Photoevaporation of protostellar disks. V. Circumstellar disks under the influence of both extreme-ultraviolet and far-ultraviolet radiation

The evolution and appearance of protostellar disks can be significantly alt ered by their UV environment. We investigate numerically the photoevaporati on of protostellar disks under the influence of an external radiation held with both EUV (hv > 13.6 eV) and FUV (6 eV < hv < 13.6 eV) components. Our two-dimensional axisymmetric radiation hydrodynamics calculations begin wit h star-disk configurations resulting from previously published collapse sim ulations. We follow the evolution after the external UV radiation source ha s been turned on. We consider the transfer of both direct (from the UV poin t source) as well as diffuse radiation fields simultaneously with the ioniz ation of hydrogen and carbon. A simplified cooling function is employed whi ch assumes that the carbon ionization front separates the molecular region from the region in atomic or ionized form. For some simulations an isotropi c stellar wind has been included at the position of the disk's central star . At selected evolutionary times a frequency-dependent ray-tracing diagnost ic code is used to calculate emission line spectra and emission line maps o ver the volume of interest. The interaction of the FUV-induced neutral how at the disk surface with the direct and diffuse EUV radiation fields leads to the typical head-tail objects with bright emission line crescents and ta ils pointing away from the external radiation source. The properties of the head-tail objects are in agreement with the properties of the proplyds in the Orion Nebula, M8, NGC 2024, and-in a more extreme UV environment-of the newly discovered proplyds in NGC 3603. After losing material via photoevap oration over a time,greater than or similar to 10(5) yr, our initially rath er massive disks are reduced to typical observed disk masses. At this time the radius of the disk, the radius of the hydrogen ionization front, and th e length of the tail are compatible to observed proplyds. Our model disks c an be either silhouetted or nonsilhouetted in the emission line maps, depen ding on orientation. The [O III] 5007 Angstrom emission appears more diffus e than [O II] 3726 Angstrom, because the abundance of O III is low near the hydrogen ionization front and in the shadow regions along the tail. Monopo lar and bipolar microjets emerging from the proplyds can be explained by sp herically symmetric stellar winds hydrodynamically focused by the neutral e vaporating flow from the disk surface.