C.D.S. - SIMBAD4 rel 1.7 - 2019.10.18CEST19:41:58

2005A&A...439..159S - Astronomy and Astrophysics, volume 439, 159-169 (2005/8-3)

How to identify the youngest protostars.


Abstract (from CDS):

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 ∼190µm. 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 100µm). 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 150µm). 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 ∼170µm, it may well contain a very young Class 0 protostar.

Abstract Copyright:

Journal keyword(s): stars: formation - ISM: clouds - dust, extinction - methods: numerical - radiative transfer - hydrodynamics

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
ICRS (J2000)
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
1 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 652 0
2 NAME [BM89] L1544 cor 05 04 22.5 +25 11 36           ~ 434 1
3 M 78 RNe 05 46 45.8 +00 04 45   8.0       ~ 334 0
4 NGC 2071 RNe 05 47 10 +00 18.0           ~ 602 1
5 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 2929 0
6 LDN 63 DNe 16 50 15.5 -18 06 06           ~ 74 0

    Equat.    Gal    SGal    Ecl

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