Rossiter–McLaughlin effect

From Wikipedia, the free encyclopedia
  (Redirected from Rossiter-McLaughlin effect)
Jump to: navigation, search

The Rossiter–McLaughlin effect is a spectroscopic phenomenon observed when either an eclipsing binary's secondary star or an extrasolar planet is seen to transit across the face of the primary or parent star. As the main star rotates on its axis, one quadrant of its photosphere will be seen to be coming towards the viewer, and the other visible quadrant to be moving away. These motions produce blueshifts and redshifts, respectively, in the star's spectrum, usually observed as a broadening of the spectral lines. When the secondary star or planet transits the primary, it blocks part of the latter's disc, preventing some of the shifted light from reaching the observer. This causes the observed mean redshift of the primary star as a whole to vary from its normal value. As the transiting object moves across to the other side of the star's disc, the redshift anomaly will switch from being negative to being positive, or vice versa. This effect has been used to show that as many as 25% of hot Jupiters are orbiting in a retrograde direction with respect to their parent stars,[1] strongly suggesting that dynamical interactions rather than planetary migration produce these objects.

Illustration showing the effect. The viewer is situated at the bottom. Light from the anticlockwise-rotating star is blue-shifted on the approaching side, and red-shifted on the receding side. As the planet passes in front of the star it sequentially blocks blue- and red-shifted light, causing the star's apparent radial velocity to change when it in fact does not.

History[edit]

J. R. Holt in 1893 proposed a method to measure the stellar rotation of stars using radial velocity measurements, he predicted that when one star of an eclipsing binary eclipsed the other it would first cover the advancing blueshifted half and then the receding redshifted half. This motion would create a redshift of the eclipsed star’s spectrum followed by a blueshift, thus appearing as a change in the radial velocity in addition to that caused by the orbital motion of the eclipsed star.[2]

Further reading[edit]

See also[edit]

References[edit]

  1. ^ Triaud, A. H. M. J.; et al. (2010). "Spin-orbit angle measurements for six southern transiting planets: New insights into the dynamical origins of hot Jupiters". Astronomy & Astrophysics 524: A25. arXiv:1008.2353. Bibcode:2010A&A...524A..25T. doi:10.1051/0004-6361/201014525. 
  2. ^ Triaud, A. H. M. J. et al. (2013). "The EBLM project I. Physical and orbital parameters, including spin-orbit angles, of two low-mass eclipsing binaries on opposite sides of the brown dwarf limit". Astronomy and Astrophysics 549. A18. arXiv:1208.4940. Bibcode:2013A&A...549A..18T. doi:10.1051/0004-6361/201219643.