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For low-mass stars, Lrad is very small, b u t it quickly rises, due to t h e strong dependence on stellar mass, Lj-ad ~ M^-^ i^* ^ . e. 2 Mass M^(MQ) Fig. 5. Dependence of the mass-radius relation on the mass accretion rate and on the initial deuterium concentration. In either case, the three curves are for different values of M, as indicated. In the upper panel, the open circles mark the onset of full convection. In the lower panel, no deuterium is present in the gas. of [D/H]. (Adapted from Stahler [47]) gravitational contraction.
Heiles, C. 1993, in Protostars and Planets III, eds. H. I. E. E. , Spitzer, L. E. 1999, in The Origin of Stars and Planetary Systems, eds. J. D. Kylafis (Dordrecht: Kluwer Acad. Press), p. W. W. W. W. W. , Stahler S. W. H. W. W. W. E. , Cassen P. E. 1998, A&A, 330, 145 Von Sengbusch, K. , 69, 79 II. 4 Pre-Main-Sequence Evolution Evolutionary Models Once the main phase of accretion is completed, the stellar core emerges as an optically visible star along the birthline. The physical process by which infall stops is still not known, although stellar winds and bipolar outflows must play a fundamental role.
The mass dependence of luminosities in protostars accreting at 10~^ M© yr ~^. The arrows on the horizontal axis indicate the critical masses where Lrad intersects Lsurf, L D , and Lace, respectively. At Ms, Lsurf climbs steeply to join Lrad (from Palla & Stahler [41]). Let us first apply Fig. 12 to t h e low mass T Tauri stars (M* < 2 M©). According to the figure, such stars begin contracting with Lsurf greater t h a n Lrad- In other words, they radiate more energy per unit time from their surfaces t h a n can be supplied by photons from the interior.