Carbon star

A carbon star is a late type giant star similar to a red giant (or occasionally to a red dwarf) whose atmosphere contains more carbon than oxygen; the two elements combine in the upper layers of the star, forming carbon monoxide, which consumes all the oxygen in the atmosphere, leaving carbon atoms free to form other carbon compounds, giving the star a "sooty" atmosphere and a strikingly red appearance.

In normal stars (such as the Sun), the atmosphere is richer in oxygen than carbon. Ordinary stars not exhibiting the characteristics of carbon stars, but that are cool enough to form carbon monoxide, are therefore called oxygen stars.

Carbon stars have quite distinctive spectral characteristics, and they were first recognized by their spectra by Angelo Secchi in the 1860s — a pioneering time in astronomical spectroscopy.

Astrophysical mechanisms

Carbon stars are explained by more than one astrophysical mechanism. McClure distinguishes between classical carbon stars, and other non-classical ones that are less massive.

In the classical carbon stars, those belonging to the modern spectral types C-R and C-N, the abundance of carbon is thought to be a product of helium fusion, specifically the triple-alpha process within a star, which giants reach near the end of their lives in the Asymptotic Giant Branch (AGB). These fusion products have been brought to the stellar surface by episodes of convection (the so-called third dredge-up) after the carbon and other products were made. Normally this kind of AGB carbon star fuses hydrogen in a hydrogen burning shell, but in episodes separated by 10⁴–10⁵ years, the star transforms to burning helium in a shell, while the hydrogen fusion temporarily ceases. In this phase, the star's luminosity rises, and material from the interior of the star (notably carbon) moves up. Since the luminosity rises, the star expands so that the helium fusion ceases, and the hydrogen shell burning restarts. During these shell helium flashes, the mass loss from the star is significant, and after many shell helium flashes, an AGB star is transformed into a hot white dwarf and its atmosphere becomes material for a planetary nebula.

The non-classical kinds of carbon stars, belonging to the types C-J and C-H, are believed to be binary stars, where one star is observed to be a giant star (or occasionally a red dwarf) and the other a white dwarf. The star presently observed to be a giant star accreted carbon-rich material when it was still a main sequence star from its companion (that is, the star that is now the white dwarf) when the latter was still a classical carbon star. That phase of stellar evolution is relatively brief, and most such stars ultimately end up as white dwarfs. We are now seeing these systems a comparatively long time after the mass transfer event, so the extra carbon observed in the present red giant was not produced within that star. This scenario is also accepted as the origin of the barium stars, which are also characterized as having strong spectral features of carbon molecules and of barium (an s-process element). Sometimes the stars whose excess carbon came from this mass transfer are called "extrinsic" carbon stars to distinguish them from the "intrinsic" AGB stars which produce the carbon internally. Many of these extrinsic carbon stars are not luminous or cool enough to have made their own carbon, which was a puzzle until their binary nature was discovered.

The enigmatic hydrogen deficient carbon stars (HdC), belonging to the spectral class C-Hd, seems to have some relation to R Coronae Borealis variables (RCB), but aren't variable themselves and lack a certain infrared radiation typical for RCB:s. Only five HdC:s are known, and none is known to be binary, so the relation to the non-classical carbon stars is not known.

Other less convincing theories, such as CNO cycle unbalancing and core helium flash have also been proposed as mechanisms for carbon enrichment in the atmospheres of smaller carbon stars.

Carbon star spectra

By definition carbon stars have dominant spectral Swan bands from the molecule C₂. Many other carbon compounds may be present at high levels, such as CH, CN (cyanogen), C₃, and SiC₂. Carbon is formed in the core and circulated into its upper layers, dramatically changing the layers' composition. Other elements formed through helium fusion and the s-process are also "dredged up" in this way, including lithium and barium.

When astronomers developed the spectral classification of the carbon stars, they got into considerable hardships when trying to correlate the spectra to the stars' effective temperatures. The trouble was with all the atmospheric carbon hiding the absorption lines normally used as temperature indicators for the stars.

Secchi

Carbon stars were discovered already in the 1860s when spectral classification pioneer Pater Angelo Secchi erected the Secchi class IV for the carbon stars, which in the late 1890s were reclassified as N class stars.

Harvard

Using this new Harvard classification, the N class was later enhanced by an R class for less deeply red stars sharing the characteristic carbon bands of the spectrum. Later correlation of this R to N scheme with conventional spectra, showed that the R-N sequence approximately run in parallel with c:a G7 to M10 with regards to star temperature.

MK-type	R0	R3	R5	R8	Na	Nb
giant equiv.	G7-G8	K1-K2	~K2-K3	K5-M0	~M2-M3	M3-M4
Teff	4300	3900	~3700	3450	---	---

Morgan-Keenan C system

The later N classes correspond less well to the counterparting M types, because the Harvard classification was only partially based on temperature, but also carbon abundance; so it soon became clear that this kind of carbon star classification was incomplete. Instead a new dual number star class C was erected so to deal with temperature and carbon abundance. Such a spectrum measured for Y Canum Venaticorum, was determined to be C5₄, where 5 refers to temperature dependent features, and 4 to the strength of the C₂ Swan bands in the spectrum. (C5₄ is very often alternatively written C5,4). This Morgan-Keenan C system classification replaced the older R-N classifications from 1960-1993.

MK-type	C0	C1	C2	C3	C4	C5	C6	C7
giant equiv.	G4-G6	G7-G8	G9-K0	K1-K2	K3-K4	K5-M0	M1-M2	M3-M4
Teff	4500	4300	4100	3900	3650	3450	---	---

The Revised Morgan-Keenan system

The two-dimensional Morgan-Keenan C classification failed to fulfill the creators' expectations:

1. it failed to correlate to temperature measurements based on infrared,
2. originally being two-dimensional it was soon enhanced by suffixes, CH, CN, j, and other features making it impractical for en-masse analyses of foreign galaxies' carbon star populations,
3. and it gradually occurred that the old R and N stars actually were two distinct types of carbon stars, having real astrophysical significance.

A new revised Morgan-Keenan classification was published in 1993 by Philip Keenan, defining the classes: C-N, C-R, and C-H. Later the classes C-J and C-Hd were added. This constitutes the established classification system used today :

class	spectrum	population	MV	theory	temperature range (K)	example(s)	# known
classical carbon stars
C-R:	the old Harvard class R reborn: are still visible at the blue end of the spectrum, strong isotopic bands, no enhanced Ba line	medium disc pop I	0	red giants?	5100-2800	S Cam	~25
C-N:	the old Harvard class N reborn: heavy diffuse blue absorption, sometimes invisible in blue, s-process elements enhanced over solar abundance, weak isotopic bands	thin disc pop I	-2.2	AGB	3100-2600	R Lep	~90
non-classical carbon stars
C-J:	very strong isotopic bands of C2 and CN	unknown	unknown	unknown	3900-2800	Y CVn	~20
C-H:	very strong CH absorption	halo pop II	-1.8	bright giants, mass transfer (all C-H:s are binary )	5000-4100	V Ari, TT CVn	~20
C-Hd:	hydrogen lines and CH bands weak or absent	thin disc pop I	-3.5	unknown	?	HD 137613	~7

Other qualities

Most classical carbon stars are variable stars of the long period variable types.

Observing carbon stars

Due to the insensitivity of night vision to red and a slow adaption of the red sensitive eye rods to the light of the stars, amateur astronomers making magnitude estimates of red variable stars, especially carbon stars, have to know how to deal with the Purkinje effect in order to not understate the luminosity of the observed star.

Interstellar carbon sowers

Owing to its low surface gravity, as much as half (or more) of the total mass of a carbon star may be lost by way of powerful stellar winds. The star's remnants, carbon-rich "dust" similar to graphite, therefore become part of the interstellar dust. This dust is believed to be a significant factor in providing the raw materials for the creation of subsequent generations of stars and their planetary systems. The material surrounding a carbon star may blanket it to the extent that the dust absorbs all visible light.

See also

• Barium stars
• S-type stars
• Marc Aaronson: an American astronomer and noted researcher of carbon stars

Specimens:

• R Leporis, Hind's Crimson Star: an example of a carbon star
• IRC +10216, CW Leonis: the most studied carbon star, and also the brightest star in the sky at N-band
• La Superba, Y Canum Venaticorum: one of the brighter carbon stars

External links

• McClure's paper on the carbon and related stars
• List of 110 carbon stars. Includes HD number; secondary identification for most; position in right ascension and declination ; magnitude; spectrum; magnitude range (for variable stars); period (of variability cycle).