A. C. Raga,1 V. Lora,2 and N. Smith3
1 Instituto de Ciencias Nucleares, Universidad Nacional Autónoma de México, Apdo. Postal 70–543, 04510 D. F., Mexico. (raga@nucleares.unam.mx).
2 Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 70–548, 04510 D. F., Mexico. (vlora@astroscu.unam.mx).
3 Department of Astronomy, University of California, Berkeley, CA 94720, USA. (nathans@astro.berkeley.edu).
Received 2010 January 11
Accepted 2010 February 15
RESUMEN
Consideramos un sistema de flujos eyectados por estrellas de baja masa sumergidas en las puntas de las "trompas de elefante". Suponemos que estos flujos tienen ejes que son intrínsecamente perpendiculares a los ejes de las trompas de elefante. Entonces, derivamos la función de distribución esperada para el ángulo entre las proyecciones sobre el plano del cielo de los ejes del flujo y de la trompa de elefante. Estas funciones de distribución son útiles para interpretar los alineamientos (o falta de alineamientos) observados entre los ejes de flujos HH y trompas de elefante en regiones fotoionizadas.
ABSTRACT
We consider a system of outflows ejected from low mass young stars embedded in the tips of elephant trunks. We assume that these outflows have axes which are intrinsically perpendicular to the axes of the host elephant trunks. We then derive the distribution function expected for the angle between the projections of the outflow and elephant trunk axes on the plane of the sky. These distribution functions are useful for interpreting the alignments (or lack thereof) observed between HH outflow and elephant trunk axes in photoionized regions.
Key Words: ISM: Herbig–Haro objects — ISM: jets and outflows — ISM: kinematics and dynamics — stars: formation.
DESCARGAR ARTÍCULO EN FORMATO PDF
]]> ACKNOWLEDGES
The work of AR and VL was supported by Conacyt grants 61547, 101356 and 101975 and DGAPA–Universidad Nacional Autónoma de México grant IN119709. NS was supported by NASA through grants GO–10241 and GO–10475 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5–26555. We thank an anonymous referee for comments which led to a complete rework of § 5.
REFERENCES
Bally, J., & Reipurth, B. 2003, AJ, 126, 893 [ Links ]
Carlqvist, P., Gahm, G. F., & Kristen, H. 2003, A & A, 403, 399 [ Links ]
Elmegreen, B. G. 1998, in ASP Conf. Ser. 148, Origins, ed. C. E. Woodward, J. M. Shull, & H. A. Thronson, Jr. (San Francisco: ASP), 150 [ Links ]
Gahm, G. F., Carlqvist, P., Johansson, L. B., & Nicolic, S. 2006, A & A, 454, 201 [ Links ]
Gritschneder, M., Naab, T., Walch, S., Burkert, A., & Heitsch, F. 2009, ApJ, 694, L26 [ Links ]
Kajdic, P., & Raga, A. C. 2007, ApJ, 670, 1173 [ Links ]
Lora, V., Raga, A. C., & Esquivel, A. 2009, A & A, 503, 477 [ Links ]
Mackey, J., & Lim, A. J. 2010, MNRAS, in press [ Links ]
Mellema, G., Arthur, S. J., Henney, W. J., Iliev, I. T., & Shapiro, P. R. 2006, ApJ, 647, 397 [ Links ]
Press, W. H., Teukolsky, S. A., Vetterling, W. T., & Flannery, B. P. 2007, Numerical Recipes (Cambridge: Cambridge Univ. Press) [ Links ]
Smith, N., Bally, J., & Brooks, K. 2004, AJ, 127, 2793 [ Links ]
Smith, N., Bally, J., & Walborn, N. R. 2010, MNRAS, (submitted) [ Links ] ]]>