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 2004 January 15
Accepted 2004 July 1.
ABSTRACT
]]> It is now well established that circular, elliptical, and bipolar planetary nebulae (PNe) possess differing physical and spatial characteristics. Not only are their structures quite distinct, but they also appear to possess differing Zanstra temperatures, abundances, expansion velocities, brightness temperatures, and scale heights above the Galactic plane. We report here a further sensitive way in which the differences between these outflows may be illustrated. We shall note that the nebulae posses varying ranges of emission line ratio, and that this is likely to arise as a consequence of their differing progenitor masses. Similarly, we point out the potential of line-ratio mapping for analyzing other morphological classes, as well as for establishing the uniqueness of their populations, and their relative progenitor masses. Thus we find that sources containing jets often possess low line emission intensities relative to hydrogen, suggesting that their progenitors may have low overall masses. This conclusion is supported by a variety of independent observational evidence. We also show that irregular sources appear to represent a distinct class of outflows. It is likely that their mean progenitor masses are greater than those of elliptical PNe, but less than those of the bipolar outflows.Key Words: ISM: Jets and Outflows — ISM: Lines and Bands — Planetary Nebulae: General.
RESUMEN
Está ahora bien establecido que las nebulosas planetarias circulares, elípticas y bipolares poseen diferentes características físicas y espaciales. No sólo son distintas sus estructuras, sino que también parecen tener distintas temperaturas de Zanstra, abundancias, velocidades de expansión, temperaturas de brillo y alturas de escala sobre el plano Galáctico. Reportamos aquí una manera más sensible para ilustrar las diferencias entre estos flujos. Señalamos que las nebulosas poseen muy distintos cocientes de intensidad de sus líneas de emisión y que esto probablemente sea consecuencia de las distintas masas de sus estrellas progenitoras. Asimismo, recalcamos el potencial del mapeo de los cocientes de intensidad de líneas para analizar otras clases morfológicas, así como para establecer la singularidad de su población y las masas relativas de sus progenitoras. Así, encontramos que las fuentes con chorros poseen a menudo líneas de emisión de baja intensidad con relación al hidrógeno, lo cual sugiere que provienen de estrellas de baja masa. Esta conclusión está sustentada en una variedad de evidencias observacionales independientes. También mostramos que las fuentes irregulares aparentemente representan una clase distinta de flujos. Es probable que las masas medias de sus progenitoras sean mayores que las de las nebulosas planetarias elípticas, pero menores que las de los flujos bipolares.
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REFERENCES
Acker, A., Ochsenbein, F., Stenholm, B., Tylenda, R., Marcout, J., & Schohn, C. 1992, Strasbourg-ESO Catalogue of Planetary Nebulae (Garching: ESO) [ Links ]
Bohigas, J. 2001, RevMexAA, 37, 237 [ Links ]
Bond, H. E. 2000, in ASP Conf. Ser. Vol. 199, Asymmetrical Planetary Nebulae II: From Origins to Microstructures, eds. J. H. Kastner, N. Soker, & S. Rappaport (San Francisco: ASP), 115 [ Links ]
Corradi, R. L. M., & Schwarz, H. E. 1995, A & A, 293, 871 [ Links ]
Ferland, G. J. 1978, ApJ, 219, 589 [ Links ]
Gorny, S. K., Stasinska, G., & Tylenda, R. 1997, A & A, 318, 256 [ Links ]
Hartigan, P., Raymond, J., & Hartmann, L. 1987, ApJ, 316, 323 [ Links ]
Hromov, G. S., & Kohoutek, L. 1968, BAC, 19, 1 [ Links ]
Huggins, P.J., Bachiller, R., Cox, P., & Forveille, T. 1996, A & A, 315, 284 [ Links ]
Iijima, T. 1981, in Photometric and Spectroscopic Binary Systems, eds. E. B. Carling & Z. Kopal (Dordrecht: Reidel), 517 [ Links ]
Journel, A. G., & Huijbregts, C. J. 1981, Mining Geostatistics (New York: Academic Press) [ Links ]
Kaler, J. B. 1978, ApJ, 220, 887 [ Links ]
Kaler, J. B., Chu, Y-H., & Jacoby, G. H. 1988, AJ, 96, 1407 [ Links ]
Kaler, J. B., & Jacoby, G. H. 1989, ApJ, 345, 871 [ Links ]
Kaler, J. B., Shaw, R.A ., & Browning, L. 1997, PASP, 109, 289 [ Links ]
López, J. A. 1997, in IAU Symp. 180, Planetary Nebulae, eds. H. J. Habing & H. J. G. L. M. Lamers (Dordercht: Kluwer), 197 [ Links ]
Maciel, W. J. 2001, New Astronomy Reviews, 45, 571 [ Links ]
Maciel, W. J., & Chiappini, C. 1994, ApSS, 219, 231 [ Links ]
Maciel, W. J., & Koeppen, J. 1994, A & A, 282, 436 [ Links ]
Manchado, A., Guerrero, M. A., Stanghellini, L., & Serra-Ricart, M. 1996, The IAC Morphological Catalog of Northern Planetary nebulae (Spain: IAC) [ Links ]
Manchado, A., Villaver, E., Stanghellini, L., & Guerrero, M. A. 2000, in ASP Conf. Ser. Vol. 30, Asymmetrical Planetary Nebulae II: From Origins to Microstructures, eds. J. H. Kastner, N. Soker, & S. Rappaport (San Francisco: ASP), 17 [ Links ]
Marigo, P., Bressan, A., & Chiosi, C. 1998, A & A, 331, 564 [ Links ]
Osterbrock, D. E. 1989, Astrophysics of Gaseous Nebulae and Active Galactic Nuclei, (Sausalito, CA: University Science Books) [ Links ]
Perinotto, M. 1991, ApJS, 76, 687 [ Links ]
Phillips, J. P. 2001a, MNRAS, 32, 1041 [ Links ]
----------. 2001b, PASP, 113, 839 [ Links ]
----------. 2002, A & A, 393, 1027 [ Links ]
----------. 2003a, MNRAS, 344, 501 [ Links ]
----------. 2003b, MNRAS, 340, 883 [ Links ]
----------. 2003c, A & A, 412, 791 [ Links ]
----------. 2004a, MNRAS, in press
]]>Phillips, J. P., & Cuesta, L. 1998, A & A, 133, 381 [ Links ]
Pottasch, S. R., & Preite-Martinez, A. 1983, A & A, 126, 31 [ Links ]
Renzini, A., & Voli, M. 1981, A & A, 94, 175 [ Links ]
Richer, M. G., & McCall, M. L. 1995, ApJ, 445, 642 [ Links ]
Schmeja, S., & Kimeswenger, S. 2001, A & A, 377, 18 [ Links ]
Schonberner, D. 1993, in IAU Symp. 155, Planetary Nebulae, eds. R. Weinberger & A. Acker (Dordercht: Kluwer), 415 [ Links ]
Shull, J. M., & McKee, C. F. 1979, ApJ, 227, 131 [ Links ]
Stanghellini, L., Corradi, R. L. M., & Schwarz, H. E. 1993, A & A, 279, 521 [ Links ]
van den Hoek, L. B., & Groenewegen, M. A. T. 1997, A & AS, 123, 305 [ Links ]
Vassiliadis E., & Wood P. R. 1994, ApJS, 92, 125 [ Links ]
Vázquez, R., Miranda, L. F., Torrelles, J. M., Olguin, L., Benitez, G., Rodriguez, L. F., & Lopez, J. A. 2002, ApJ, 576, 860 [ Links ]
Zijlstra, A. A., & Pottasch, S. R. 1989, A & A, 216, 245 [ Links ]
Zuckerman, B., & Aller, L. H. 1986, ApJ, 301, 772 [ Links ]
Zuckerman, B., & Gatley, I. 1988, ApJ, 324, 501 [ Links ] ]]>