DYNAMICS OF DUST GRAINS AND SMALL BODIES IN ACCRETION DISKS OF YOUNG STARS WITH FOSSIL MAGNETIC FIELD
Section: STARS AND THE INTERSTELLAR MEDIUM
Authors:
1.
Saint-Petersburg State University
2.
Ural Federal University
Saint-Petersburg University
Chelyabinsk State University
Saint-Petersburg University
Chelyabinsk State University
Type:
Сonference article
Published:
27.12.2024
Subject area:
52
53
520
521
523
524
52-1
52-6
41.00
29.35
29.31
29.33
29.27
29.05
03.06.01
03.05.01
03.04.03
2
223
614
6135
SCI004000
SCI005000
53
520
521
523
524
52-1
52-6
41.00
29.35
29.31
29.33
29.27
29.05
03.06.01
03.05.01
03.04.03
2
223
614
6135
SCI004000
SCI005000
Language:
English
Keywords:
ISM: magnetic fields, dust; accretion disks; magnetohydrodynamics (MHD); protoplanetary disks
Abstract (English):
The paper discusses a numerical model that explores the dynamics of dust particles and small bodies within accretion disks that contain fossil magnetic fields. The model equations include gravitational force, centrifugal force, and drag force depending on particle size and speed. The disk structure is simulated using the magnetohydrodynamic model of Dudorov and Khaibrakhmanov, taking into account the effect of magnetic tensions on gas rotation speed. The dynamics of particles ranging in size from $10^{-4}$ cm to $10^2$ cm in an accretion disk of a typical T Tauri star are modeled. The simulations indicate that the dynamics of particles with a size of 1 m consists in fast sedimentation towards the midplane, followed by a slower radial drift. Sedimentation is accompanied by damped oscillations around the midplane. The slowdown of gas rotation due to magnetic tension leads to an increase in radial drift speed at the disk's periphery. Therefore, the depletion of solid particles in the outer regions of the disks and their accumulation in the “dead” zones with weak magnetic fields may occur more rapidly in disks with magnetic fields.
The paper discusses a numerical model that explores the dynamics of dust particles and small bodies within accretion disks that contain fossil magnetic fields. The model equations include gravitational force, centrifugal force, and drag force depending on particle size and speed. The disk structure is simulated using the magnetohydrodynamic model of Dudorov and Khaibrakhmanov, taking into account the effect of magnetic tensions on gas rotation speed. The dynamics of particles ranging in size from $10^{-4}$ cm to $10^2$ cm in an accretion disk of a typical T Tauri star are modeled. The simulations indicate that the dynamics of particles with a size of 1 m consists in fast sedimentation towards the midplane, followed by a slower radial drift. Sedimentation is accompanied by damped oscillations around the midplane. The slowdown of gas rotation due to magnetic tension leads to an increase in radial drift speed at the disk's periphery. Therefore, the depletion of solid particles in the outer regions of the disks and their accumulation in the “dead” zones with weak magnetic fields may occur more rapidly in disks with magnetic fields.
Keywords:
ISM: magnetic fields, dust; accretion disks; magnetohydrodynamics (MHD); protoplanetary disks
ISM: magnetic fields, dust; accretion disks; magnetohydrodynamics (MHD); protoplanetary disks
1. Dudorov A. and Khaibrakhmanov S., 2014, Astrophysics and Space Science, 352, p. 103
2. Khaibrakhmanov S., 2024, Astronomical and Astrophysical Transactions, arXiv:2401.14180
3. Khaibrakhmanov S. and Dudorov A., 2022, Astronomy Reports, 99, 10, p. 832
4. Williams J. and Cieza L., 2011, Annual Review of Astronomy and Astrophysics, 49, p. 67
