Yıldız sınıflandırma (astronomi): Revizyonlar arasındaki fark

([[1943]], [[William Wilson Morgan]], [[Phillip C. Keenan]] ve [[Edith Kellman]])(Yerkes Gözlemevi, [[Wisconsin]], [[Amerika Birleşik Devletleri|ABD]])

==Yerkes spectral classification==

 

The '''Yerkes spectral classification''', also called the '''MKK''' system from the authors' initials, is a system of stellar spectral classification introduced in 1943 by [[William Wilson Morgan]], [[Phillip C. Keenan]] and [[Edith Kellman]] from [[Yerkes Observatory]].<ref>Morgan, William Wilson; Keenan, Philip Childs; Kellman, Edith (1943), "An atlas of stellar spectra, with an outline of spectral classification", Chicago, Ill., The University of Chicago press</ref> This classification is based on [[spectral line]]s sensitive to stellar surface gravity which is related to luminosity, as opposed to the Harvard classification which is based on surface temperature. Later, in 1953, after some revisions of list of standard stars and classification criteria, the scheme was named '''MK''' (by William Wilson Morgan and Phillip C. Keenan initials).<ref name="ref_MK">{{Dergi kaynağı