Young stellar object
Young stellar object
T Tauri star
Herbig Ae/Be star
|Initial mass function
Classification by mass
These stars may be differentiated by mass: Massive YSOs, intermediate mass YSOs, and brown dwarfs.
Classification by spectral energy distribution
YSOs are usually classified using criteria based on the slope of their spectral energy distribution, introduced by Lada (1987). He proposed three classes (I, II and III), based on the values of intervals of spectral index :
Here is wavelength, and is flux density.
The is calculated in the wavelength interval of 2.2–20 (near- and mid-infrared region). Andre et al. (1993) discovered a class 0: objects with strong submillimeter emission, but very faint at . Greene et al. (1994) added a fifth class of "flat spectrum" sources.
- Class 0 sources – undetectable at
- Class I sources have
- Flat spectrum sources have
- Class II sources have
- Class III sources have
This classification schema roughly reflects evolutionary sequence. It is believed that most deeply embedded Class 0 sources evolve towards Class I stage, dissipating their circumstellar envelopes. Eventually they become optically visible on the stellar birthline as pre-main-sequence stars.
- Lada, Charles J. (1987). "Star Formation: From OB Associations to Protostars". In Peimbert, Manuel; Jugaku, Jun. Star Forming Regions: Proceedings of the 115th Symposium of the International Astronomical Union Held in Tokyo, Japan, November 11–15, 1985. Dordrecht: D. Reidel. pp. 1–17. Bibcode:1987IAUS..115....1L. ISBN 978-90-277-2388-8.
- Andre, Philippe; Ward-Thompson, Derek; Barsony, Mary (March 1993). "Submillimeter Continuum Observations of Ophiuchi A: The Candidate Protostar VLA 1623 and Prestellar Clumps". The Astrophysical Journal, Part 1. 406 (1): 122–141. Bibcode:1993ApJ...406..122A. doi:10.1086/172425.
- Greene, Thomas P.; Wilking, Bruce A.; Andre, Philippe; Young, Erick T.; Lada, Charles J. (October 1994). "Further Mid-infrared Study of the Ophiuchi Cloud Young Stellar Population: Luminosities and Masses of Pre-main-sequence Stars". The Astrophysical Journal, Part 1. 434 (2): 614–626. Bibcode:1994ApJ...434..614G. doi:10.1086/174763.
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