SEDs of massive protostars
Abstract
Massive protostars are generally enshrouded in dust, so that most of their radiation emerges in the far infrared. For protostars embedded in opaque, spherical cores, the spectral energy distribution (SED) is determined by two distance-independent parameters, the luminosity-to-mass ratio, L/M_c, and the surface density of the core, Σ=M_c/(π R_c^2), where R_c is the radius of the core. Chakrabarti & McKee (2005a) have derived an approximate analytic expression for the SED that agrees well with numerical results. It is generally not possible to infer the power-law of the density from the SED of a massive protostar. Masses and accretion rates are inferred for several well-studied sources.
- Publication:
-
Massive Star Birth: A Crossroads of Astrophysics
- Pub Date:
- 2005
- DOI:
- 10.1017/S1743921305004631
- Bibcode:
- 2005IAUS..227..276M