Sergey A Khaibrakhmanov
I am a theoretical physicist working in the field of astrophysics. In May 2014, I defended PhD thesis "Fossil magnetic field of accretion disks of young stars". I investigate the physical processes in the accretion disks with fossil large-scale magnetic field, paying special attention to ionization, ohmic diffusion, magnetic ambopolar diffusion and Hall effect. Additionally, I participated in the field survey of Chelyabinsk meteorite, and performed the statistical analysis of its fragments.
Supervisors: prof. Alexander E. Dudorov
Phone: +7-351-799-71-93
Supervisors: prof. Alexander E. Dudorov
Phone: +7-351-799-71-93
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We investigate intensity and geometry of the large-scale fossil magnetic field of young stars’ accretion disks in frame of the model. Analytical estimations and numerical calculations show that, in presence of dust, magnetic field is quasi-azimuthal close to the accretion disk inner edge and quasi-poloidal in the ``dead’’ zones with low ionization fraction and efficient magnetic diffusion. Magnetic field is either quasi-radial or quasi-azimuthal in the outer regions of the accretion disk depending on dust and ionization parameters. In absence of dust, magnetic field is frozen-in in the disk and it is quasi-azimuthal in the inner accretion disk regions and quasi-radial in the outer regions.
Calculations show that inner boundary of the dusty ``dead’’ zone is placed at 0.1-0.6 AU depending on stellar mass. Outer boundary of the ``dead’’ zone is placed at 3-21 AU from the star and it is determined by magnetic ambipolar diffusion. Mass of solid material inside ``dead’’ zones is more than 3 $M_{\oplus}$ for stars with $M \geq 1\,M_{\odot}$.