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.
Saint-Petersburg State University
Chelyabinsk State University
Chelyabinsk State University
Type:
Сonference article
Published:
27.12.2024
Subject area:
UDK 52 Астрономия. Геодезия
UDK 53 Физика
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
UDK 53 Физика
UDK 520 Инструменты, приборы и методы астрономических наблюдений, измерений и анализа
UDK 521 Теоретическая астрономия. Небесная механика. Фундаментальная астрономия. Теория динамической и позиционной астрономии
UDK 523 Солнечная система
UDK 524 Звезды и звездные системы. Вселенная Солнце и Солнечная система
UDK 52-1 Метод изучения
UDK 52-6 Излучение и связанные с ним процессы
GRNTI 41.00 АСТРОНОМИЯ
GRNTI 29.35 Радиофизика. Физические основы электроники
GRNTI 29.31 Оптика
GRNTI 29.33 Лазерная физика
GRNTI 29.27 Физика плазмы
GRNTI 29.05 Физика элементарных частиц. Теория полей. Физика высоких энергий
OKSO 03.06.01 Физика и астрономия
OKSO 03.05.01 Астрономия
OKSO 03.04.03 Радиофизика
BBK 2 ЕСТЕСТВЕННЫЕ НАУКИ
BBK 223 Физика
TBK 614 Астрономия
TBK 6135 Оптика
BISAC SCI004000 Astronomy
BISAC SCI005000 Physics / Astrophysics
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
