A two-dimensional study for cooling and self-gravitating accretion discs
Abstract The importance of cooling for the structure and evolution of self-gravitating accretion discs has been confirmed through the use of direct numerical simulations. In this paper, we present a two-dimensional study for self-gravitating accretion discs, to investigate the influence of the cooli...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Faghei, Kazem [verfasserIn] |
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| Format: |
Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2014 |
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| Schlagwörter: |
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| Anmerkung: |
© Springer Science+Business Media Dordrecht 2014 |
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| Übergeordnetes Werk: |
Enthalten in: Astrophysics and space science - Springer Netherlands, 1968, 353(2014), 2 vom: 01. Okt., Seite 641-649 |
|---|---|
| Übergeordnetes Werk: |
volume:353 ; year:2014 ; number:2 ; day:01 ; month:10 ; pages:641-649 |
| Links: |
|---|
| DOI / URN: |
10.1007/s10509-014-2035-3 |
|---|
| Katalog-ID: |
OLC2066275581 |
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| 245 | 1 | 0 | |a A two-dimensional study for cooling and self-gravitating accretion discs |
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| 520 | |a Abstract The importance of cooling for the structure and evolution of self-gravitating accretion discs has been confirmed through the use of direct numerical simulations. In this paper, we present a two-dimensional study for self-gravitating accretion discs, to investigate the influence of the cooling rate on the latitudinal structure of such accretion discs. The disc is cooled using a simple parametrization for the cooling function, (de/dt)cool=−e/tcool with e as the internal energy and tcool as the cooling timescale. The cooling timescale is in units of the dynamical timescale, tdyn[=Ω−1], is Ωtcool=β, where β is a free parameter. The mechanism of energy dissipation is assumed to be turbulent viscosity in the disc and an α-prescription is applied for the kinematic coefficient of viscosity. To study the gravitational stability of the self-gravitating disc, we use the Toomre parameter. We obtain the radial dependence of the physical variables through the use of a self-similar method and we numerically solve the equations to obtain the latitudinal dependence of the physical variables. The solutions show that the radial velocity is smaller than the Keplerian rotational velocity; however, the disc, dependent on the values of parameters α and β and only near the zone close to the equatorial plane, can rotate in a super-Keplerian manner. With the magnitude of both parameters α and β, the disc thickness increases due to the increase of the vertical pressure gradient. The dependence of the gas density on the parameters α and β indicates two zones in the accretion disc. In the first zone near the equatorial plane, the mass density decreases by increasing these parameters. However, in the second zone, the regions with higher latitude, the mass density increases with the magnitude of parameters α and β. | ||
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10.1007/s10509-014-2035-3 doi (DE-627)OLC2066275581 (DE-He213)s10509-014-2035-3-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Faghei, Kazem verfasserin aut A two-dimensional study for cooling and self-gravitating accretion discs 2014 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2014 Abstract The importance of cooling for the structure and evolution of self-gravitating accretion discs has been confirmed through the use of direct numerical simulations. In this paper, we present a two-dimensional study for self-gravitating accretion discs, to investigate the influence of the cooling rate on the latitudinal structure of such accretion discs. The disc is cooled using a simple parametrization for the cooling function, (de/dt)cool=−e/tcool with e as the internal energy and tcool as the cooling timescale. The cooling timescale is in units of the dynamical timescale, tdyn[=Ω−1], is Ωtcool=β, where β is a free parameter. The mechanism of energy dissipation is assumed to be turbulent viscosity in the disc and an α-prescription is applied for the kinematic coefficient of viscosity. To study the gravitational stability of the self-gravitating disc, we use the Toomre parameter. We obtain the radial dependence of the physical variables through the use of a self-similar method and we numerically solve the equations to obtain the latitudinal dependence of the physical variables. The solutions show that the radial velocity is smaller than the Keplerian rotational velocity; however, the disc, dependent on the values of parameters α and β and only near the zone close to the equatorial plane, can rotate in a super-Keplerian manner. With the magnitude of both parameters α and β, the disc thickness increases due to the increase of the vertical pressure gradient. The dependence of the gas density on the parameters α and β indicates two zones in the accretion disc. In the first zone near the equatorial plane, the mass density decreases by increasing these parameters. However, in the second zone, the regions with higher latitude, the mass density increases with the magnitude of parameters α and β. Accretion Accretion discs Planetary systems: protoplanetary discs Planetary systems: formation Pak, Milad aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 353(2014), 2 vom: 01. Okt., Seite 641-649 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:353 year:2014 number:2 day:01 month:10 pages:641-649 https://doi.org/10.1007/s10509-014-2035-3 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 353 2014 2 01 10 641-649 |
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10.1007/s10509-014-2035-3 doi (DE-627)OLC2066275581 (DE-He213)s10509-014-2035-3-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Faghei, Kazem verfasserin aut A two-dimensional study for cooling and self-gravitating accretion discs 2014 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2014 Abstract The importance of cooling for the structure and evolution of self-gravitating accretion discs has been confirmed through the use of direct numerical simulations. In this paper, we present a two-dimensional study for self-gravitating accretion discs, to investigate the influence of the cooling rate on the latitudinal structure of such accretion discs. The disc is cooled using a simple parametrization for the cooling function, (de/dt)cool=−e/tcool with e as the internal energy and tcool as the cooling timescale. The cooling timescale is in units of the dynamical timescale, tdyn[=Ω−1], is Ωtcool=β, where β is a free parameter. The mechanism of energy dissipation is assumed to be turbulent viscosity in the disc and an α-prescription is applied for the kinematic coefficient of viscosity. To study the gravitational stability of the self-gravitating disc, we use the Toomre parameter. We obtain the radial dependence of the physical variables through the use of a self-similar method and we numerically solve the equations to obtain the latitudinal dependence of the physical variables. The solutions show that the radial velocity is smaller than the Keplerian rotational velocity; however, the disc, dependent on the values of parameters α and β and only near the zone close to the equatorial plane, can rotate in a super-Keplerian manner. With the magnitude of both parameters α and β, the disc thickness increases due to the increase of the vertical pressure gradient. The dependence of the gas density on the parameters α and β indicates two zones in the accretion disc. In the first zone near the equatorial plane, the mass density decreases by increasing these parameters. However, in the second zone, the regions with higher latitude, the mass density increases with the magnitude of parameters α and β. Accretion Accretion discs Planetary systems: protoplanetary discs Planetary systems: formation Pak, Milad aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 353(2014), 2 vom: 01. Okt., Seite 641-649 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:353 year:2014 number:2 day:01 month:10 pages:641-649 https://doi.org/10.1007/s10509-014-2035-3 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 353 2014 2 01 10 641-649 |
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10.1007/s10509-014-2035-3 doi (DE-627)OLC2066275581 (DE-He213)s10509-014-2035-3-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Faghei, Kazem verfasserin aut A two-dimensional study for cooling and self-gravitating accretion discs 2014 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2014 Abstract The importance of cooling for the structure and evolution of self-gravitating accretion discs has been confirmed through the use of direct numerical simulations. In this paper, we present a two-dimensional study for self-gravitating accretion discs, to investigate the influence of the cooling rate on the latitudinal structure of such accretion discs. The disc is cooled using a simple parametrization for the cooling function, (de/dt)cool=−e/tcool with e as the internal energy and tcool as the cooling timescale. The cooling timescale is in units of the dynamical timescale, tdyn[=Ω−1], is Ωtcool=β, where β is a free parameter. The mechanism of energy dissipation is assumed to be turbulent viscosity in the disc and an α-prescription is applied for the kinematic coefficient of viscosity. To study the gravitational stability of the self-gravitating disc, we use the Toomre parameter. We obtain the radial dependence of the physical variables through the use of a self-similar method and we numerically solve the equations to obtain the latitudinal dependence of the physical variables. The solutions show that the radial velocity is smaller than the Keplerian rotational velocity; however, the disc, dependent on the values of parameters α and β and only near the zone close to the equatorial plane, can rotate in a super-Keplerian manner. With the magnitude of both parameters α and β, the disc thickness increases due to the increase of the vertical pressure gradient. The dependence of the gas density on the parameters α and β indicates two zones in the accretion disc. In the first zone near the equatorial plane, the mass density decreases by increasing these parameters. However, in the second zone, the regions with higher latitude, the mass density increases with the magnitude of parameters α and β. Accretion Accretion discs Planetary systems: protoplanetary discs Planetary systems: formation Pak, Milad aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 353(2014), 2 vom: 01. Okt., Seite 641-649 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:353 year:2014 number:2 day:01 month:10 pages:641-649 https://doi.org/10.1007/s10509-014-2035-3 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 353 2014 2 01 10 641-649 |
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10.1007/s10509-014-2035-3 doi (DE-627)OLC2066275581 (DE-He213)s10509-014-2035-3-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Faghei, Kazem verfasserin aut A two-dimensional study for cooling and self-gravitating accretion discs 2014 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2014 Abstract The importance of cooling for the structure and evolution of self-gravitating accretion discs has been confirmed through the use of direct numerical simulations. In this paper, we present a two-dimensional study for self-gravitating accretion discs, to investigate the influence of the cooling rate on the latitudinal structure of such accretion discs. The disc is cooled using a simple parametrization for the cooling function, (de/dt)cool=−e/tcool with e as the internal energy and tcool as the cooling timescale. The cooling timescale is in units of the dynamical timescale, tdyn[=Ω−1], is Ωtcool=β, where β is a free parameter. The mechanism of energy dissipation is assumed to be turbulent viscosity in the disc and an α-prescription is applied for the kinematic coefficient of viscosity. To study the gravitational stability of the self-gravitating disc, we use the Toomre parameter. We obtain the radial dependence of the physical variables through the use of a self-similar method and we numerically solve the equations to obtain the latitudinal dependence of the physical variables. The solutions show that the radial velocity is smaller than the Keplerian rotational velocity; however, the disc, dependent on the values of parameters α and β and only near the zone close to the equatorial plane, can rotate in a super-Keplerian manner. With the magnitude of both parameters α and β, the disc thickness increases due to the increase of the vertical pressure gradient. The dependence of the gas density on the parameters α and β indicates two zones in the accretion disc. In the first zone near the equatorial plane, the mass density decreases by increasing these parameters. However, in the second zone, the regions with higher latitude, the mass density increases with the magnitude of parameters α and β. Accretion Accretion discs Planetary systems: protoplanetary discs Planetary systems: formation Pak, Milad aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 353(2014), 2 vom: 01. Okt., Seite 641-649 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:353 year:2014 number:2 day:01 month:10 pages:641-649 https://doi.org/10.1007/s10509-014-2035-3 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 353 2014 2 01 10 641-649 |
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10.1007/s10509-014-2035-3 doi (DE-627)OLC2066275581 (DE-He213)s10509-014-2035-3-p DE-627 ger DE-627 rakwb eng 520 530 620 VZ 16,12 ssgn Faghei, Kazem verfasserin aut A two-dimensional study for cooling and self-gravitating accretion discs 2014 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Springer Science+Business Media Dordrecht 2014 Abstract The importance of cooling for the structure and evolution of self-gravitating accretion discs has been confirmed through the use of direct numerical simulations. In this paper, we present a two-dimensional study for self-gravitating accretion discs, to investigate the influence of the cooling rate on the latitudinal structure of such accretion discs. The disc is cooled using a simple parametrization for the cooling function, (de/dt)cool=−e/tcool with e as the internal energy and tcool as the cooling timescale. The cooling timescale is in units of the dynamical timescale, tdyn[=Ω−1], is Ωtcool=β, where β is a free parameter. The mechanism of energy dissipation is assumed to be turbulent viscosity in the disc and an α-prescription is applied for the kinematic coefficient of viscosity. To study the gravitational stability of the self-gravitating disc, we use the Toomre parameter. We obtain the radial dependence of the physical variables through the use of a self-similar method and we numerically solve the equations to obtain the latitudinal dependence of the physical variables. The solutions show that the radial velocity is smaller than the Keplerian rotational velocity; however, the disc, dependent on the values of parameters α and β and only near the zone close to the equatorial plane, can rotate in a super-Keplerian manner. With the magnitude of both parameters α and β, the disc thickness increases due to the increase of the vertical pressure gradient. The dependence of the gas density on the parameters α and β indicates two zones in the accretion disc. In the first zone near the equatorial plane, the mass density decreases by increasing these parameters. However, in the second zone, the regions with higher latitude, the mass density increases with the magnitude of parameters α and β. Accretion Accretion discs Planetary systems: protoplanetary discs Planetary systems: formation Pak, Milad aut Enthalten in Astrophysics and space science Springer Netherlands, 1968 353(2014), 2 vom: 01. Okt., Seite 641-649 (DE-627)129062723 (DE-600)629-4 (DE-576)014393522 0004-640X nnns volume:353 year:2014 number:2 day:01 month:10 pages:641-649 https://doi.org/10.1007/s10509-014-2035-3 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-TEC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_40 GBV_ILN_47 GBV_ILN_70 GBV_ILN_2279 GBV_ILN_4012 AR 353 2014 2 01 10 641-649 |
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A two-dimensional study for cooling and self-gravitating accretion discs |
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A two-dimensional study for cooling and self-gravitating accretion discs |
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Faghei, Kazem |
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Faghei, Kazem Pak, Milad |
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a two-dimensional study for cooling and self-gravitating accretion discs |
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A two-dimensional study for cooling and self-gravitating accretion discs |
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Abstract The importance of cooling for the structure and evolution of self-gravitating accretion discs has been confirmed through the use of direct numerical simulations. In this paper, we present a two-dimensional study for self-gravitating accretion discs, to investigate the influence of the cooling rate on the latitudinal structure of such accretion discs. The disc is cooled using a simple parametrization for the cooling function, (de/dt)cool=−e/tcool with e as the internal energy and tcool as the cooling timescale. The cooling timescale is in units of the dynamical timescale, tdyn[=Ω−1], is Ωtcool=β, where β is a free parameter. The mechanism of energy dissipation is assumed to be turbulent viscosity in the disc and an α-prescription is applied for the kinematic coefficient of viscosity. To study the gravitational stability of the self-gravitating disc, we use the Toomre parameter. We obtain the radial dependence of the physical variables through the use of a self-similar method and we numerically solve the equations to obtain the latitudinal dependence of the physical variables. The solutions show that the radial velocity is smaller than the Keplerian rotational velocity; however, the disc, dependent on the values of parameters α and β and only near the zone close to the equatorial plane, can rotate in a super-Keplerian manner. With the magnitude of both parameters α and β, the disc thickness increases due to the increase of the vertical pressure gradient. The dependence of the gas density on the parameters α and β indicates two zones in the accretion disc. In the first zone near the equatorial plane, the mass density decreases by increasing these parameters. However, in the second zone, the regions with higher latitude, the mass density increases with the magnitude of parameters α and β. © Springer Science+Business Media Dordrecht 2014 |
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Abstract The importance of cooling for the structure and evolution of self-gravitating accretion discs has been confirmed through the use of direct numerical simulations. In this paper, we present a two-dimensional study for self-gravitating accretion discs, to investigate the influence of the cooling rate on the latitudinal structure of such accretion discs. The disc is cooled using a simple parametrization for the cooling function, (de/dt)cool=−e/tcool with e as the internal energy and tcool as the cooling timescale. The cooling timescale is in units of the dynamical timescale, tdyn[=Ω−1], is Ωtcool=β, where β is a free parameter. The mechanism of energy dissipation is assumed to be turbulent viscosity in the disc and an α-prescription is applied for the kinematic coefficient of viscosity. To study the gravitational stability of the self-gravitating disc, we use the Toomre parameter. We obtain the radial dependence of the physical variables through the use of a self-similar method and we numerically solve the equations to obtain the latitudinal dependence of the physical variables. The solutions show that the radial velocity is smaller than the Keplerian rotational velocity; however, the disc, dependent on the values of parameters α and β and only near the zone close to the equatorial plane, can rotate in a super-Keplerian manner. With the magnitude of both parameters α and β, the disc thickness increases due to the increase of the vertical pressure gradient. The dependence of the gas density on the parameters α and β indicates two zones in the accretion disc. In the first zone near the equatorial plane, the mass density decreases by increasing these parameters. However, in the second zone, the regions with higher latitude, the mass density increases with the magnitude of parameters α and β. © Springer Science+Business Media Dordrecht 2014 |
| abstract_unstemmed |
Abstract The importance of cooling for the structure and evolution of self-gravitating accretion discs has been confirmed through the use of direct numerical simulations. In this paper, we present a two-dimensional study for self-gravitating accretion discs, to investigate the influence of the cooling rate on the latitudinal structure of such accretion discs. The disc is cooled using a simple parametrization for the cooling function, (de/dt)cool=−e/tcool with e as the internal energy and tcool as the cooling timescale. The cooling timescale is in units of the dynamical timescale, tdyn[=Ω−1], is Ωtcool=β, where β is a free parameter. The mechanism of energy dissipation is assumed to be turbulent viscosity in the disc and an α-prescription is applied for the kinematic coefficient of viscosity. To study the gravitational stability of the self-gravitating disc, we use the Toomre parameter. We obtain the radial dependence of the physical variables through the use of a self-similar method and we numerically solve the equations to obtain the latitudinal dependence of the physical variables. The solutions show that the radial velocity is smaller than the Keplerian rotational velocity; however, the disc, dependent on the values of parameters α and β and only near the zone close to the equatorial plane, can rotate in a super-Keplerian manner. With the magnitude of both parameters α and β, the disc thickness increases due to the increase of the vertical pressure gradient. The dependence of the gas density on the parameters α and β indicates two zones in the accretion disc. In the first zone near the equatorial plane, the mass density decreases by increasing these parameters. However, in the second zone, the regions with higher latitude, the mass density increases with the magnitude of parameters α and β. © Springer Science+Business Media Dordrecht 2014 |
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A two-dimensional study for cooling and self-gravitating accretion discs |
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