VERTICAL STRUCTURE OF MAGNETIZED ACCRETION DISKS AROUND YOUNG STARS

ABSTRACT We model the vertical structure of the magnetized accretion disks that are subject to viscous and resistive heating and irradiation by the central star. We apply our formalism to the radial structure of the magnetized accretion disks that are threaded by the poloidal magnetic field dragged...

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Veröffentlicht in:The Astrophysical journal Jg. 817; H. 1; S. 35 - 52
Hauptverfasser: Lizano, S., Tapia, C., Boehler, Y., D'Alessio, P.
Format: Journal Article
Sprache:Englisch
Veröffentlicht: United Kingdom The American Astronomical Society 20.01.2016
Schlagworte:
ACCRETION DISKS
accretion, accretion disks
ASPECT RATIO
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Balances (scales)
COMPARATIVE EVALUATIONS
Disks
EMISSION
Formalism
Heating
Irradiation
ISM: magnetic fields
MAGNETIC FIELDS
MAGNETIZATION
MAGNETOHYDRODYNAMICS
magnetohydrodynamics (MHD)
MASS
protoplanetary disks
PROTOPLANETS
PROTOSTARS
ROTATION
STAR EVOLUTION
STARS
stars: formation
STELLAR ATMOSPHERES
VELOCITY
ISSN:0004-637X, 1538-4357
Online-Zugang:Volltext
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Abstract ABSTRACT We model the vertical structure of the magnetized accretion disks that are subject to viscous and resistive heating and irradiation by the central star. We apply our formalism to the radial structure of the magnetized accretion disks that are threaded by the poloidal magnetic field dragged during the process of star formation, which was developed by Shu and coworkers. We consider disks around low-mass protostars, T Tauri, and FU Orionis stars, as well as two levels of disk magnetization: (strongly magnetized disks) and (weakly magnetized disks). The rotation rates of strongly magnetized disks have large deviations from Keplerian rotation. In these models, resistive heating dominates the thermal structure for the FU Ori disk, and the T Tauri disk is very thin and cold because it is strongly compressed by magnetic pressure; it may be too thin compared with observations. Instead, in the weakly magnetized disks, rotation velocities are close to Keplerian, and resistive heating is always less than 7% of the viscous heating. In these models, the T Tauri disk has a larger aspect ratio, which is consistent with that inferred from observations. All the disks have spatially extended hot atmospheres where the irradiation flux is absorbed, although most of the mass (∼90%-95%) is in the disk midplane. With the advent of ALMA one expects direct measurements of magnetic fields and their morphology at disk scales. It will then be possible to determine the mass-to-flux ratio of magnetized accretion disks around young stars, an essential parameter for their structure and evolution. Our models contribute to the understanding of the vertical structure and emission of these disks.
AbstractList We model the vertical structure of the magnetized accretion disks that are subject to viscous and resistive heating and irradiation by the central star. We apply our formalism to the radial structure of the magnetized accretion disks that are threaded by the poloidal magnetic field dragged during the process of star formation, which was developed by Shu and coworkers. Instead, in the weakly magnetized disks, rotation velocities are close to Keplerian, and resistive heating is always less than 7% of the viscous heating. In these models, the T Tauri disk has a larger aspect ratio, which is consistent with that inferred from observations. All the disks have spatially extended hot atmospheres where the irradiation flux is absorbed, although most of the mass (~90%-95%) is in the disk midplane. With the advent of ALMA one expects direct measurements of magnetic fields and their morphology at disk scales. Our models contribute to the understanding of the vertical structure and emission of these disks.
We model the vertical structure of the magnetized accretion disks that are subject to viscous and resistive heating and irradiation by the central star. We apply our formalism to the radial structure of the magnetized accretion disks that are threaded by the poloidal magnetic field dragged during the process of star formation, which was developed by Shu and coworkers. We consider disks around low-mass protostars, T Tauri, and FU Orionis stars, as well as two levels of disk magnetization: (strongly magnetized disks) and (weakly magnetized disks). The rotation rates of strongly magnetized disks have large deviations from Keplerian rotation. In these models, resistive heating dominates the thermal structure for the FU Ori disk, and the T Tauri disk is very thin and cold because it is strongly compressed by magnetic pressure; it may be too thin compared with observations. Instead, in the weakly magnetized disks, rotation velocities are close to Keplerian, and resistive heating is always less than 7% of the viscous heating. In these models, the T Tauri disk has a larger aspect ratio, which is consistent with that inferred from observations. All the disks have spatially extended hot atmospheres where the irradiation flux is absorbed, although most of the mass (∼90%–95%) is in the disk midplane. With the advent of ALMA one expects direct measurements of magnetic fields and their morphology at disk scales. It will then be possible to determine the mass-to-flux ratio of magnetized accretion disks around young stars, an essential parameter for their structure and evolution. Our models contribute to the understanding of the vertical structure and emission of these disks.
ABSTRACT We model the vertical structure of the magnetized accretion disks that are subject to viscous and resistive heating and irradiation by the central star. We apply our formalism to the radial structure of the magnetized accretion disks that are threaded by the poloidal magnetic field dragged during the process of star formation, which was developed by Shu and coworkers. We consider disks around low-mass protostars, T Tauri, and FU Orionis stars, as well as two levels of disk magnetization: (strongly magnetized disks) and (weakly magnetized disks). The rotation rates of strongly magnetized disks have large deviations from Keplerian rotation. In these models, resistive heating dominates the thermal structure for the FU Ori disk, and the T Tauri disk is very thin and cold because it is strongly compressed by magnetic pressure; it may be too thin compared with observations. Instead, in the weakly magnetized disks, rotation velocities are close to Keplerian, and resistive heating is always less than 7% of the viscous heating. In these models, the T Tauri disk has a larger aspect ratio, which is consistent with that inferred from observations. All the disks have spatially extended hot atmospheres where the irradiation flux is absorbed, although most of the mass (∼90%-95%) is in the disk midplane. With the advent of ALMA one expects direct measurements of magnetic fields and their morphology at disk scales. It will then be possible to determine the mass-to-flux ratio of magnetized accretion disks around young stars, an essential parameter for their structure and evolution. Our models contribute to the understanding of the vertical structure and emission of these disks.
We model the vertical structure of the magnetized accretion disks that are subject to viscous and resistive heating and irradiation by the central star. We apply our formalism to the radial structure of the magnetized accretion disks that are threaded by the poloidal magnetic field dragged during the process of star formation, which was developed by Shu and coworkers. We consider disks around low-mass protostars, T Tauri, and FU Orionis stars, as well as two levels of disk magnetization: λ{sub sys}=4 (strongly magnetized disks) and λ{sub sys}=12 (weakly magnetized disks). The rotation rates of strongly magnetized disks have large deviations from Keplerian rotation. In these models, resistive heating dominates the thermal structure for the FU Ori disk, and the T Tauri disk is very thin and cold because it is strongly compressed by magnetic pressure; it may be too thin compared with observations. Instead, in the weakly magnetized disks, rotation velocities are close to Keplerian, and resistive heating is always less than 7% of the viscous heating. In these models, the T Tauri disk has a larger aspect ratio, which is consistent with that inferred from observations. All the disks have spatially extended hot atmospheres where the irradiation flux is absorbed, although most of the mass (∼90%–95%) is in the disk midplane. With the advent of ALMA one expects direct measurements of magnetic fields and their morphology at disk scales. It will then be possible to determine the mass-to-flux ratio of magnetized accretion disks around young stars, an essential parameter for their structure and evolution. Our models contribute to the understanding of the vertical structure and emission of these disks.
Author Tapia, C.
D'Alessio, P.
Lizano, S.
Boehler, Y.
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  surname: Lizano
  fullname: Lizano, S.
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  givenname: C.
  surname: Tapia
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  surname: Boehler
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  organization: Department of Physics and Astronomy Rice University, 6100 Main Street, Houston, TX, 77005, USA
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  givenname: P.
  surname: D'Alessio
  fullname: D'Alessio, P.
  organization: Instituto de Radioastronomía y Astrofísica , UNAM, Apartado Postal 3-72, 58089 Morelia, Michoacán, México
BackLink https://www.osti.gov/biblio/22882295$$D View this record in Osti.gov
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Snippet ABSTRACT We model the vertical structure of the magnetized accretion disks that are subject to viscous and resistive heating and irradiation by the central...
We model the vertical structure of the magnetized accretion disks that are subject to viscous and resistive heating and irradiation by the central star. We...
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StartPage 35
SubjectTerms ACCRETION DISKS
accretion, accretion disks
ASPECT RATIO
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
Balances (scales)
COMPARATIVE EVALUATIONS
Disks
EMISSION
Formalism
Heating
Irradiation
ISM: magnetic fields
MAGNETIC FIELDS
MAGNETIZATION
MAGNETOHYDRODYNAMICS
magnetohydrodynamics (MHD)
MASS
protoplanetary disks
PROTOPLANETS
PROTOSTARS
ROTATION
STAR EVOLUTION
STARS
stars: formation
STELLAR ATMOSPHERES
VELOCITY
Title VERTICAL STRUCTURE OF MAGNETIZED ACCRETION DISKS AROUND YOUNG STARS
URI https://iopscience.iop.org/article/10.3847/0004-637X/817/1/35
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https://www.proquest.com/docview/1816036137
https://www.osti.gov/biblio/22882295
Volume 817
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