Magnetic fields of T Tauri stars in the framework of disk accretion theories
Some disk accretion models developed in recent years predict that each CTTS has a particular magnetic ﬁeld strength depending on its own parameters – masses M∗, radii R∗, the rotation period of a star Prot and mass accretion rate. By measuring these parameters of a star we can evaluate the surface magnetic ﬁeld strength on each classical T Tauri star.
Using a statistically signiﬁcant number of stars with known physical parameters we have got empirical formulas that allow deﬁning one of the key parameters – the mass accretion rate. By using the otherwise method this parameter have been calculated on the bolometrical luminosity, mass and radius of the star. The obtained values of the magnetic ﬁeld strength in the framework of three disk accretion models show valuable diﬀerences for diﬀerent stars and do not agree with measurements of the magnetic ﬁeld strength obtained by direct observations.
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