Carbon star

Last updated
Y Canum Venaticorum, a carbon star in the Canes Venatici constellation, in optical light Y Canum Venaticorum RGB.jpg
Y Canum Venaticorum, a carbon star in the Canes Venatici constellation, in optical light

A carbon star (C-type star) is typically an asymptotic giant branch star, a luminous red giant, whose atmosphere contains more carbon than oxygen. [1] The two elements combine in the upper layers of the star, forming carbon monoxide, which consumes most of the oxygen in the atmosphere, leaving carbon atoms free to form other carbon compounds, giving the star a "sooty" atmosphere and a strikingly ruby red appearance. There are also some dwarf and supergiant carbon stars, with the more common giant stars sometimes being called classical carbon stars to distinguish them.

Contents

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

Carbon stars have quite distinctive spectral characteristics, [2] and they were first recognized by their spectra by Angelo Secchi in the 1860s, a pioneering time in astronomical spectroscopy.

Spectra

Echelle spectra of the carbon star UU Aurigae Echelle Spectra of the Carbon Star UU Aurigae.jpg
Echelle spectra of the carbon star UU Aurigae

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. In addition to carbon, S-process elements such as barium, technetium, and zirconium are formed in the shell flashes and are "dredged up" to the surface. [3]

When astronomers developed the spectral classification of the carbon stars, they had considerable difficulty 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.

Carbon stars also show a rich spectrum of molecular lines at millimeter wavelengths and submillimeter wavelengths. In the carbon star CW Leonis more than 50 different circumstellar molecules have been detected. This star is often used to search for new circumstellar molecules.

Secchi

Carbon stars were discovered already in the 1860s when spectral classification pioneer Angelo Secchi erected the Secchi class IV for the carbon stars, which in the late 1890s were reclassified as N class stars. [4]

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. [5]

MK-typeR0R3R5R8NaNb
giant equiv.G7–G8K1–K2~K2–K3K5–M0~M2–M3M3–M4
Teff43003900~37003450——

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). [6] This Morgan–Keenan C system classification replaced the older R-N classifications from 1960 to 1993.

MK-typeC0C1C2C3C4C5C6C7
giant equiv.G4–G6G7–G8G9–K0K1–K2K3–K4K5–M0M1–M2M3–M4
Teff450043004100390036503450——

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. [7] This constitutes the established classification system used today. [8]

classspectrum population MV theorytemperature
range (K) [9] 		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 linemedium disc pop I0red giants?5100–2800S 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 bandsthin disc pop I−2.2 AGB 3100–2600 R Lep ~90
non-classical carbon stars
C-J:very strong isotopic bands of C2 and CNunknownunknownunknown3900–2800 Y CVn ~20
C-H:very strong CH absorptionhalo pop II−1.8bright giants, mass transfer (all C-H:s are binary [10] )5000–4100V Ari, TT CVn~20
C-Hd:hydrogen lines and CH bands weak or absentthin disc pop I−3.5unknown?HM Lib~7

Astrophysical mechanisms

Carbon stars can be explained by more than one astrophysical mechanism. Classical carbon stars are distinguished from non-classical ones on the grounds of mass, with classical carbon stars being the more massive. [11]

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. These systems are now being observed 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. [11] 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 are not 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, [12] 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.

Other characteristics

Optical light image of the carbon star VX Andromedae VX Andromedae.jpg
Optical light image of the carbon star VX Andromedae

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, astronomers making magnitude estimates of red variable stars, especially carbon stars, have to know how to deal with the Purkinje effect in order not to underestimate the magnitude of the observed star.

Generation of interstellar dust

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. [13] 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.

Silicon carbide outflow from carbon stars was accreted in the early solar nebula and survived in the matrices of relatively unaltered chondritic meteorites. This allows for direct isotopic analysis of the circumstellar environment of 1-3 M☉ carbon stars. Stellar outflow from carbon stars is the source of the majority of presolar silicon carbide found in meteorites. [14]

Other classifications

Other types of carbon stars include:

Use as standard candles

A histogram showing the relative number of LMC carbon stars with a given near-infrared luminosity. The median value is marked in red. Adapted from Ripoche et al. (2020) LMCCarbonStarPDF.png
A histogram showing the relative number of LMC carbon stars with a given near-infrared luminosity. The median value is marked in red. Adapted from Ripoche et al. (2020)

Classical carbon stars are very luminous, especially in the near-infrared, so they can be detected in nearby galaxies. Because of the strong absorption features in their spectra, carbon stars are redder in the near-infrared than oxygen-rich stars are, and they can be identified by their photometric colors. [16] While individual carbon stars do not all have the same luminosity, a large sample of carbon stars will have a luminosity probability density function (PDF) with nearly the same median value, in similar galaxies. So the median value of that function can be used as a standard candle for the determination of the distance to a galaxy. The shape of the PDF may vary depending upon the average metallicity of the AGB stars within a galaxy, so it is important to calibrate this distance indicator using several nearby galaxies for which the distances are known through other means. [15] [17]

See also

Related Research Articles

<span class="mw-page-title-main">Main sequence</span> Continuous band of stars that appears on plots of stellar color versus brightness

In astronomy, the main sequence is a classification of stars which appear on plots of stellar color versus brightness as a continuous and distinctive band. Stars on this band are known as main-sequence stars or dwarf stars, and positions of stars on and off the band are believed to indicate their physical properties, as well as their progress through several types of star life-cycles. These are the most numerous true stars in the universe and include the Sun. Color-magnitude plots are known as Hertzsprung–Russell diagrams after Ejnar Hertzsprung and Henry Norris Russell.

<span class="mw-page-title-main">Stellar classification</span> Classification of stars based on spectral properties

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 spectral lines. Each line indicates a particular chemical element or molecule, with the line strength indicating the abundance of that element. The strengths of the different spectral lines vary mainly due to the temperature of the photosphere, although in some cases there are true abundance differences. The spectral class of a star is a short code primarily summarizing the ionization state, giving an objective measure of the photosphere's temperature.

<span class="mw-page-title-main">Supergiant</span> Type of star that is massive and luminous

Supergiants are among the most massive and most luminous stars. Supergiant stars occupy the top region of the Hertzsprung–Russell diagram with absolute visual magnitudes between about −3 and −8. The temperature range of supergiant stars spans from about 3,400 K to over 20,000 K.

<span class="mw-page-title-main">Red supergiant</span> Stars with a supergiant luminosity class with a spectral type of K or M

Red supergiants (RSGs) are stars with a supergiant luminosity class and a stellar classification K or M. They are the largest stars in the universe in terms of volume, although they are not the most massive or luminous. Betelgeuse and Antares A are the brightest and best known red supergiants (RSGs), indeed the only first magnitude red supergiant stars.

<span class="mw-page-title-main">Blue giant</span> Hot, giant star of early spectral type

In astronomy, a blue giant is a hot star with a luminosity class of III (giant) or II. In the standard Hertzsprung–Russell diagram, these stars lie above and to the right of the main sequence.

<span class="mw-page-title-main">Giant star</span> Type of star, larger and brighter than the Sun

A giant star has a substantially larger radius and luminosity than a main-sequence star of the same surface temperature. They lie above the main sequence on the Hertzsprung–Russell diagram and correspond to luminosity classes II and III. The terms giant and dwarf were coined for stars of quite different luminosity despite similar temperature or spectral type by Ejnar Hertzsprung in 1905 or 1906.

<span class="mw-page-title-main">Asymptotic giant branch</span> Stars powered by fusion of hydrogen and helium in shell with an inactive core of carbon and oxygen

The asymptotic giant branch (AGB) is a region of the Hertzsprung–Russell diagram populated by evolved cool luminous stars. This is a period of stellar evolution undertaken by all low- to intermediate-mass stars (about 0.5 to 8 solar masses) late in their lives.

<span class="mw-page-title-main">B-type main-sequence star</span> Stellar classification distinguished by bright blue luminosity

A B-type main-sequence star is a main-sequence (hydrogen-burning) star of spectral type B and luminosity class V. These stars have from 2 to 16 times the mass of the Sun and surface temperatures between 10,000 and 30,000 K. B-type stars are extremely luminous and blue. Their spectra have strong neutral helium absorption lines, which are most prominent at the B2 subclass, and moderately strong hydrogen lines. Examples include Regulus, Algol A and Acrux.

<span class="mw-page-title-main">Chi Cygni</span> Star in the constellation Cygnus

Chi Cygni is a Mira variable star in the constellation Cygnus, and also an S-type star. It is around 500 light years away.

Barium stars are spectral class G to K stars whose spectra indicate an overabundance of s-process elements by the presence of singly ionized barium, Ba II, at λ 455.4 nm. Barium stars also show enhanced spectral features of carbon, the bands of the molecules CH, CN and C2. The class was originally recognized and defined by William P. Bidelman and Philip Keenan. Initially, after their discovery, they were thought to be red giants, but the same chemical signature has been observed in main-sequence stars as well.

<span class="mw-page-title-main">R Andromedae</span> Star in the constellation Andromeda

R Andromedae is a Mira-type variable star in the constellation Andromeda. Its spectral class is type S because it shows absorption bands of zirconium monoxide (ZrO) in its spectrum. It was among the stars found by Paul Merrill to show absorption lines of the unstable element technetium, establishing that nucleosynthesis must be occurring in stars. The SH molecule was found for the first time outside earth in the atmosphere of this star. The star is losing mass due to stellar winds at a rate of 1.09×10−6M☉/yr.

A technetium star, or more properly a Tc-rich star, is a star whose stellar spectrum contains absorption lines of the light radioactive metal technetium. The most stable isotope of technetium is 97Tc with a half-life of 4.21 million years, which is too short a time to allow the metal to be material from before the star's formation. Therefore, the detection in 1952 of technetium in stellar spectra provided unambiguous proof of nucleosynthesis in stars, one of the more extreme cases being R Geminorum.

<span class="mw-page-title-main">Yellow supergiant</span> Star that has a supergiant luminosity class, with a spectral type of F or G

A yellow supergiant (YSG) is a star, generally of spectral type F or G, having a supergiant luminosity class. They are stars that have evolved away from the main sequence, expanding and becoming more luminous.

<span class="mw-page-title-main">S-type star</span> Cool giant with approximately equal quantities of carbon and oxygen in its atmosphere

An S-type star is a cool giant with approximately equal quantities of carbon and oxygen in its atmosphere. The class was originally defined in 1922 by Paul Merrill for stars with unusual absorption lines and molecular bands now known to be due to s-process elements. The bands of zirconium monoxide (ZrO) are a defining feature of the S stars.

<span class="mw-page-title-main">TX Piscium</span> Carbon star visible to the naked eye in the constellation Pisces

TX Piscium is a variable red giant star in the constellation Pisces. It is amongst the reddest naked eye stars, with a significant reddish hue when seen in binoculars. It is approximately 800 light years from Earth.

<span class="mw-page-title-main">Red giant</span> Type of large cool star

A red giant is a luminous giant star of low or intermediate mass in a late phase of stellar evolution. The outer atmosphere is inflated and tenuous, making the radius large and the surface temperature around 5,000 K or lower. The appearance of the red giant is from yellow-white to reddish-orange, including the spectral types K and M, sometimes G, but also class S stars and most carbon stars.

<span class="mw-page-title-main">Hertzsprung–Russell diagram</span> Scatter plot of stars showing the relationship of luminosity to stellar classification

The Hertzsprung–Russell diagram is a scatter plot of stars showing the relationship between the stars' absolute magnitudes or luminosities and their stellar classifications or effective temperatures. The diagram was created independently in 1911 by Ejnar Hertzsprung and by Henry Norris Russell in 1913, and represented a major step towards an understanding of stellar evolution.

<span class="mw-page-title-main">U Camelopardalis</span> Star in the constellation Camelopardalis

U Camelopardalis is a semiregular variable star in the constellation Camelopardalis. Based on parallax measurements made by the Hipparcos spacecraft, it is located about 3,000 light-years away from the Earth. Its apparent visual magnitude is about 8, which is dim enough that it cannot be seen with the unaided eye.

<span class="mw-page-title-main">O-type star</span> Stellar classification

An O-type star is a hot, blue-white star of spectral type O in the Yerkes classification system employed by astronomers. They have temperatures in excess of 30,000 kelvins (K). Stars of this type have strong absorption lines of ionised helium, strong lines of other ionised elements, and hydrogen and neutral helium lines weaker than spectral type B.

<span class="mw-page-title-main">X Cancri</span> Variable star in the constellation Cancer

X Cancri is a variable star in the northern constellation of Cancer. It has a red hue and is visible to the naked eye at its brightest. The distance to this object is approximately 1,860 light years based on parallax measurements, but is drifting closer with a radial velocity of −5 km/s. It lies very close to the ecliptic and so is subject to lunar occultations.

References

  1. ↑ "C Stars". lweb.cfa.harvard.edu. Retrieved 2023-07-23.
  2. ↑ Hille, Karl (2018-08-10). "Hubble Views Striking Carbon Star in Colorful Cluster". NASA. Retrieved 2023-07-23.
  3. ↑ Savina, Michael R.; Davis, Andrew M.; Tripa, C. Emil; Pellin, Michael J.; Clayton, Robert N.; Lewis, Roy S.; Amari, Sachiko; Gallino, Roberto; Lugaro, Maria (2003). "Barium isotopes in individual presolar silicon carbide grains from the Murchison meteorite". Geochimica et Cosmochimica Acta. 67 (17): 3201. Bibcode:2003GeCoA..67.3201S. doi:10.1016/S0016-7037(03)00083-8.
  4. ↑ Gottesman, S. (Spring 2009). "Classification of Stellar Spectra: Some History". AST2039 Materials. Retrieved 2012-03-21.
  5. ↑ Clowes, C. (25 October 2003). "Carbon Stars". peripatus.gen.nz. Archived from the original on 2012-02-05. Retrieved 2012-03-21.
  6. ↑ Keenan, P. C.; Morgan, W. W. (1941). "The Classification of the Red Carbon Stars". The Astrophysical Journal . 94: 501. Bibcode:1941ApJ....94..501K. doi:10.1086/144356.
  7. ↑ Keenan, P. C. (1993). "Revised MK Spectral Classification of the Red Carbon Stars". Publications of the Astronomical Society of the Pacific . 105: 905. Bibcode:1993PASP..105..905K. doi: 10.1086/133252 .
  8. ↑ "Spectral Atlas of Carbon Stars" . Retrieved 2012-03-21.
  9. ↑ Tanaka, M.; et al. (2007). "Near-Infrared Spectra of 29 Carbon Stars: Simple Estimates of Effective Temperature". Publications of the Astronomical Society of Japan . 59 (5): 939–953. Bibcode:2007PASJ...59..939T. doi: 10.1093/pasj/59.5.939 .
  10. ↑ McClure, R. D.; Woodsworth, A. W. (1990). "The Binary Nature of the Barium and CH Stars. III – Orbital Parameters". The Astrophysical Journal . 352: 709. Bibcode:1990ApJ...352..709M. doi: 10.1086/168573 .
  11. 1 2 McClure, R. D. (1985). "The Carbon and Related Stars". Journal of the Royal Astronomical Society of Canada . 79: 277. Bibcode:1985JRASC..79..277M.
  12. ↑ Clayton, G. C. (1996). "The R Coronae Borealis Stars". Publications of the Astronomical Society of the Pacific . 108: 225. Bibcode:1996PASP..108..225C. doi: 10.1086/133715 .
  13. ↑ Wallerstein, George; Knapp, Gillian R. (September 1998). "CARBON STARS". Annual Review of Astronomy and Astrophysics. 36 (1): 369–433. Bibcode:1998ARA&A..36..369W. doi:10.1146/annurev.astro.36.1.369.
  14. ↑ Zinner, E. (1 January 2014). "1.4 - Presolar Grains". Treatise on Geochemistry (Second Edition): 181–213. doi:10.1016/B978-0-08-095975-7.00101-7. ISBN   978-0-08-098300-4.
  15. 1 2 Ripoche, Paul; Heyl, Jeremy; Parada, Javiera; Richer, Harvey (January 2020). "Carbon stars as standard candles: I. The luminosity function of carbon stars in the Magellanic Clouds". Monthly Notices of the Royal Astronomical Society. 495 (3): 2858–2866. arXiv: 2005.05539 . Bibcode:2020MNRAS.495.2858R. doi: 10.1093/mnras/staa1346 . Retrieved 14 December 2022.
  16. ↑ Mould, J.; Aaronson, M. (September 1980). "The extended giant branches of intermediate age globular clusters in the Magellanic Clouds". Astrophysical Journal. 240: 464–477. Bibcode:1980ApJ...240..464M. doi:10.1086/158252 . Retrieved 14 December 2022.
  17. ↑ Parada, Javiera; Heyl, Jeremy; Richer, Harvey; Ripoche, Paul; Rousseau-Nepton, Laurie (February 2021). "Carbon stars as standard candles – II. The median J magnitude as a distance indicator". Monthly Notices of the Royal Astronomical Society. 501 (1): 933–947. arXiv: 2011.11681 . Bibcode:2021MNRAS.501..933P. doi: 10.1093/mnras/staa3750 . Retrieved 14 December 2022.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.