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Modelling the Dust Emission of the L1551 IRS5 Binary System

Published online by Cambridge University Press:  22 February 2018

M. Osorio
Affiliation:
Instituto de Astrofísica de Andalucía, CSIC, Spain, email: [email protected]
P. D’Alessio
Affiliation:
Centro de Radioastronomía y Astrofísica, UNAM, Mexico
J. Muzerolle
Affiliation:
Steward Observatory, University of Arizona, USA
N. Calvet
Affiliation:
Harvard-Smitsonian Center for Astrophysics, USA.
L. Hartmann
Affiliation:
Harvard-Smitsonian Center for Astrophysics, USA.

Abstract

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We model the L1551 IRS5 source as a system containing two protostars, each surrounded by a circumstellar disk, both encircled by a circumbinary disk, and all disks surrounded by an extended infalling flattened envelope With this composite model, we can calculate self-consistently the spectral energy distribution of the source the shape of the ice and silicate features, and the spatial intensity distributions of the envelope and disks. We compare our model results with the observations, determining the physical parameters of the disks and the envelope. We find that flattened envelope collapse models are required in order to explain the observations and that the infall rate of the envelope is much larger than the accretion rates of the binary disks.

Resumen

Resumen

Modelamos la fuente L1551 IRS5 como un sistema de dos protoestrellas consus discos circunestelares, los cuales a su vez están rodeados por un disco circunbinario. Todos los elementos del sistema todavía están inmersos su envoltura natal, que se encuentra en colapso. Con este modelo calculamos autoconsistentemente la distribución espectral de energía de la fuente, y reproducimos las absorciones características de agua y silicato, así como la distribución espacialde brillo de la envolvente y de los discos. Comparando el modelo con las observaciones determinamos los parametros de todas las componentes del sistema. Encontramos que una envoltura achatada es la más adecuada para explicar las observaciones y que la tasa de acreción de material en esta envoltura es mucho mayor que la tasa de accreción en los discos circunestelares.

Type
Astrophysical Processes of Multiple Stars in Clusters
Copyright
Copyright © Instituto de Astronomia – Mexico 2004

References

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