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Rossby wave instability

(Redirected from Rossby Wave Instability in Astrophysical Discs)

Rossby Wave Instability (RWI) is a concept related to astrophysical accretion 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.[2] The Rossby vortices in the discs around stars and black holes may cause the observed quasi-periodic modulations of the disc's thermal emission.

Rossby wave instability in a Keplerian disk.[1]

Rossby waves, named after Carl-Gustaf Arvid Rossby, are important in planetary atmospheres and oceans and are also known as planetary waves.[3][4][5][6] 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.[7] 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][3]

The theory of the Rossby wave instability in accretion discs was developed by Lovelace et al.[8] and Li et al.[9] for thin Keplerian discs with negligible self-gravity and earlier by Lovelace and Hohlfeld[10] for thin disc galaxies where the self-gravity may or may not be important and where the rotation is in general non-Keplerian.

The Rossby wave instability occurs because of the local wave trapping in a disc. It is related to the Papaloizou and Pringle instability;[11][12] where the wave is trapped between the inner and outer radii of a disc or torus.

References

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  1. ^ Lovelace, R V E.; Romanova, M. M. (2014). "Rossby wave instability in astrophysical discs". Fluid Dynamics Research. 46 (4): 041401. arXiv:1312.4572. Bibcode:2014FlDyR..46d1401L. doi:10.1088/0169-5983/46/4/041401. S2CID 118504602.
  2. ^ a b Lyra, W.; Johansen, J.; Zsom, A.; Klahr, H.; Piskunov, N. (April 2009). "Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks". Astronomy & Astrophysics. 497 (3): 869–888. arXiv:0901.1638. Bibcode:2009A&A...497..869L. doi:10.1051/0004-6361/200811265. S2CID 15820108.
  3. ^ a b Rossby, C.-G. (1939). "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. S2CID 27148455.
  4. ^ Brekhovskikh, Leonid; Goncharov, Valery (1985). "Waves in Rotating Fluids". Mechanics of Continua and Wave Dynamics. Springer Series on Wave Phenomena. Vol. 1. pp. 236–261. doi:10.1007/978-3-642-96861-7_11. ISBN 978-3-642-96863-1.
  5. ^ Chelton, D. B.; Schlax, M. G. (1996). "Global Observations of Oceanic Rossby Waves" (PDF). Science. 272 (5259): 234–238. Bibcode:1996Sci...272..234C. doi:10.1126/science.272.5259.234. S2CID 126953559.
  6. ^ Lindzen, Richard S. (1988). "Instability of plane parallel shear flow (toward a mechanistic picture of how it works)". Pure and Applied Geophysics. 126 (1): 103–121. Bibcode:1988PApGe.126..103L. doi:10.1007/BF00876917. S2CID 128547643.
  7. ^ Marcus, Philip S. (1993). "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.
  8. ^ Lovelace, R. V. E.; Li, H.; Colgate, S. A.; Nelson, A. F. (March 1999). "Rossby Wave Instability of Keplerian Accretion Disks". The Astrophysical Journal. 513 (2): 805–810. arXiv:astro-ph/9809321. Bibcode:1999ApJ...513..805L. doi:10.1086/306900. S2CID 8914218.
  9. ^ Li, H.; Finn, J. M.; Lovelace, R. V. E.; Colgate, S. A. (2000). "Rossby Wave Instability of Thin Accretion Disks. II. Detailed Linear Theory". The Astrophysical Journal. 533 (2): 1023–1034. arXiv:astro-ph/9907279. Bibcode:2000ApJ...533.1023L. doi:10.1086/308693. S2CID 119382697.
  10. ^ Lovelace, R. V. E.; Hohlfeld, R. G. (1978). "Negative mass instability of flat galaxies". The Astrophysical Journal. 221: 51. Bibcode:1978ApJ...221...51L. doi:10.1086/156004.
  11. ^ Papaloizou, J. C. B.; Pringle, J. E. (1984). "The dynamical stability of differentially rotating discs with constant specific angular momentum". Monthly Notices of the Royal Astronomical Society. 208 (4): 721–750. Bibcode:1984MNRAS.208..721P. doi:10.1093/mnras/208.4.721.
  12. ^ Papaloizou, J. C. B.; Pringle, J. E. (1985). "The dynamical stability of differentially rotating discs - II". Monthly Notices of the Royal Astronomical Society. 213 (4): 799–820. Bibcode:1985MNRAS.213..799P. doi:10.1093/mnras/213.4.799.

Further reading

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