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Dynamics of magnetic flux tubes and IR-variability of young stellar objects. / Khaibrakhmanov, Sergey; Dudorov, Alexander; Sobolev, Andrey.

In: Research in Astronomy and Astrophysics, Vol. 18, No. 8, 01.08.2018.

Research output: Contribution to journal › Article › peer-review

Harvard

Khaibrakhmanov, S, Dudorov, A & Sobolev, A 2018, 'Dynamics of magnetic flux tubes and IR-variability of young stellar objects', Research in Astronomy and Astrophysics, vol. 18, no. 8. https://doi.org/10.1088/1674-4527/18/8/90

APA

Khaibrakhmanov, S., Dudorov, A., & Sobolev, A. (2018). Dynamics of magnetic flux tubes and IR-variability of young stellar objects. Research in Astronomy and Astrophysics, 18(8). https://doi.org/10.1088/1674-4527/18/8/90

Vancouver

Khaibrakhmanov S, Dudorov A, Sobolev A. Dynamics of magnetic flux tubes and IR-variability of young stellar objects. Research in Astronomy and Astrophysics. 2018 Aug 1;18(8). https://doi.org/10.1088/1674-4527/18/8/90

Author

Khaibrakhmanov, Sergey ; Dudorov, Alexander ; Sobolev, Andrey. / Dynamics of magnetic flux tubes and IR-variability of young stellar objects. In: Research in Astronomy and Astrophysics. 2018 ; Vol. 18, No. 8.

BibTeX

@article{a271c8edf0de42159c8929bb78e84c3b,
title = "Dynamics of magnetic flux tubes and IR-variability of young stellar objects",
abstract = "We simulate the dynamics of slender magnetic flux tubes (MFTs) in the accretion disks of T Tauri stars. The dynamical equations of our model take into account aerodynamic and turbulent drag forces, and the radiative heat exchange between the MFT and ambient gas. The structure of the disk is calculated with the help of our MHD model of the accretion disks. We consider the MFTs formed at distances of 0.027-0.8 au from the star with various initial radii and plasma betas β 0. The simulations show that MFTs with a weak magnetic field (β 0 = 10) rise slowly with speeds less than the speed of sound. MFTs with β 0 = 1 form an outflowing magnetized corona above the disk. Strongly magnetized MFTs (β 0 = 0.1) can cause outflows with velocities 20 - 50 km s-1. The tubes rise periodically over times from several days to several months according to our simulations. We propose that periodically rising MFTs can absorb stellar radiation and contribute to the IR-variability of young stellar objects.",
keywords = "accretion disks, instabilities, magnetohydrodynamics (MHD), protoplanetary disks",
author = "Sergey Khaibrakhmanov and Alexander Dudorov and Andrey Sobolev",
year = "2018",
month = aug,
day = "1",
doi = "10.1088/1674-4527/18/8/90",
language = "English",
volume = "18",
journal = "Research in Astronomy and Astrophysics",
issn = "1674-4527",
publisher = "IOP Publishing Ltd.",
number = "8",

}

RIS

TY - JOUR

T1 - Dynamics of magnetic flux tubes and IR-variability of young stellar objects

AU - Khaibrakhmanov, Sergey

AU - Dudorov, Alexander

AU - Sobolev, Andrey

PY - 2018/8/1

Y1 - 2018/8/1

N2 - We simulate the dynamics of slender magnetic flux tubes (MFTs) in the accretion disks of T Tauri stars. The dynamical equations of our model take into account aerodynamic and turbulent drag forces, and the radiative heat exchange between the MFT and ambient gas. The structure of the disk is calculated with the help of our MHD model of the accretion disks. We consider the MFTs formed at distances of 0.027-0.8 au from the star with various initial radii and plasma betas β 0. The simulations show that MFTs with a weak magnetic field (β 0 = 10) rise slowly with speeds less than the speed of sound. MFTs with β 0 = 1 form an outflowing magnetized corona above the disk. Strongly magnetized MFTs (β 0 = 0.1) can cause outflows with velocities 20 - 50 km s-1. The tubes rise periodically over times from several days to several months according to our simulations. We propose that periodically rising MFTs can absorb stellar radiation and contribute to the IR-variability of young stellar objects.

AB - We simulate the dynamics of slender magnetic flux tubes (MFTs) in the accretion disks of T Tauri stars. The dynamical equations of our model take into account aerodynamic and turbulent drag forces, and the radiative heat exchange between the MFT and ambient gas. The structure of the disk is calculated with the help of our MHD model of the accretion disks. We consider the MFTs formed at distances of 0.027-0.8 au from the star with various initial radii and plasma betas β 0. The simulations show that MFTs with a weak magnetic field (β 0 = 10) rise slowly with speeds less than the speed of sound. MFTs with β 0 = 1 form an outflowing magnetized corona above the disk. Strongly magnetized MFTs (β 0 = 0.1) can cause outflows with velocities 20 - 50 km s-1. The tubes rise periodically over times from several days to several months according to our simulations. We propose that periodically rising MFTs can absorb stellar radiation and contribute to the IR-variability of young stellar objects.

KW - accretion disks

KW - instabilities

KW - magnetohydrodynamics (MHD)

KW - protoplanetary disks

UR - http://www.scopus.com/inward/record.url?scp=85051504825&partnerID=8YFLogxK

U2 - 10.1088/1674-4527/18/8/90

DO - 10.1088/1674-4527/18/8/90

M3 - Article

AN - SCOPUS:85051504825

VL - 18

JO - Research in Astronomy and Astrophysics

JF - Research in Astronomy and Astrophysics

SN - 1674-4527

IS - 8

ER -

ID: 103443273