Survival of H2 and CO in MHD Disk Winds of Class 0, Class I and Class II Stars

Abstract

We present a model of warm self–similar disk winds [1], aimed at constraining the origin of molecular jets from young stars. We computed the thermal properties, ionization structure and chemical evolution, after imposing an extended molecular network of species and reactions [2]. Here we report results for typical class 0, class I and class II stars. In particular, no H2 and CO destruction occurs for younger stars (higher accretion rates), since the temperature, the ionization fraction and the X-ray photoreaction rate are lower. In general, there is as less molecular gas remaining at the recollimation point as older is the protostar.