Rossby wave instability in astrophysical discs

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search
Fig. 3. Rossby wave instability in a Keplerian Disk.[1]

Rossby Wave Instability (RWI) is a concept related to astrophysical discs. In non-self-gravitating discs, for example around newly forming stars, the instability can be triggered by an axisymmetric bump, at some radius , in the disc surface mass-density. It gives rise to exponentially growing non-axisymmetric perturbation [, ] in the vicinity of consisting of anticyclonic vortices. These vortices are regions of high pressure and consequently act to trap dust particles which in turn can facilitate planetesimal growth in proto-planetary discs. The Rossby vortices in the discs around stars and black holes may cause the observed quasi-periodic modulations of the disc's thermal emission.

The theory of the Rossby wave instability (RWI) in accretion discs was developed by Lovelace et al.[2] and Li et al.[3] for thin Keplerian discs with negligible self-gravity and earlier by Lovelace and Hohlfeld[4] for thin disc galaxies where the self-gravity may or may not be important and where the rotation is in general non-Keplerian. In the first case the instability can occur if there is an axisymmetric bump (as a function of radius) in the inverse potential vorticity

at some radius , where is the surface mass density of the disc, is the flow velocity of the disc, is the angular velocity of the flow (with the mass of the central star), is the specific entropy of the gas, and is the specific heat ratio. The approximations involve the neglect of the relatively small radial pressure force. Note that is related to the inverse of the vortensity which is defined as . A sketch of a bump in is shown in Figure 1.

Rossby waves, named after Carl-Gustaf Arvid Rossby are important in planetary atmospheres and oceans and are also known as it planetary waves.[5][6][7][8] These waves have a significant role in the transport of heat from equatorial to polar regions of the Earth. They may have a role in the formation of the long-lived ( yr) Great Red Spot on Jupiter which is an anticyclonic vortex.[9] The Rossby waves have the notable property of having the phase velocity opposite to the direction of motion of the atmosphere or disc in the comoving frame of the fluid.[2][6]

Schrödinger-like equation for perturbation[edit]

Fig. 1. Schematic view of the Rossby wave instability with the two propagating regions for the Rossby waves, and in between the evanescent regions close to the inner and outer Lindblad resonant radii, ( and ), respectively.[10] The radii of these Lindblad resonances are given by the equations , where is the radial epicyclic frequency which is approximately equal to for a Keplerian disc. The corotation radius is the radius where .

Linearization of the Euler and continuity equations for a thin fluid disc with perturbations proportional to (with azimuthal mode number and angular frequency ) leads to a Schrödinger-like equation for the enthalpy perturbation ,

The effective potential well is closely related to : If the height of the bump in is too small the potential well is shallow and there are no 'bound Rossby wave states' in the well. On the other hand, for a sufficiently large bump in the potential is sufficiently deep to have a bound state. The condition for there to be just one bound state allows one to solve for the imaginary part of the wave frequency, which is the growth rate of the instability.[2]

For moderate strength bumps (with fractional amplitudes ), the growth rates are of the order of . The real part of the wave frequency is approximately . A more complete analysis[11][12][13] reveals that the Rossby wave is not completely trapped in the potential well , but leaks outward across a forbidden region at an outer Lindblad resonance (at indicated in Figure 1) and inward across another forbidden region at an inner Lindblad resonance (at ). Once the waves cross the forbidden regions they propagate as spiral density wave. The full expression for the effective potential for a thin homentropic ( const) disc is

where is the Doppler shifted wave frequency in the reference frame moving with the disc matter, is the sound speed in the disc, and is the radial epicyclic angular frequency, with and the specific angular momentum.[10]

Fig. 2. Effective potential for a Gaussian surface density bump of peak amplitude and width for (upper panel) and (lower panel).[10] Waves can propagate only in the regions where . The large positive values of occur at the inner and outer Lindblad resonance radii.

Figure 2 shows the effective potential for sample cases. Note that the inward propagating waves with have negative energy () whereas the outward propagating waves with have positive energy ().[10]

The Rossby wave instability occurs because of the local wave trapping in a disc. It is related to the Papaloizou and Pringle instability;[14][15] where the wave is trapped between the inner and outer radii of a disc or torus.


  1. ^ "Rossby wave instability in astrophysical discs". Fluid Dynamics Research. 46: 041401. arXiv:1312.4572Freely accessible. Bibcode:2014FlDyR..46d1401L. doi:10.1088/0169-5983/46/4/041401. 
  2. ^ a b c "Rossby Wave Instability of Keplerian Accretion Disks". The Astrophysical Journal. 513: 805–810. arXiv:astro-ph/9809321Freely accessible. Bibcode:1999ApJ...513..805L. doi:10.1086/306900. 
  3. ^ "Rossby Wave Instability of Thin Accretion Disks. II. Detailed Linear Theory". The Astrophysical Journal. 533: 1023–1034. arXiv:astro-ph/9907279Freely accessible. Bibcode:2000ApJ...533.1023L. doi:10.1086/308693. 
  4. ^ "Negative mass instability of flat galaxies". The Astrophysical Journal. 221: 51. Bibcode:1978ApJ...221...51L. doi:10.1086/156004. 
  5. ^ "Relation between variations in the intensity of the zonal circulation of the atmosphere and the displacements of the semi-permanent centers of action". Journal of Marine Research. 2: 38–55. doi:10.1357/002224039806649023. 
  6. ^ a b "Mechanics of continua and wave dynamics". Springer Series on Wave Phenomena. 1. 1985. Bibcode:1985SSWP....1.....B. 
  7. ^ "Global Observations of Oceanic Rossby Waves" (PDF). Science. 272: 234–238. Bibcode:1996Sci...272..234C. doi:10.1126/science.272.5259.234. 
  8. ^ "Instability of plane parallel shear flow (toward a mechanistic picture of how it works)". Pure and Applied Geophysics. 126: 103–121. Bibcode:1988PApGe.126..103L. doi:10.1007/BF00876917. 
  9. ^ "Jupiter's Great Red Spot and Other Vortices". Annual Review of Astronomy and Astrophysics. 31: 523–569. Bibcode:1993ARA&A..31..523M. doi:10.1146/annurev.aa.31.090193.002515. 
  10. ^ a b c d "How strong are the Rossby vortices?". Monthly Notices of the Royal Astronomical Society. 430: 1988–1993. arXiv:1301.0689Freely accessible. Bibcode:2013MNRAS.430.1988M. doi:10.1093/mnras/stt022. 
  11. ^ "On Rossby waves and vortices with differential rotation". Astronomy and Astrophysics. 380: 750–757. arXiv:astro-ph/0110298Freely accessible. Bibcode:2001A&A...380..750T. doi:10.1051/0004-6361:20011423. 
  12. ^ "Super-reflection in fluid discs: corotation amplifier, corotation resonance, Rossby waves and overstable modes". Monthly Notices of the Royal Astronomical Society. 387: 446–462. arXiv:0710.2313Freely accessible. Bibcode:2008MNRAS.387..446T. doi:10.1111/j.1365-2966.2008.13252.x. 
  13. ^ "Corotational instability of inertial-acoustic modes in black hole accretion discs and quasi-periodic oscillations". Monthly Notices of the Royal Astronomical Society. 393: 979–991. arXiv:0810.0203Freely accessible. Bibcode:2009MNRAS.393..979L. doi:10.1111/j.1365-2966.2008.14218.x. 
  14. ^ "The dynamical stability of differentially rotating discs with constant specific angular momentum". Monthly Notices of the Royal Astronomical Society. 208: 721–750. Bibcode:1984MNRAS.208..721P. doi:10.1093/mnras/208.4.721. 
  15. ^ "The dynamical stability of differentially rotating discs - II". Monthly Notices of the Royal Astronomical Society. 213: 799–820. Bibcode:1985MNRAS.213..799P. doi:10.1093/mnras/213.4.799. 

Further reading[edit]