In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Electromagnetic radiation from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with absorption lines. Each line indicates an ion of a certain chemical element, with the line strength indicating the abundance of that ion. The relative abundance of the different ions varies with the temperature of the photosphere. The spectral class of a star is a short code summarizing the ionization state, giving an objective measure of the photosphere's temperature and density.
Most stars are currently classified under the Morgan–Keenan (MK) system using the letters O, B, A, F, G, K, and M, a sequence from the hottest (O type) to the coolest (M type). Each letter class is then subdivided using a numeric digit with 0 being hottest and 9 being coolest (e.g. A8, A9, F0, F1 form a sequence from hotter to cooler). The sequence has been expanded with classes for other stars and star-like objects that do not fit in the classical system, such as class D for white dwarfs and class C for carbon stars.
In the MK system, a luminosity class is added to the spectral class using Roman numerals. This is based on the width of certain absorption lines in the star's spectrum, which vary with the density of the atmosphere and so distinguish giant stars from dwarfs. Luminosity class 0 or Ia+ stars for hypergiants, class I stars for supergiants, class II for bright giants, class III for regular giants, class IV for sub-giants, class V for main-sequence stars, class sd for sub-dwarfs, and class D for white dwarfs. The full spectral class for the Sun is then G2V, indicating a main-sequence star with a temperature around 5,800 K.
- 1 Conventional color description
- 2 Modern classification
- 3 History
- 4 Spectral types
- 5 Extended spectral types
- 5.1 Hot blue emission star classes
- 5.2 Cool red and brown dwarf classes
- 5.3 Carbon-related late giant-star classes
- 5.4 White dwarf classifications
- 6 Stellar remnants
- 7 See also
- 8 Notes
- 9 References
- 10 External links
Conventional color description
The conventional color description takes into account only the peak of the stellar spectrum. However, in actuality stars radiate in all parts of the spectrum, and because all spectral colors combined appear white, the actual apparent colors the human eye would observe are lighter than the conventional color descriptions. This means that the simplified assignment of colors of the spectrum can be misleading. There are no green, indigo, or violet stars. Likewise, the "brown" dwarfs do not literally appear brown.
The modern classification system is known as the Morgan–Keenan (MK) classification. Each star is assigned a spectral class from the older Harvard spectral classification and a luminosity class using Roman numerals as explained below, forming the star's spectral type.
Harvard spectral classification
The Harvard classification system is a one-dimensional classification scheme using single letters of the alphabet, optionally with numeric subdivisions, to group stars according to their spectral characteristics. Main-sequence stars vary in surface temperature from approximately 2,000 to 50,000 K, whereas more-evolved stars can have temperatures above 100,000 K. Physically, the classes indicate the temperature of the star's atmosphere and are normally listed from hottest to coldest.
|Class||Effective temperature||Vega-relative chromaticity[nb 1]||Chromaticity (D65)[nb 2]||Main-sequence mass
|Fraction of all
|O||≥ 30,000 K||blue||blue||≥ 16 M☉||≥ 6.6 R☉||≥ 30,000 L☉||Weak||~0.00003%|
|B||10,000–30,000 K||blue white||deep blue white||2.1–16 M☉||1.8–6.6 R☉||25–30,000 L☉||Medium||0.13%|
|A||7,500–10,000 K||white||blue white||1.4–2.1 M☉||1.4–1.8 R☉||5–25 L☉||Strong||0.6%|
|F||6,000–7,500 K||yellow white||white||1.04–1.4 M☉||1.15–1.4 R☉||1.5–5 L☉||Medium||3%|
|G||5,200–6,000 K||yellow||yellowish white||0.8–1.04 M☉||0.96–1.15 R☉||0.6–1.5 L☉||Weak||7.6%|
|K||3,700–5,200 K||light orange||pale yellow orange||0.45–0.8 M☉||0.7–0.96 R☉||0.08–0.6 L☉||Very weak||12.1%|
|M||2,400–3,700 K||orange red||light orange red||0.08–0.45 M☉||≤ 0.7 R☉||≤ 0.08 L☉||Very weak||76.45%|
The spectral classes O through M, as well as other more specialized classes discussed later, are subdivided by Arabic numerals (0–9), where 0 denotes the hottest stars of a given class. For example, A0 denotes the hottest stars in the A class and A9 denotes the coolest ones. Fractional numbers are allowed; for example, the star Mu Normae is classified as O9.7. The Sun is classified as G2.
The conventional color descriptions are traditional in astronomy, and represent colors relative to the mean color of an A-class star, which is considered to be white. The apparent color descriptions are what the observer would see if trying to describe the stars under a dark sky without aid to the eye, or with binoculars. However, most stars in the sky, except the brightest ones, appear white or bluish white to the unaided eye because they are too dim for color vision to work. Red supergiants are cooler and redder than dwarfs of the same spectral type, and stars with particular spectral features such as carbon stars may be far redder than any black body.
The fact that the Harvard classification of a star indicated its surface or photospheric temperature (or more precisely, its effective temperature) was not fully understood until after its development, though by the time the first Hertzsprung–Russell diagram was formulated (by 1914), this was generally suspected to be true. In the 1920s, the Bengali physicist Meghnad Saha derived a theory of ionization by extending well-known ideas in physical chemistry pertaining to the dissociation of molecules to the ionization of atoms. First he applied it to the solar chromosphere, then to stellar spectra. The Harvard astronomer Cecilia Helena Payne (later to become Cecilia Payne-Gaposchkin) then demonstrated that the OBAFGKM spectral sequence is actually a sequence in temperature. Because the classification sequence predates our understanding that it is a temperature sequence, the placement of a spectrum into a given subtype, such as B3 or A7, depends upon (largely subjective) estimates of the strengths of absorption features in stellar spectra. As a result, these subtypes are not evenly divided into any sort of mathematically representable intervals.
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, Philip C. Keenan, and Edith Kellman from Yerkes Observatory. This two-dimensional (temperature and luminosity) classification scheme is based on spectral lines sensitive to stellar temperature and surface gravity, which is related to luminosity (whilst the Harvard classification is based on just surface temperature). Later, in 1953, after some revisions of list of standard stars and classification criteria, the scheme was named the Morgan–Keenan classification, or MK (by William Wilson Morgan and Philip C. Keenan's initials), and this system remains the system in modern use today.
Denser stars with higher surface gravity exhibit greater pressure broadening of spectral lines. The gravity, and hence the pressure, on the surface of a giant star is much lower than for a dwarf star because the radius of the giant is much greater than a dwarf of similar mass. Therefore, differences in the spectrum can be interpreted as luminosity effects and a luminosity class can be assigned purely from examination of the spectrum.
A number of different luminosity classes are distinguished
- 0 or Ia+ (hypergiants or extremely luminous supergiants). Example: Cygnus OB2#12 (B3-4Ia+)
- Ia (luminous supergiants). Example: Eta Canis Majoris (B5Ia)
- Iab (intermediate luminous supergiants). Example: Gamma Cygni (F8Iab)
- Ib (less luminous supergiants). Example: Zeta Persei (B1Ib)
- II bright giants. Example: Beta Leporis (G0II)
- III normal giants. Example: Arcturus (K0III)
- IV subgiants. Example: Gamma Cassiopeiae (B0.5IVpe)
- V main-sequence stars (dwarfs). Example: Achernar (B6Vep)
- sd (prefix) subdwarfs. Example: HD 149382 (sdB5)
- D (prefix) white dwarfs.[nb 3] Example: van Maanen 2 (DZ8)
Marginal cases are allowed; for example, a star may be either a supergiant or a bright giant, or may be in between the subgiant and main-sequence classifications. In these cases, two special symbols are used: a slash (/) means that a star is either one class or the other, and a dash (-) means that the star is in between the two classes. For example, a star classified as A3-4III/IV would be in between spectral types A3 and A4, while being either a giant star or a subgiant. Sub-dwarf classes have also been used: VI for sub-dwarfs, stars slightly less luminous than the main sequence; VII and sometimes higher numerals for white dwarf or "hot sub-dwarf" classes.
Additional nomenclature, in the form of lower-case letters, can follow the spectral type to indicate peculiar features of the spectrum.
|Code||Spectral peculiarities for stars|
|:||uncertain spectral value|
|...||Undescribed spectral peculiarities exist|
|e||Emission lines present|
|[e]||"Forbidden" emission lines present|
|er||"Reversed" center of emission lines weaker than edges|
|eq||Emission lines with P Cygni profile|
|f||N III and He II emission|
|f*||N IV λ4058Å is stronger than the N III λ4634Å, λ4640Å, & λ4642Å lines|
|f+||Si IV λ4089Å & λ4116Å are emission in addition to the N III line|
|(f)||N III emission, absence or weak absorption of He II|
|((f))||Displays strong He II absorption accompanied by weak N III emissions|
|h||WR stars with emission lines due to hydrogen.|
|ha||WR stars with hydrogen emissions seen on both absorption and emission.|
|He wk||Weak He lines|
|k||Spectra with interstellar absorption features|
|m||Enhanced metal features|
|n||Broad ("nebulous") absorption due to spinning|
|nn||Very broad absorption features|
|neb||A nebula's spectrum mixed in|
|p||Unspecified peculiarity, peculiar star.[nb 4]|
|pq||Peculiar spectrum, similar to the spectra of novae|
|q||Red & blue shifts line present|
|s||Narrowly "sharp" absorption lines|
|ss||Very narrow lines|
|sh||Shell star features|
|var||Variable spectral feature (sometimes abbreviated to "v")|
|wl||Weak lines (also "w" & "wk")|
|Abnormally strong spectral lines of the specified element(s)|
The reason for the odd arrangement of letters in the Harvard classification is historical, having evolved from the earlier Secchi classes and been progressively modified as understanding improved.
During the 1860s and 1870s, pioneering stellar spectroscopist Angelo Secchi created the Secchi classes in order to classify observed spectra. By 1866, he had developed three classes of stellar spectra:
- Class I: white and blue stars with broad heavy hydrogen lines, such as Vega and Altair. This includes the modern class A and early class F.
- Class II: yellow stars—hydrogen less strong, but evident metallic lines, such as the Sun, Arcturus, and Capella. This includes the modern classes G and K as well as late class F.
- Class III: orange to red stars with complex band spectra, such as Betelgeuse and Antares. This corresponds to the modern class M.
- Class IV: red stars with significant carbon bands and lines (carbon stars.)
In 1877, he added a fifth class:
In the late 1890s, this classification began to be superseded by the Harvard classification, which is discussed in the remainder of this article. The roman numerals used for Secchi classes should not be confused with the completely unrelated roman numerals used for Yerkes luminosity classes.
|I||A, B, C, D||Hydrogen lines dominant.|
|II||E, F, G, H, I, K, L|
|IV||N||Did not appear in the catalogue.|
|O||Wolf–Rayet spectra with bright lines.|
In the 1880s, the astronomer Edward C. Pickering began to make a survey of stellar spectra at the Harvard College Observatory, using the objective-prism method. A first result of this work was the Draper Catalogue of Stellar Spectra, published in 1890. Williamina Fleming classified most of the spectra in this catalogue. It used a scheme in which the previously used Secchi classes (I to IV) were divided into more specific classes, given letters from A to N. Also, the letters O, P and Q were used, O for stars whose spectra consisted mainly of bright lines, P for planetary nebulae, and Q for stars not fitting into any other class.
In 1897, another worker at Harvard, Antonia Maury, placed the Orion subtype of Secchi class I ahead of the remainder of Secchi class I, thus placing the modern type B ahead of the modern type A. She was the first to do so, although she did not use lettered spectral types, but rather a series of twenty-two types numbered from I to XXII.
In 1901, Annie Jump Cannon returned to the lettered types, but dropped all letters except O, B, A, F, G, K, and M, used in that order, as well as P for planetary nebulae and Q for some peculiar spectra. She also used types such as B5A for stars halfway between types B and A, F2G for stars one-fifth of the way from F to G, and so forth. Finally, by 1912, Cannon had changed the types B, A, B5A, F2G, etc. to B0, A0, B5, F2, etc. This is essentially the modern form of the Harvard classification system. A common mnemonic for remembering the spectral type letters is "Oh, Be A Fine Guy/Girl, Kiss Me".
Early and late
|Look up late-type star or early-type star in Wiktionary, the free dictionary.|
Stars are often referred to as early or late types. Early indicates hotter while late indicates cooler. This stems from an early 20th-century model of stellar evolution in which stars were powered by gravitational contraction via the Kelvin–Helmholtz mechanism whereby stars start their lives as very hot "early-type" stars, and then gradually cool down, evolving into "late-type″ stars. This mechanism provided ages of the Sun that were much smaller than what is observed, and was rendered obsolete by the discovery that stars are powered by nuclear fusion.
Depending on the context, early and late may be absolute or relative terms. Early may therefore refer to O or B, possibly A, stars, or it may simply refer to stars hotter than others such as "early K" being perhaps K0, K1, and K3. Late is used in the same way, with an unqualified use of the term indicating stars with spectral types such as K and M, but it can also be used for relatively cool stars, as in "late A".
O-type stars are very hot and extremely luminous, with most of their radiated output in the ultraviolet range. These are the rarest of all main-sequence stars. About 1 in 3,000,000 (0.00003%) of the main-sequence stars in the solar neighborhood are O-type stars.[nb 5] Some of the most massive stars lie within this spectral class. O-type stars frequently have complicated surroundings that make measurement of their spectra difficult.
O-type spectra used to be defined by the ratio of the strength of the He II λ4541 relative to that of He I λ4471, where λ is the wavelength, measured in ångströms. Spectral type O7 was defined to be the point at which the two intensities are equal, with the He I line weakening towards earlier types. Type O3 was, by definition, the point at which said line disappears altogether, although it can be seen very faintly with modern technology. Due to this, the modern definition uses the ratio of the nitrogen line N IV λ4058 to N III λλ4634-40-42.
O-type stars have dominant lines of absorption and sometimes emission for He II lines, prominent ionized (Si IV, O III, N III, and C III) and neutral helium lines, strengthening from O5 to O9, and prominent hydrogen Balmer lines, although not as strong as in later types. Because they are so massive, O-type stars have very hot cores and burn through their hydrogen fuel very quickly, so they are the first stars to leave the main sequence.
When the MKK classification scheme was first described in 1943, the only subtypes of class O used were O5 to O9.5. The MKK scheme was extended to O9.7 in 1971 and O4 in 1978, and new classification schemes that add types O2, O3 and O3.5 have subsequently been introduced.
- Spectral standards:
B-type stars are very luminous and blue. Their spectra have neutral helium, which are most prominent at the B2 subclass, and moderate hydrogen lines. As O- and B-type stars are so energetic, they only live for a relatively short time. Thus, due to the low probability of kinematic interaction during their lifetime, they are unable to stray far from the area in which they formed, apart from runaway stars.
The transition from class O to class B was originally defined to be the point at which the He II λ4541 disappears. However, with today's better equipment, the line is still apparent in the early B-type stars. Today for main-sequence stars, the B-class is instead defined by the intensity of the He I violet spectrum, with the maximum intensity corresponding to class B2. For supergiants, lines of silicon are used instead; the Si IV λ4089 and Si III λ4552 lines are indicative of early B. At mid B, the intensity of the latter relative to that of Si II λλ4128-30 is the defining characteristic, while for late B, it is the intensity of Mg II λ4481 relative to that of He I λ4471.
These stars tend to be found in their originating OB associations, which are associated with giant molecular clouds. The Orion OB1 association occupies a large portion of a spiral arm of the Milky Way and contains many of the brighter stars of the constellation Orion. About 1 in 800 (0.125%) of the main-sequence stars in the solar neighborhood are B-type main-sequence objects.[nb 5]
Massive yet non-supergiant entities known as "Be stars" are main-sequence stars that notably have, or had at some time, one or more Balmer lines in emission, with the hydrogen-related electromagnetic radiation series projected out by the stars being of particular interest. Be stars are generally thought to feature unusually strong stellar winds, high surface temperatures, and significant attrition of stellar mass as the objects rotate at a curiously rapid rate. Objects known as "B(e)" or "B[e]" stars possess distinctive neutral or low ionisation emission lines that are considered to have 'forbidden mechanisms', undergoing processes not normally allowed under current understandings of quantum mechanics.
- Spectral standards:
- B0V: Upsilon Orionis
- B0Ia: Alnilam
- B2Ia: Chi2 Orionis
- B2Ib: 9 Cephei
- B3V: Eta Ursae Majoris
- B3V: Eta Aurigae
- B3Ia: Omicron2 Canis Majoris
- B5Ia: Eta Canis Majoris
- B8Ia: Rigel
A-type stars are among the more common naked eye stars, and are white or bluish-white. They have strong hydrogen lines, at a maximum by A0, and also lines of ionized metals (Fe II, Mg II, Si II) at a maximum at A5. The presence of Ca II lines is notably strengthening by this point. About 1 in 160 (0.625%) of the main-sequence stars in the solar neighborhood are A-type stars.[nb 5]
- Spectral standards:
F-type stars have strengthening H and K lines of Ca II. Neutral metals (Fe I, Cr I) beginning to gain on ionized metal lines by late F. Their spectra are characterized by the weaker hydrogen lines and ionized metals. Their color is white. About 1 in 33 (3.03%) of the main-sequence stars in the solar neighborhood are F-type stars.[nb 5]
- Spectral standards:
G-type stars, including the Sun have prominent H and K lines of Ca II, which are most pronounced at G2. They have even weaker hydrogen lines than F, but along with the ionized metals, they have neutral metals. There is a prominent spike in the G band of CH molecules. Class G main-sequence stars make up about 7.5%, nearly one in thirteen, of the main-sequence stars in the solar neighborhood.[nb 5]
G is host to the "Yellow Evolutionary Void". Supergiant stars often swing between O or B (blue) and K or M (red). While they do this, they do not stay for long in the yellow supergiant G classification as this is an extremely unstable place for a supergiant to be.
- Spectral standards:
- G0V: Beta Canum Venaticorum
- G0IV: Eta Boötis
- G0Ib: Beta Aquarii
- G2V: Sun
- G5V: Kappa Ceti
- G5IV: Mu Herculis
- G5Ib: 9 Pegasi
- G8V: 61 Ursae Majoris
- G8IV: Beta Aquilae
- G8IIIa: Kappa Geminorum
- G8IIIab: Epsilon Virginis
- G8Ib: Epsilon Geminorum
K-type stars are orangish stars that are slightly cooler than the Sun. They make up about 12%, nearly one in eight, of the main-sequence stars in the solar neighborhood.[nb 5] There are also giant K-type stars, which range from hypergiants like RW Cephei, to giants and supergiants, such as Arcturus, whereas orange dwarfs, like Alpha Centauri B, are main-sequence stars.
They have extremely weak hydrogen lines, if they are present at all, and mostly neutral metals (Mn I, Fe I, Si I). By late K, molecular bands of titanium oxide become present. There is a suggestion that K Spectrum stars may potentially increase the chances of life developing on orbiting planets that are within the habitable zone.
- Spectral standards:
- K0V: Sigma Draconis
- K0III: Pollux
- K0III: Epsilon Cygni
- K2V: Epsilon Eridani
- K2III: Kappa Ophiuchi
- K3III: Rho Boötis
- K5V: 61 Cygni A
- K5III: Gamma Draconis
Class M stars are by far the most common. About 76% of the main-sequence stars in the solar neighborhood are class M stars.[nb 5][nb 6] However, class M main-sequence stars (red dwarfs) have such low luminosities that none are bright enough to be seen with the unaided eye, unless under exceptional conditions. The brightest known M-class main-sequence star is M0V Lacaille 8760, with magnitude 6.6 (the limiting magnitude for typical naked-eye visibility under good conditions is typically quoted as 6.5), and it is extremely unlikely that any brighter examples will be found.
Although most class M stars are red dwarfs, most giants and some supergiants such as VY Canis Majoris, Antares and Betelgeuse are also class M. Furthermore, the hotter brown dwarfs are late class M. This is usually in the range of M6.5 to M9.5. The spectrum of a class M star contains lines from oxide molecules, especially TiO, in the visible and all neutral metals, but absorption lines of hydrogen are usually absent. TiO bands can be strong in class M stars, usually dominating their visible spectrum by about M5. Vanadium(II) oxide bands become present by late M.
- Spectral standards:
Extended spectral types
A number of new spectral types have been taken into use from newly discovered types of stars.
Hot blue emission star classes
Spectra of some very hot and bluish stars exhibit marked emission lines from carbon or nitrogen, or sometimes oxygen.
Class W: Wolf–Rayet
Class W or WR represents the Wolf–Rayet stars, notable for spectra lacking hydrogen lines. Instead their spectra are dominated by broad emission lines of highly ionized helium, nitrogen, carbon and sometimes oxygen. They are thought to mostly be dying supergiants with their hydrogen layers blown away by stellar winds, thereby directly exposing their hot helium shells. Class W is further divided into subclasses according to the relative strength of nitrogen and carbon emission lines in their spectra (and outer layers).
- WN, spectrum dominated by NitrogenIII-V and HeliumI-II lines
- WNE (WN2 to WN5 with some WN6), hotter or "early"
- WNL (WN7 to WN9 with some WN6), cooler or "late"
- Extended WN classes WN10 and WN11 sometimes used for the Ofpe/WN9 stars
- h tag used (e.g. WN9h) for WR with hydrogen emission and ha (e.g. WN6ha) for both hydrogen emission and absorption
- WN/C, WN stars plus strong CarbonIV lines, intermediate between WN and WC stars
- WC, spectrum with strong CarbonII-IV lines
- WCE (WC4 to WC6), hotter or "early"
- WCL (WC7 to WC9), cooler or "late"
- WO (WO1 to WO4), strong OxygenVI lines, extremely rare
Although the central stars of most planetary nebulae (CSPNe) show O-type spectra, around 10% are hydrogen-deficient and show WR spectra. These are low-mass stars and to distinguish them from the massive Wolf Rayet stars, their spectra are enclosed in square brackets: e.g. [WC]. Most of these show [WC] spectra, some [WO], and very rarely [WN].
The "Slash" stars
The slash stars are O-type stars with WN-like lines in their spectra. The name "slash" comes from their printed spectral type having a slash in it (e.g. "Of/WNL").
There is a secondary group found with this spectra, a cooler, "intermediate" group designated "Ofpe/WN9". These stars have also been referred to as WN10 or WN11, but that has become less popular with the realisation of the evolutionary difference from other Wolf–Rayet stars. Recent discoveries of even rarer stars have extended the range of slash stars as far as O2-3.5If*/WN5-7, which are even hotter than the original slash stars.
Cool red and brown dwarf classes
Brown dwarfs, whose energy comes from gravitational attraction alone, cool as they age and so progress to later spectral types. Brown dwarfs start their lives with M-type spectra and will cool through the L, T, and Y spectral classes; faster the less massive they are—the highest-mass brown dwarfs cannot have cooled to Y or even T dwarfs within the age of the universe. Because this leads to a degeneracy between mass and age for a given effective temperature and luminosity, no unique values can be assigned to a given spectral type.
Class L dwarfs get their designation because they are cooler than M stars and L is the remaining letter alphabetically closest to M. Some of these objects have masses large enough to support hydrogen fusion and are therefore stars, but most are of substellar mass and are therefore brown dwarfs. They are a very dark red in color and brightest in infrared. Their atmosphere is cool enough to allow metal hydrides and alkali metals to be prominent in their spectra.
Due to low surface gravity in giant stars, TiO- and VO-bearing condensates never form. Thus, L-type stars larger than dwarfs can never form in an isolated environment. It may be possible for these L-type supergiants to form through stellar collisions, however. An example of which is V838 Monocerotis while in the height of its luminous red nova eruption.
Class T: methane dwarfs
Class T dwarfs are cool brown dwarfs with surface temperatures between approximately 550 and 1,300 K (277 and 1,027 °C; 530 and 1,880 °F). Their emission peaks in the infrared. Methane is prominent in their spectra.
Classes T and L could be more common than all the other classes combined if recent research is accurate. Study of the number of proplyds (protoplanetary disks, clumps of gas in nebulae from which stars and planetary systems are formed) indicates that the number of stars in the galaxy should be several orders of magnitude higher than what was previously speculated. It is theorized that these proplyds are in a race with each other. The first one to form will become a protostar, which are very violent objects and will disrupt other proplyds in the vicinity, stripping them of their gas. The victim proplyds will then probably go on to become main-sequence stars or brown dwarfs of the L and T classes, which are quite invisible to us. Because brown dwarfs can live so long, these smaller bodies accumulate over time.
Brown dwarfs of spectral class Y are cooler than those of spectral class T and have qualitatively different spectra from them. A total of 17 objects have been placed in class Y as of August 2013. Although such dwarfs have been modelled and detected within forty light years by the Wide-field Infrared Survey Explorer (WISE) there is no well-defined spectral sequence yet with prototypes. Nevertheless, several objects have been assigned spectral classes Y0, Y1, and Y2. The spectra of these objects display absorption around 1.55 micrometers. Delorme et al. has suggested that this feature is due to absorption from ammonia and that this should be taken as indicating the T–Y transition, making these objects of type Y0. In fact, this ammonia-absorption feature is the main criterion that has been adopted to define this class. However, this feature is difficult to distinguish from absorption by water and methane, and other authors have stated that the assignment of class Y0 is premature.
The brown dwarf with the latest assigned spectral type, WISE 1828+2650, is a >Y2 dwarf with an effective temperature originally estimated around 300 K, the temperature of the human body. Parallax measurements have, however, since shown that its luminosity is inconsistent with it being colder than ~400 K. The coolest Y dwarf currently known is WISE 0855-0714 with an approximate temperature of 250 K.
The mass range for Y dwarfs is 9–25 Jupiter masses, but for young objects might reach below one Jupiter mass, which means that Y class objects straddle the 13 Jupiter mass deuterium-fusion limit that marks the division between brown dwarfs and planets.
Carbon-related stars are stars whose spectra indicate production of carbon by helium triple-alpha fusion. With increased carbon abundance, and some parallel s-process heavy element production, the spectra of these stars become increasingly deviant from the usual late spectral classes G, K and M. The giants among those stars are presumed to produce this carbon themselves, but not too few of this class of stars are believed to be double stars whose odd atmosphere once was transferred from a former carbon star companion that is now a white dwarf.
Class C: carbon stars
Originally classified as R and N stars, these are also known as 'carbon stars'. These are red giants, near the end of their lives, in which there is an excess of carbon in the atmosphere. The old R and N classes ran parallel to the normal classification system from roughly mid G to late M. These have more recently been remapped into a unified carbon classifier C with N0 starting at roughly C6. Another subset of cool carbon stars are the J-type stars, which are characterized by the strong presence of molecules of 13CN in addition to those of 12CN. A few main-sequence carbon stars are known, but the overwhelming majority of known carbon stars are giants or supergiants. There are several subclasses:
- C-R: Formerly a class on its own representing the carbon star equivalent of late G to early K-type stars.
- C-N: Formerly a class on its own representing the carbon star equivalent of late K to M stars.
- C-J: A subtype of cool C stars with a high content of 13C.
- C-H: Population II analogues of the C-R stars.
- C-Hd: Hydrogen-deficient carbon stars, similar to late G supergiants with CH and C2 bands added.
Class-S stars form a continuum between class-M stars and carbon stars. Those most similar to class-M stars have strong ZrO absorption bands analogous to the TiO bands of class-M stars, whereas those most similar to carbon stars have strong sodium D lines and weak C2 bands. Class-S stars have excess amounts of zirconium and other elements produced by the s-process, and have more similar carbon and oxygen abundances than class-M or carbon stars. Like carbon stars, nearly all known class-S stars are asymptotic-giant-branch stars.
The spectral type is formed by the letter S and a number between zero and ten. This number corresponds to the temperature of the star and approximately follows the temperature scale used for class-M giants. The most common types are S3 to S5, and S10 has only been used for the star χ Cygni when at an extreme minimum.
The basic classification is usually followed by an abundance indication, following one of several schemes: S2,5; S2/5; S2 Zr4 Ti2; or S2*5. A number following a comma is a scale between 1 and 9 based on the ratio of ZrO and TiO. A number following a slash is a more recent but less common scheme designed to represent the ratio of carbon to oxygen on a scale of 1 to 10, where a 0 would be an MS star. Intensities of zirconium and titanium may be indicated explicitly. Also occasionally seen is a number following an asterisk, which represents the strength of the ZrO bands on a scale from 1 to 5.
In between the M and S classes, border cases are named MS stars. In a similar way, border cases between the S and C-N classes are named SC or CS. The sequence M → MS → S → SC → C-N is believed to be a sequence of increased carbon abundance with age for carbon stars in the asymptotic giant branch.
White dwarf classifications
The class D (for Degenerate) is the modern classification used for white dwarfs – low-mass stars that are no longer undergoing nuclear fusion and have shrunk to planetary size, slowly cooling down. Class D is further divided into spectral types DA, DB, DC, DO, DQ, DX, and DZ. The letters are not related to the letters used in the classification of other stars, but instead indicate the composition of the white dwarf's visible outer layer or atmosphere.
- DA: a hydrogen-rich atmosphere or outer layer, indicated by strong Balmer hydrogen spectral lines.
- DB: a helium-rich atmosphere, indicated by neutral helium, He I, spectral lines.
- DO: a helium-rich atmosphere, indicated by ionized helium, He II, spectral lines.
- DQ: a carbon-rich atmosphere, indicated by atomic or molecular carbon lines.
- DZ: a metal-rich atmosphere, indicated by metal spectral lines (a merger of the obsolete white dwarf spectral types, DG, DK and DM).
- DC: no strong spectral lines indicating one of the above categories.
- DX: spectral lines are insufficiently clear to classify into one of the above categories.
The type is followed by a number giving the white dwarf's surface temperature. This number is a rounded form of 50400/Teff, where Teff is the effective surface temperature, measured in kelvins. Originally, this number was rounded to one of the digits 1 through 9, but more recently fractional values have started to be used, as well as values below 1 and above 9.
Two or more of the type letters may be used to indicate a white dwarf that displays more than one of the spectral features above.
Extended white dwarf spectral types:
- DAB: a hydrogen- and helium-rich white dwarf displaying neutral helium lines.
- DAO: a hydrogen- and helium-rich white dwarf displaying ionized helium lines.
- DAZ: a hydrogen-rich metallic white dwarf.
- DBZ: a helium-rich metallic white dwarf.
A different set of spectral peculiarity symbols are used for white dwarfs than for other types of stars:
|Code||Spectral peculiarities for stars|
|P||Magnetic white dwarf with detectable polarization|
|E||Emission lines present|
|H||Magnetic white dwarf without detectable polarization|
|PEC||Spectral peculiarities exist|
Stellar remnants are objects associated with the death of stars. Because the Hertzsprung-Russell diagram is observational in nature, these remnants cannot easily be plotted on the diagram, or cannot be placed at all. Neutron stars are relatively small and cold, and would fall far on the left side of the diagram. Planetary nebulae are dynamic and tend to quickly fade in brightness as the progenitor star transitions to the white dwarf branch. If shown, a planetary nebula would be plotted to the left of the diagram's upper left quadrant. A black hole emits no visible light of its own, and therefore would not appear on the diagram.
- Guest star
- Spectral signature
- Stellar evolution
- Star count, survey of stars
- UBV photometric system
- This is the relative color of the star if Vega, generally considered a bluish star, is used as a standard for "white".
- Chromaticity can vary significantly within a class; for example, the Sun (a G2 star) is white, while a G9 star is yellow.
- Use a different set of spectral types from element-burning stars
- When used with A-type stars, this instead refers to abnormally strong metallic spectral lines
- These proportions are fractions of stars brighter than absolute magnitude 16; lowering this limit will render earlier types even rarer, whereas generally adding only to the M class.
- This rises to 78.6% if we include all stars. (See the above note.)
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