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Title:
How to identify the youngest protostars
Authors:
Stamatellos, D.; Whitworth, A. P.; Boyd, D. F. A.; Goodwin, S. P.
Affiliation:
AA(School of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff CF24 3YB, Wales, UK ), AB(School of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff CF24 3YB, Wales, UK), AC(School of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff CF24 3YB, Wales, UK), AD(School of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff CF24 3YB, Wales, UK)
Publication:
Astronomy and Astrophysics, Volume 439, Issue 1, August III 2005, pp.159-169 (A&A Homepage)
Publication Date:
08/2005
Origin:
EDP Sciences
Astronomy Keywords:
stars: formation, ISM: clouds, dust, extinction, methods: numerical, radiative transfer, hydrodynamics
DOI:
10.1051/0004-6361:20052952
Bibliographic Code:
2005A&A...439..159S

Abstract

We study the transition from a prestellar core to a Class 0 protostar, using SPH to simulate the dynamical evolution, and a Monte Carlo radiative transfer code to generate the SED and isophotal maps. For a prestellar core illuminated by the standard interstellar radiation field, the luminosity is low and the SED peaks at ~190 μ m. Once a protostar has formed, the luminosity rises (due to a growing contribution from accretion onto the protostar) and the peak of the SED shifts to shorter wavelengths (80~to 100 μ m). However, by the end of the Class 0 phase, the accretion rate is falling, the luminosity has decreased, and the peak of the SED shifts back towards longer wavelengths (90 to 150 μ m). In our simulations, the density of material around the protostar remains sufficiently high well into the Class 0 phase that the protostar only becomes visible in the NIR if it is displaced from the centre dynamically. Raw submm/mm maps of Class 0 protostars tend to be much more centrally condensed than those of prestellar cores. However, when convolved with a typical telescope beam, the difference in central concentration is less marked, although the Class 0 protostars appear more circular. Our results suggest that, if a core is deemed to be prestellar on the basis of having no associated IRAS source, no cm radio emission, and no outflow, but it has a circular appearance and an SED which peaks at wavelengths below ~170 μ m, it may well contain a very young Class 0 protostar.
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