Herbig Ae/Be star

Herbig Ae/Be star

A Herbig Ae/Be star (HABe) is a Herbig criteria were:

Nowadays there are several known isolated Herbig Ae/Be stars (i.e. not connected with dark clouds or nebulae). Thus the most reliable criteria now can be:

Sometimes Herbig Ae/Be stars show significant brightness variability. They are believed to be due to clumps (protoplanets and planetesimals) in the circumstellar disk. In the lowest brightness stage the radiation from the star becomes bluer and linearly polarized (when the clump obscures direct star light, scattered from disk light relatively increases – it is the same effect as the blue color of our sky).

Analogs of Herbig Ae/Be stars in the smaller mass range (<2 M) - F, G, K, M spectral type pre-main-sequence stars, are called T Tauri stars. More massive (>8 M) stars in pre-main-sequence stage are not observed, because they evolve very quickly: when they become visible (i.e. disperses surrounding circumstellar gas and dust cloud), the hydrogen in the center is already burning and they are main-sequence objects.

Planets

Planets around Herbig Ae/Be stars include:

References

  1. ^ V. Mannings & A. Sargent (2000) High-resolution studies of gas and dust around young intermediate-mass stars: II. observations of an additional sample of Herbig Ae/Be systems. Astrophysical Journal, vol. 529, p. 391
  • Pérez M.R., Grady C.A. (1997), , Space Science Reviews, Vol 82, p. 407-450Observational Overview of Young Intermediate-Mass Objects: Herbig Ae/Be Stars
  • Waters L. B. F. M., Waelkens, C. (1998), , Annual Review of Astronomy and Astrophysics, Vol. 36, p. 233-266HERBIG Ae/Be STARS
  • Herbig Ae/Be stars
  • "Molecular Hydrogen In The Circumstellar Environment Of Herbig Ae/Be Stars" (PDF). http://www.mpia-hd.mpg.de. Retrieved 2008-10-16.