Pre-stellar cores

This type of mechanism is a general one and may well occur in regions with high abundances of atomic deuterium such as the centres of pre-stellar cores, discussed in Sec. 1.5. Secondly and more specifically, atomic deuterium can react with methanol to form CH2DOH although the exact mechanism by which this happens is not known definitively. Surface deuteration followed by desorption may well be an important source of gas-phase fractionation, as discussed in Sec. 1.5 following a detailed discussion of gas-phase fractionation. 

Ward-Thompson D, Motte F, Andre P. (1999) The initial conditions of isolated star formation - III. Millimetre continuum mapping of pre-stellar cores. Mon. Not. R. Astron. Soc. 305 143-150. 

Caselli P, van der Tak EPS, Ceccarelli C, Bacmann A (2003) Abundant H2D in the pre-stellar core L1544. Astron Astrophys 403 L37... 

Andr4 P., Ward-Thompson, D., and Baisony, M. (2000). Prom Pre-Stellar Cores to Protostars The Initial Conditions of Star Eormation. In Protostars and Planets IV (V. Mannings, A. P. Boss, and S. S. Russell, eds.), in press. University of Arizona Press, Tucson, AZ. Bachiller, R. (1996). Bipolar molecular outflows from young stars and protostars, Ann. Rev. Astron. Astrophys. 34,111-154. 

Detailed models of deuterium chemistry have been made using realistic density profiles for static pre-stellar cloud cores.These show that Dg becomes more abundant than Hg within a radial distance of 6000 AU from... 

T Tauri star An unstable young variable star in its pre-main sequence phase (see Hertzsprung-Russell diagram). The instability, brought about by the beginning of nuclear fusion in the core of the star, causes pulsations and stellar winds, possibly with bipolar outflows. Groups of such stars, often associated with Herbig-Haro objects, are called T Tauri associations. 

---