Spectral type is the category to which a star is assigned according to the characteristics of its spectrum. The classification scheme in use today has evolved from that devised at Harvard College Observatory at the end of the ninteenth century in which stars were grouped into 16 classes from A to Q. Advances in stellar astronomy led to many of these original spectral classes being dropped and others rearranged, so that the modern classification scheme (see Table 1) of stellar spectra consists of seven main groups which form a temperature sequence (see stars, temperature of). From hottest to coolest they are: O, B, A, F, G, K, and M.
Each class is characterized by the appearance of certain types of spectral lines and is further subdivided into 10 sub-classes numbered from 0 to 9. The Sun, for example, is assigned the spectral class G2 in the modern Harvard classification, corresponding to a surface temperature of about 5,700°C. Other spectral characteristics, such as the presence of emission lines, are indicated by an additional small letter placed after the spectral type (see Table 2).
In the 1890s, it was realized that stars of a particular spectral type could differ widely in luminosity. As a result, systems of luminosity classification were developed. That used today was introduced in the 1930s (see Table 3).
|Table 1: Main spectral types|
|type||features of spectrum||surface temp. (°C)||color|
|O||Both emission and absorption lines of ionized helium and other highly ionized ions of light elements||30,000 - >50,000||bluish-white|
|B||No emission lines. Absorption line of ionized helium disappears after B5. Neutral helium reaches a max. at B2. Hydrogen becomes more prominent||9,400 - 30,000||bluish-white or white|
|A||Neutral hydrogen lines dominant||6,900 - 9,400||white|
|F||Many lines of neutral and singly-ionized metals such as calcium, iron, chromium, and titanium||5,800 - 6,900||white or yellowish white|
|G||Lines of neutral metals dominate||4,200 - 5,200||yellow giants|
|5,000 - 5,800||yellow main-sequence|
|K||Increasing numbers of lines of neutral metals and bands due to molecules such titanium oxide||3,200 - 4,600||orange giants|
|3,600 - 5,000||orange main-sequence|
|M||Numerous neutral metal lines and prominent molecular bands||<3,000||red giants|
|Table 2: Nonstandard spectral features|
|e||emission lines of hydrogen|
|f||emission lines of helium and neon|
|m||emission lines of metals|
|Table 3: Luminosity classes|
|V||main sequence (dwarfs)|