Magnetic fields of T Tauri stars in the framework of disk accretion theories

  • N.Z. Ismailov Шамахинская астрофизическая обсерватория НАН Азербайджана, пос. Ю. Мамедалиева, г. Шамахы, Азербайджан, AZ 5624
  • G.R. Bahaddinova Шамахинская астрофизическая обсерватория НАН Азербайджана, пос. Ю. Мамедалиева, г. Шамахы, Азербайджан, AZ 5624
  • H.A. Abdi Шамахинская астрофизическая обсерватория НАН Азербайджана, пос. Ю. Мамедалиева, г. Шамахы, Азербайджан, AZ 5624

Abstract

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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Published
2013-07-01
How to Cite
Ismailov N., Bahaddinova G., Abdi H., 2013. Izvestiya Krymskoi Astrofizicheskoi Observatorii, vol. 109, no. 4, pp. 126-133. Available at: https://jn.craocrimea.ru/index.php/izvcrao/article/view/438 (Accessed: 5December2020)
Section
Сonference proceedings