Accretion and Current Discs Controlled by Strong Magnetic Field
Affiliation(s)
Institute of Nuclear Physics, Moscow State University, Moscow, Russia. Space Research Institute, Austrian Academy of Sciences, Graz, Austria.
Institute of Nuclear Physics, Moscow State University, Moscow, Russia. Space Research Institute, Austrian Academy of Sciences, Graz, Austria.
ABSTRACT
In the presence of a strong magnetic field, accretion discs surrounding neutron stars, black holes, and white dwarfs have their inner edges at their Alfvén radii, i.e., at the distance where magnetic energy density becomes equal to the kinetic energy density. Young stars, X-ray binaries, active galactic nuclei possess discs which could generate jets. Jets arise at the inner boundary of the disc at the Alfvén radius when magnetic field is sufficiently strong. We emphasize here that not only accretion discs possess this feature. The inner edge of the heliospheric current sheet is located at the solar Alfvén radius. The inner edges of the Jovian magnetodisc and Saturnian ring current are also placed close to their Alfvén radii. Thus, in the presence of a strong magnetic field the inner edges of a lot of astrophysical discs are located at Alfvén radii regardless of the nature of their origin, material, and motion direction. This means that discs under such conditions are well described by MHD theory.
In the presence of a strong magnetic field, accretion discs surrounding neutron stars, black holes, and white dwarfs have their inner edges at their Alfvén radii, i.e., at the distance where magnetic energy density becomes equal to the kinetic energy density. Young stars, X-ray binaries, active galactic nuclei possess discs which could generate jets. Jets arise at the inner boundary of the disc at the Alfvén radius when magnetic field is sufficiently strong. We emphasize here that not only accretion discs possess this feature. The inner edge of the heliospheric current sheet is located at the solar Alfvén radius. The inner edges of the Jovian magnetodisc and Saturnian ring current are also placed close to their Alfvén radii. Thus, in the presence of a strong magnetic field the inner edges of a lot of astrophysical discs are located at Alfvén radii regardless of the nature of their origin, material, and motion direction. This means that discs under such conditions are well described by MHD theory.
Cite this paper
E. Belenkaya and M. Khodachenko, "Accretion and Current Discs Controlled by Strong Magnetic Field," International Journal of Astronomy and Astrophysics, Vol. 2 No. 2, 2012, pp. 81-96. doi: 10.4236/ijaa.2012.22012.
E. Belenkaya and M. Khodachenko, "Accretion and Current Discs Controlled by Strong Magnetic Field," International Journal of Astronomy and Astrophysics, Vol. 2 No. 2, 2012, pp. 81-96. doi: 10.4236/ijaa.2012.22012.
References
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Beskin, “Magnetohydrodynamic Models of Astrophysical Jets,” Physics-Uspekhi, Vol. 53, No. 12, 2010, pp. 1241-1278. doi:10.3367/UFNe.0180.201012b.1241 [6] Y. N. Istomin, “Synchrotron Radiation of a Pulsar Wind,” Astrophys and Space Science, Vol. 331, No. 1, 2011, pp. 127-133. doi:10.1007/s10509-010-0421-z [7] A. M. Cherepashchuk, “Highly Evolved Close Binary Stars,” Space Science Reviews, Vol. 74, No. 3-4, 1995, pp. 313-324. doi:10.1007/BF00751417 [8] A. M. Cherepashchuk, “X-Ray Nova Binary Systems,” Space Science Reviews, Vol. 93, No. 3-4, 2000, pp. 473- 580. doi:10.1023/A:1026507625481 [9] A. M. Cherepashchuk, “Observational Manifestations of Precession of Accretion Disk in the SS 433 Binary System,” Space Science Reviews, Vol. 102, No. 1-4, 2002, pp. 23-25. doi:10.1023/A:1021356630889 [10] P. Ghosh and F. K. Lamb, “Accretion by Rotating Magnetic Neutron Stars. III—Accretion Torques and Period Changes in Pulsating X-Ray Sources” The Astrophysical Journal, Vol. 234, 1979, pp. 296-316. doi:10.1086/157498 [11] K. S. Cheng, K. N. Yu and K. Y. Ding, “X-Ray and Gamma-Ray Emission from Active Galactic Nuclei,” Astronomy & Astrophysics, Vol. 275, 1993, pp. 53-60. [12] P. Ghosh and F. K. Lamb, “Accretion by Rotating Magnetic Neutron Stars. II—Radial and Vertical Structure of the Transition Zone in Disk,” The Astrophysical Journal, Vol. 232, 1979, pp. 259-276. doi:10.1086/157285 [13] U. Torkelsson, “Magnetic Torques between Accretion Discs and Stars,” Monthly Notices of the Royal Astronomical Society, Vol. 298, No. 3, 1998, pp. L55-L59. doi:10.1046/j.1365-8711.1998.01927.x [14] X.-D. Li, “Evolution of the Inner Radius of the Accretion Disk in the X-Ray Pulsar A0535+26,” The Astrophysical Journal, Vol. 476, No. 1, 1997, pp. 278-280. doi:10.1086/303624 [15] V. F. 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