Astronomy:Lindblad resonance

From HandWiki
Short description: Phenomenon in astrophysics
A diagram showing a wide rectangular cropped view of the right-side of the radius of a satellite's orbit around a planet, along with the radii of its inner (ILR) and outer (OLR) Lindblad resonances. A small portion of the right side of the planet, coloured in yellow, is visible on the left of the diagram. The ILRs are coloured in red, and the OLRs are coloured in blue. The ILRs start from m=2 which is roughly half-way between the planet and the satellite's orbit, and higher order ILRs get closer together as they get arbitrarily close to the satellite's orbital radius. The OLRs start from m=1 which is roughly twice as far away from the planet as the satellite, and higher order OLRs also get closer together as they approach the satellite's orbital radius.
The radii of a satellite's mth inner (ILR) and outer (OLR) Lindblad resonances relative to the satellite's orbit, located at the corotation circle (CC).

A Lindblad resonance, named for the Swedish galactic astronomer Bertil Lindblad,[1] is an orbital resonance in which an object's epicyclic frequency (the rate at which one periapse follows another) is a simple multiple of some forcing frequency. Resonances of this kind tend to increase the object's orbital eccentricity[2] and to cause its longitude of periapse to line up in phase with the forcing. Lindblad resonances drive spiral density waves[3] both in galaxies (where stars are subject to forcing by the spiral arms themselves) and in Saturn's rings (where ring particles are subject to forcing by Saturn's moons).

Lindblad resonances affect stars at such distances from a disc galaxy's centre where the natural frequency of the radial component of a star's orbital velocity is close to the frequency of the gravitational potential maxima encountered during its course through the spiral arms. If a star's orbital speed around the galactic centre is greater than that of the part of the spiral arm through which it is passing, then an inner Lindblad resonance occurs—if smaller, then an outer Lindblad resonance.[4] At an inner resonance, a star's orbital speed is increased, moving the star outwards, and decreased for an outer resonance causing inward movement.

References

  1. ↑ Binney, James; Tremaine, Scott (1988). Galactic dynamics (Princeton series in astrophysics). Princeton University Press. p. 149. ISBN 978-0-691-08445-9. https://books.google.com/books?id=01yNf7mipb0C&pg=PA149. 
  2. ↑ Miyama, Shoken M.; Tomisaka, Kohji; Hanawa, Tomoyuki (1999). Numerical astrophysics: proceedings of the International Conference on Numerical Astrophysics 1998 (NAP98). Springer. p. 162. ISBN 978-0-7923-5566-3. https://books.google.com/books?id=9mvhdGS8nCAC&pg=PA162. 
  3. ↑ Johnstone, D. (2004). Star formation in the interstellar medium: in honor of David Hollenbach, Chris McKee, and Frank Shu. Astronomical Society of the Pa. p. 73. ISBN 978-1-58381-185-6. https://books.google.com/books?id=RpDvAAAAMAAJ. 
  4. ↑ Shu, Frank H. (1992). The Physics of Astrophysics: Gas dynamics. University Science Books. p. 147. ISBN 978-0-935702-65-1. https://books.google.com/books?id=50VYSc56URUC&pg=PA147. 

Further reading

  • Murray, C.D., and S.F. Dermott 1999, Solar System Dynamics (Cambridge: Cambridge University Press).




Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Lindblad_resonance&oldid=3932306"