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Abstract: Based on results obtained from the study for MHD (magneto-hydrodynamics) of advective accretion disk, which are applied to real source showing typical values for CBS (close binary star-system), it will investigate on self-structuring in the disk under the impact of the distribution of leading parameters (density, velocity ...). The paper is considering the problem of development of the corona and will analyze the process of interaction of the plasma with the magnetic field in connection to support for the instabilities.
Key words: Accretion disk, advection, MHD (magneto-hydrodynamics) instabilities.
1. Introduction
In a series of papers is developed a model, related to the interaction of the field and the plasma in the accretion disk. Magneto hydrodynamics of accretion flows is investigates. Accretion is qualitatively and quantitatively more effective in the presence of a magnetic field. Instabilities are arising more quickly and they are more diverse. This results in generation of different structures, as vortices, spirals, corona and jets. They are observable in powerful X-ray or/and γ-ray emission and even annihilation lines.
Disks around massive compact objects can not be cooled efficiently by mechanisms in there and disk generated corona. The corona is a macrostructure, which ensures the disk cooling, when the flow in it weakly radiates. It regulates processes in the disk and controls its stability.
Here it will be not discussing our model and his modifications. The aim is to demonstrate applications and using model’s results for typical objects.
References
[1] Kr.D. Iankova, L.G. Filipov, Zones of Action of Instabilities in Disk in Depending on Its Parameters—Formulation of the Problem, Scientific report for Jubilee Scientific Session 2003 “100 years of the flight the Right brothers”, Dolna Metropolia, Bulgaria, Volume 1, 2003, pp. 210-214.
[2] Kr.D. Iankova, L.G. Filipov, Influence of the magnetic field of the compact object on the accretion disk results, Aerospace Research in Bulgaria [Online], 20 (2005) 167-170, http://www.space.bas.bg/astro/Rogen2004/StPh-2.pdf.
[3] Kr.D. Iankova, Accretion disk with advection and magnetic field, Presented at BSSPP Proceedings [Online], Series No. 1, 2007, pp. 143-146, http://sp.phys.uni-sofia.bg/Kiten06/Pres/Iankova.pdf.
[4] Kr.D. Iankova, Generate of corona on magnetized disk, in: International Scientific Conference: Space Ecology Safety, Varna, Bulgaria, June 10-13, 2005.
[5] M.M. Romanova, G.V. Ustyugova, A.V. Koldova, J.V. Wick, R.V.E. Lovelace, Three-dimensional simulations of disk accretion to an inclined dipole: II. hot spots and variability, Astrophys. J. 610 (2004) 920-932.
[6] D. Biskamp, MHD Turbulence, Cambridge University Press, Cambridge, 1993.
[7] S. Fromang, C. Terquem, S.A. Balbus, J.P. de Villiers, Evolution of Massive and Magnetized Protoplanetary Disks, Presented at Proceedings of the XIXth IAP Colloquium “Extrasolar Planets: Today and Tomorrow”[Online], Paris, France, Vol. 321, 2004, p. 262 arXiv: astro-ph/0402373v1.
[8] M. Abramowicz, A. Brandenburg, J.P. Lasota, The dependence of the viscosity in accretion discs on the shear/vorticity ratio, Monthly Notices of the Royal Astronomical Society 281 (1996) L21-L24.
[9] P.J. Armitage, M. Livio, J.E. Pringle, Dynamo-driven accretion disks and dwarf nova eruptions, Astrophys. J. 457 (1996) 332-339.
[10] Kr.D. Yankova, Theoretical modelling of accretion discs: Correlation of the global coefficients with the distributions of local wave numbers in the disc, in: International Conference MSS-09 “Mode Conversion, Coherent Structures and Turbulence”, Moscow, Nov. 23-25, 2009, pp. 409-414.
[11] Kr.D. Yankova, Generation and development of the disk corona, in: Viii Serbian-Bulgarian Astronomical Conference (Viii Sbac) Leskovac, Serbia, May 8-12, 2012.(In Press)
Key words: Accretion disk, advection, MHD (magneto-hydrodynamics) instabilities.
1. Introduction
In a series of papers is developed a model, related to the interaction of the field and the plasma in the accretion disk. Magneto hydrodynamics of accretion flows is investigates. Accretion is qualitatively and quantitatively more effective in the presence of a magnetic field. Instabilities are arising more quickly and they are more diverse. This results in generation of different structures, as vortices, spirals, corona and jets. They are observable in powerful X-ray or/and γ-ray emission and even annihilation lines.
Disks around massive compact objects can not be cooled efficiently by mechanisms in there and disk generated corona. The corona is a macrostructure, which ensures the disk cooling, when the flow in it weakly radiates. It regulates processes in the disk and controls its stability.
Here it will be not discussing our model and his modifications. The aim is to demonstrate applications and using model’s results for typical objects.
References
[1] Kr.D. Iankova, L.G. Filipov, Zones of Action of Instabilities in Disk in Depending on Its Parameters—Formulation of the Problem, Scientific report for Jubilee Scientific Session 2003 “100 years of the flight the Right brothers”, Dolna Metropolia, Bulgaria, Volume 1, 2003, pp. 210-214.
[2] Kr.D. Iankova, L.G. Filipov, Influence of the magnetic field of the compact object on the accretion disk results, Aerospace Research in Bulgaria [Online], 20 (2005) 167-170, http://www.space.bas.bg/astro/Rogen2004/StPh-2.pdf.
[3] Kr.D. Iankova, Accretion disk with advection and magnetic field, Presented at BSSPP Proceedings [Online], Series No. 1, 2007, pp. 143-146, http://sp.phys.uni-sofia.bg/Kiten06/Pres/Iankova.pdf.
[4] Kr.D. Iankova, Generate of corona on magnetized disk, in: International Scientific Conference: Space Ecology Safety, Varna, Bulgaria, June 10-13, 2005.
[5] M.M. Romanova, G.V. Ustyugova, A.V. Koldova, J.V. Wick, R.V.E. Lovelace, Three-dimensional simulations of disk accretion to an inclined dipole: II. hot spots and variability, Astrophys. J. 610 (2004) 920-932.
[6] D. Biskamp, MHD Turbulence, Cambridge University Press, Cambridge, 1993.
[7] S. Fromang, C. Terquem, S.A. Balbus, J.P. de Villiers, Evolution of Massive and Magnetized Protoplanetary Disks, Presented at Proceedings of the XIXth IAP Colloquium “Extrasolar Planets: Today and Tomorrow”[Online], Paris, France, Vol. 321, 2004, p. 262 arXiv: astro-ph/0402373v1.
[8] M. Abramowicz, A. Brandenburg, J.P. Lasota, The dependence of the viscosity in accretion discs on the shear/vorticity ratio, Monthly Notices of the Royal Astronomical Society 281 (1996) L21-L24.
[9] P.J. Armitage, M. Livio, J.E. Pringle, Dynamo-driven accretion disks and dwarf nova eruptions, Astrophys. J. 457 (1996) 332-339.
[10] Kr.D. Yankova, Theoretical modelling of accretion discs: Correlation of the global coefficients with the distributions of local wave numbers in the disc, in: International Conference MSS-09 “Mode Conversion, Coherent Structures and Turbulence”, Moscow, Nov. 23-25, 2009, pp. 409-414.
[11] Kr.D. Yankova, Generation and development of the disk corona, in: Viii Serbian-Bulgarian Astronomical Conference (Viii Sbac) Leskovac, Serbia, May 8-12, 2012.(In Press)