Abstract
We discuss evidence supporting the magnetospheric accretion mode of mass transfer onto the star for a much larger range of masses that previously known, ∼ 0.03M⊙ — ∼ 5M⊙, and show corresponding mass accretion rate determination over this mass range. We find that the mass accretion rate M increases with stellar mass M*, roughly asÿ M ∝ M 2* . The physical principles behind this correlation are unknown at present; they must involve mechanisms for transporting angular momentum outwards in the disk which must be active for accretion to take place. The recently found correlation between X-ray luminosity and stellar mass may play a role, by influencing the ionization degree in the disk, necessary for the magnetorotational instability, the most accepted mechanism driving accretion, to operate.
Smithsonian Astrophysical Observatory
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Calvet, N., Muzerolle, J. (2003). Accretion Powered Emission in Young Stellar Objects. In: Lépine, J., Gregorio-Hetem, J. (eds) Open Issues in Local Star Formation. Astrophysics and Space Science Library, vol 299. Springer, Dordrecht. https://doi.org/10.1007/1-4020-2600-5_11
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DOI: https://doi.org/10.1007/1-4020-2600-5_11
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