- Young stellar object
Young stellar object (YSO) denotes a star in its early stage of evolution.
This class consists of two groups of objects:
protostars and pre-main sequence stars. Sometimes they are divided by mass - massive YSO (MYSO), intermediate mass YSO and brown dwarfs.
YSO are usually classified using criteria based on the slope of their SED, introduced by Lada C.J. and Wilking B.A. in 1984. They proposed three classes (I, II and III), based on the values of intervals of
Here is frequency, is flux density.
The is calculated in the wavelength interval of 2.2–10 (near infrared region).Later Greene et al. in 1994 added a fourth class of "flat spectrum" class sources. In 1993 Andre et al. discovered class 0—objects with strong submillimeter emission, but very faint at .
*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 birthlineas pre-main sequence stars.
YSO are also associated with early star evolution phenomena:
circumstellar jets and bipolar outflows, masers, Herbig-Haro objects, protoplanetary disks (circumstellar disks or proplyds).
*Lada, C. J.; Wilking, B. A. (1984),"The nature of the embedded population in the Rho Ophiuchi dark cloud - Mid-infrared observations", The Astrophysical Journal, vol. 287, pp. 610-621
*Greene, Thomas P.; Wilking, Bruce A.; Andre, Philippe; Young, Erick T.; Lada, Charles J. (1994), "Further mid-infrared study of the rho Ophiuchi cloud young stellar population: Luminosities and masses of pre-main-sequence stars", The Astrophysical Journal, vol. 434, pp. 614-626
*Andre, Philippe; Ward-Thompson, Derek; Barsony, Mary (1993), "Submillimeter continuum observations of Rho Ophiuchi A - The candidate protostar VLA 1623 and prestellar clumps", The Astrophysical Journal, vol. 406, pp. 122-141
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