Ballooning Modes in Thin Accretion Disks: Limits for their Excitation

Details Ballooning Modes in Thin Accretion Disks: Limits for their Excitation Ballooning Modes in Thin Accretion Disks: Limits for their Excitation

2003-06-17

arxiv.org/abs/astro-ph/0306351v1

Astrophys.J. 595 (2003) 1000-1008

Astronomy and Astrophysics

Astrophysics

25 pages, 7 figures. Accepted to ApJ

Scientific paper

10.1086/377429

The conditions that limit the possible excitation of ideal MHD axisymmetric ballooning modes in thin accretion disks are discussed. As shown earlier by Coppi and Coppi (2001), these modes are well-localized in the vertical direction but have characteristic oscillatory and non-localized profiles in the radial direction. A necessary condition for their excitation is that the magnetic energy be considerably lower than the thermal energy. Even when this is satisfied, there remains the problem of identifying the possible physical factors which can make the considered modes radially localized. The general solution of the normal mode equation describing the modes is given, showing that it is characterized by a discrete spectrum of eigensolutions. The growth rates are reduced and have a different scaling relative to those of the "long-cylinder" modes, commonly known as the Magneto Rotational Instability, that have been previously studied.

Affiliated with

Also associated with

No associations

Rating

Ballooning Modes in Thin Accretion Disks: Limits for their Excitation does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Ballooning Modes in Thin Accretion Disks: Limits for their Excitation, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Ballooning Modes in Thin Accretion Disks: Limits for their Excitation will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-51390