Modelling of the continuum emission from Class 0 sources
| dc.creator | Rengel, M. | |
| dc.creator | Froebrich, D. | |
| dc.creator | Wolf, S. | |
| dc.creator | Eisloeffel, J. | |
| dc.date | 2003-11-24 | |
| dc.date.accessioned | 2026-07-25T19:11:55Z | |
| dc.description | Class 0 sources are objects representing the earliest phase of the protostellar evolution. Since they are highly obscured by an extended dusty envelope, these objects emit mainly in the far-infrared to millimetre wavelength range. The analysis of their spectral energy distributions with wide wavelength coverage allows to determine the bolometric temperature and luminosity. However, a more detailed physical interpretation of the internal physical structure of these objects requires radiative transfer modelling. We present modelling results of spectral energy distributions of a sample of nine Class 0 sources in the Perseus and Orion molecular clouds. The SEDs have been simulated using a radiative transfer code based on the Monte Carlo method. We find that a spherically symmetric model for the youngest Class 0 sources allows to reproduce the observed SEDs reasonably well. From our modelling we derive physical parameters of our sources, such as their mass, density distribution, size, etc. We find a density structure of $ρ\sim r^{-2}$ for the collapsing cores at young ages, evolving to $ρ\sim r^{-3/2}$ at later times. | |
| dc.description | 5 pages, 2 figures, Latex, macro included, oral contribution in JENAM 2003, "The early phases of star formation", in press | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0311531 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0311531 | |
| dc.identifier.uri | https://dspace.dare.co.zw/handle/123456789/62413 | |
| dc.subject | Astrophysics | |
| dc.title | Modelling of the continuum emission from Class 0 sources | |
| dc.type | text |