J. P. Phillips
Instituto de Astronomía y Meteorología, Universidad de Guadalajara, Av. Vallarta No. 2602, Col. Arcos Vallarta, 44130 Guadalajara, Jalisco, México (jpp@cencar.udg.mx).
Received, 2005 January 12
Accepted 2005 April 20
]]> RESUMEN
La mayoría de nebulosas planetarias parecen provenir de progenitores con masas MPG ≈ 1 M๏, y es probable que estén relacionadas con estrellas localizadas dentro del disco delgado de la Galaxia. Esto ha sido confirmado a través de una serie de estimaciones de alturas de escala, las cuales implican valores z0(PNe) del orden de ~ 220 pc. Mostraremos que es también posible evaluar la variación de z0(PNe) con la distancia galactocéntrica R. Aunque tal análisis está sujeto a varias incertidumbres, incluyendo las asociadas con las distancias de las nebulosas, es posible demostrar que cuando se incrementa R, aumenta z0(PNe). Esta variación espacial es congruente con lo que conocemos sobre otros componentes del disco.
ABSTRACT
Most planetary nebulae appear to arise from progenitors with mass MPG ≈ 1 M๏. One would therefore expect them to be closely associated with stars located within the galactic thin disk. This has been confirmed through a series of recent estimates of scale height, which imply values z0(PNe) of order ~ 220 pc. We shall show, 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 several uncertainties, including those associated with the distances to these outflows, it is nevertheless possible to demonstrate that z0(PNe) increases with increasing R. This spatial "flaring" is consistent with what is known of various other disk components.
Key Words: ISM: Jets and outflows — Planetary nebulae: General.
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