can serve as a collusion device in one-shot first- and se...
  3. In Vivo Selection of a Computationally Designed SCHEMA AAV Library Yields a Novel Variant for Infection of Adult Neural Stem Cells in the SVZ Directed evolution continues to expand the capabilities of complex biomolecules for a range of appli...
  4. Generic HRTFs May be Good Enough in Virtual Reality. Improving Source Localization through Cross-Modal Plasticity Auditory spatial localization in humans is performed using a combination of interaural time differen...
  5. Intercomparison of OH and OH reactivity measurements in a high isoprene and low NO environment during the Southern Oxidant and Aerosol Study (SOAS) We intercompare OH and OH reactivity datasets from two different techniques, chemical ionization mas...

Aviso de cookies: Usamos cookies propias y de terceros para mejorar nuestros servicios, para análisis estadístico y para mostrarle publicidad. Si continua navegando consideramos que acepta su uso en los términos establecidos en la Política de cookies.