O-type star

Short description: Stellar classification

Relative size of O-type stars with other main-sequence stars

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.

Stars of this type are very rare, but because they are very bright, they can be seen at great distances; out of the 90 brightest stars as seen from Earth, 4 are type O.[lower-alpha 1] Due to their high mass, O-type stars end their lives rather quickly in violent supernova explosions, resulting in black holes or neutron stars. Most of these stars are young massive main sequence, giant, or supergiant stars, but also some central stars of planetary nebulae, old low-mass stars near the end of their lives, which typially have O-like spectra.

O-type stars are typically found in regions of active star formation, such as the spiral arms of a spiral galaxy or a pair of galaxies undergoing collision and merger (such as the Antennae Galaxies). These stars illuminate any surrounding material and are largely responsible for the distinct bluish-white and pink coloration of a galaxy's arms. Furthermore, O-type stars often occur in multiple star systems, where their evolution is more difficult to predict due to mass transfer and the possibility of component stars exploding as supernovae at different times.

## Contents

* 1 Classification
* 2 Characteristics
* 2.1 Structure
* 2.2 Evolution
* 3 Examples
* 4 Location
* 4.1 Spiral arms
* 4.2 O/OB associations
* 4.3 Molecular clouds
* 5 Footnotes
* 6 References

## Classification

O-type stars are classified by the relative strength of certain spectral lines.[1] The key lines are the prominent He+ lines at 454.1 nm and 420.0 nm, which vary from very weak at O9.5 to very strong in O2–O7, and the He0 lines at 447.1 nm and 402.6 nm, which vary from absent in O2/3 to prominent in O9.5. The O7 class is defined where the 454.1 nanometer He+ and 447.1 nanometer He0 lines have equal strength. The very hottest O-type stars have such weak neutral He lines that they must be separated on the relative strength of the N2+ and N3+ lines.[2]

The luminosity classes of O-type stars are assigned on the relative strengths of the He+ emission lines and certain ionised nitrogen and silicon lines. These are indicated by the "f" suffix on the spectral type, with "f" alone indicating N2+ and He+ emission, "(f)" meaning the He emission is weak or absent, "((f))" meaning the N emission is weak or absent, "f*" indicates the addition of very strong N3+ emission, and "f+" the presence of Si3+ emission. Luminosity class V, main-sequence stars, generally have weak or missing emission lines, with giants and supergiants showing increasing emission line strength. At O2–O4, the distinction between main sequence and supergiant stars is narrow, and may not even represent true luminosity or evolutionary differences. At intermediate O5–O8 classes, the distinction between "O((f))" main sequence, "O(f)" giants, and "Of" supergiants is well-defined and represents a definite increase in luminosity. The increasing strength of Si3+ emission is also an indicator of increasing luminosity and this is the primary means of assigning luminosity classes to the late O type stars.[3]

Star types O3 to O8 are classified as luminosity class sub-type "Vz" if they have a particularly strong 468.6 nm ionised helium line. The line's presence is thought to indicate extreme youth; the "z" stands for zero-age.[4]

To help with the classification of O-type stars, standard examples are listed for most of the defined types. The following table gives one of the standard stars for each spectral type. In some cases, a standard star has not been defined. For spectral types O2 to O5.5, supergiants are not split into Ia / Iab / Ib sub-types: Subgiant spectral types are not defined for types O2, O2.5, or O3. Bright giant luminosity classes are not defined for stars hotter than O6.[5]

Class O spectral standard stars[5] | Vz | V | IV | III | II | I | Ib | Iab | Ia

|
|
|
|
|
|
|
|
|

O2 |  | BI 253[2] |  | HD 269810[2] |  | HD 93129 Aa / Ab |  |  |
O3 | HD 64568 | TBD |  | TBD |  | Cyg OB2-7 |  |  |
O3.5 | HD 93128 | HD 93129 B[2] |  | Pismis 24-17 |  | Sher 18 |  |  |
O4 | HD 96715 | HD 46223 | HD 93250 | ST 2-22[2] |  | HD 15570 |  |  |
O4.5 | TBD | HD 15629 | HD 193682 | TBD |  | Cyg OB2-9 |  |  |
O5 | HD 46150 | HDE 319699 | HD 168112 | HD 93843 |  | CPD -47 2963 AB |  |  |
O5.5 | TBD | HD 93204 | TBD | TBD |  | Cyg OB2-11 |  |  |
O6 | HD 42088 | ALS 4880 | HD 101190 Aa / Ab | HDE 338931 | HDE 229196 |  | TBD | TBD | HD 169582
O6.5 | HD 91572 | HD 12993 | HDE 322417 | HD 152733 Aa / Ab | HD 157857 |  | TBD | TBD | HD 163758
O7 | HD 97966 | HD 93146 | ALS 12320 | Cyg OB2-4 A | HD 94963 |  | HD 69464 | TBD | TBD
O7.5 | HD 152590 | HD 35619 | HD 97319 | HD 163800 | HD 34656 |  | HD 17603 | 9 Sge | TBD
O8 | HDE 305539 | HD 101223 | HD 94024 | λ Ori A | 63 Oph |  | BD-11°4586 | HD 225160 | HD 151804
O8.5 |  | HD 14633 Aa / Ab | HD 46966 Aa / Ab | HD 114737 A / B | HD 75211 |  | HD 125241 | TBD | HDE 303492
O9 |  | 10 Lac | HD 93028 | HD 93249 A | τ CMa Aa / Ab |  | 19 Cep | HD 202124 | α Cam
O9.2 |  | HD 46202 | HD 96622 | HD 16832 | ALS 11761 |  | HD 76968 | HD 218915 | HD 152424
O9.5 |  | AE Aur, μ Col | HD 192001 | HD 96264 | δ Ori Aa / Ab |  | TBD | HD 188209 | TBD
O9.7 |  | υ Ori | HD 207538 | HD 189957 | HD 68450 |  | HD 47432 | μ Nor | GS Mus

## Characteristics

The Trifid Nebula (M20) is sculpted and lit by the luminous O7.5III star visible at its centre in this infrared image.

O-type stars are hot and luminous. They have characteristic surface temperatures ranging from 30,000–52,000 K, emit intense ultraviolet ('actinic') light, and so appear in the visible spectrum as bluish-white. Because of their high temperatures the luminosities of main sequence O-type stars range from 10,000 times the Sun to around 1,000,000 times, giants from 100,000 times the Sun to over 1,000,000, and supergiants from about 200,000 times the Sun to several million times, although their masses are no more than about 200M☉.[6]

Other stars in the same temperature range include rare subdwarf O-type (sdO) stars, the central stars of planetary nebulae (CSPNe), and white dwarfs. The white dwarfs have their own spectral classification scheme, but many CSPNe have O-type spectra. Even these small low-mass subdwarfs and CSPNe have luminosities several hundred to several thousand times that of the Sun. Type sdO stars generally have somewhat higher temperatures than massive O-type stars, up to 100,000 K.[7]

O-type stars represent the highest masses of stars on the main sequence. The coolest of them have initial masses of around 16 times the Sun.[8] It is unclear what the upper limit to the mass of an O-type star would be. At solar metallicity levels, stars should not be able to form with masses above 120–150M☉, but at lower metallicity this limit is much higher. O-type stars form only a tiny fraction of main-sequence stars and the vast majority of these are towards the lower end of the mass range. The most massive and hottest types O3 and O2 are extremely rare, were only defined in 1971[9] and 2002[2] respectively, and only a handful are known in total. Giant and supergiant stars are somewhat less massive than the most massive main sequence O-type stars due to mass loss, but are still among the most massive stars known.

The formation rate of class O stars cannot be observed directly, but initial mass functions (IMF) can be derived that model observations of existing star populations and particularly young star clusters. Depending on the chosen IMF, class O stars form at a rate of one in several hundred main sequence stars.[10] Because the luminosity of these stars increases out of proportion to their masses, they have correspondingly shorter lifespans. The most massive spend less than a million years on the main sequence and explode as supernovae after three or four million years. The least luminous O-type stars can remain on the main sequence for around 10 million years, but cool slowly during that time and become early B-type stars. No massive star remains with spectral class O for more than about 5–6 million years.[6][8] Although sdO and CSPNe stars are low-mass stars billions of years old, the time spent in this phase of their lives is extremely short, of the order of 10,000,000 years.[11] The present day mass function can be directly observed, and in the solar neighbourhood less than one in 2,000,000 stars is class O. Differing estimates find between 0.00003% (0.00002% if white dwarfs are included) and 0.00005% of stars being of class O.[12][13]

It has been estimated that there are around 20,000 massive O-type stars in the Milky Way. The low-mass sdO and CSPNe O-type stars are probably more common, although less luminous and therefore harder to find. Despite their short lifetimes, they are thought to be normal stages in the evolution of common stars only a little more massive than the Sun.

### Structure

CNO cycle that powers massive O-type stars. Structure of low-mass, intermediate-mass, and high-mass stars. "M" indicates units of solar masses.

O-type main-sequence stars are fueled by nuclear fusion, as all main-sequence stars are. However, the high mass of O-type stars results in extremely high core temperatures. At these temperatures, hydrogen fusion with the CNO cycle dominates the production of the star's energy and consumes its nuclear fuel at a much higher rate than low-mass stars which fuse hydrogen predominantly with the proton–proton cycle. The intense amount of energy generated by O-type stars cannot be radiated out of their cores efficiently enough, and consequently their cores have vigourous convective flow. The radiative zones of O-type stars occur between the core and photosphere. This mixing of core material into the upper layers is often enhanced by fast rotation, and has a dramatic effect on the evolution of O-type stars. They start to slowly expand and show giant or supergiant characteristics while still burning hydrogen in their cores, then may remain as blue supergiants for much of the time during helium core burning.[8][lower-alpha 2]

Error creating thumbnail: Unable to save thumbnail to destinationsdO-type star cross-section showing inert core and helium shell burning

Type "sdO" stars and CSPNe-type have a substantially different structure. Although they have a wide range of distinct characteristics, it is not fully understood how they all form and develop; they are thought to have degenerate cores that will eventually be exposed as a white dwarf. Before then, the material outside that core, is mostly helium with a thin layer of hydrogen, which is rapidly being lost due to the strong stellar wind. There may be several different origins for this type of star, but at least some of them have an internal shell-like layer where helium is being fused. That shell-burning enlarges the core and provides the power for these small stars' high luminosities.[14]

### Evolution

Evolutionary tracks on the HR diagram. The 15M☉ and 60M☉ tracks are typical of massive O-type stars.

In the lifecycle of O-type stars, different metallicities and rotation rates introduce considerable variation in their evolution, but the basics remain the same.[8]

O-type stars start to move slowly from the zero-age main sequence almost immediately, gradually becoming cooler and slightly more luminous. Although they may be characterised spectroscopically as giants or supergiants, they continue to burn hydrogen in their cores for several million years and develop in a very different manner from low-mass stars such as the Sun. Most O-type main-sequence stars will evolve more or less horizontally in the HR diagram towards cooler temperatures, from an 'actinic' violet to blue, becoming blue supergiants. Core helium ignition occurs smoothly as the stars expand and cool. There are a number of complex phases depending on the exact mass of the star and other initial conditions, but the lowest mass O-type stars will eventually evolve into red supergiants while still burning helium in their cores. If they do not explode as a supernova first, they will then lose their outer layers and become hotter again, sometimes going through a number of blue loops before finally reaching the Wolf–Rayet stage.

The more-massive stars, initially main-sequence stars hotter than about O9, never become red supergiants because strong convection and high luminosity blow away the outer layers too quickly. 25–60M☉ stars may become yellow hypergiants before either exploding as a supernova or evolving back to hotter temperatures. Above about 60M☉, O-type stars evolve though a short blue hypergiant or luminous blue variable phase directly to Wolf–Rayet stars. The most massive O-type stars develop a WNLh spectral type as they start to convect material from the core towards the surface, and these are the most luminous stars that exist.

Low to intermediate-mass stars age in a very different way, through red giant, horizontal branch, asymptotic giant branch (AGB), and then post-AGB phases. Post-AGB evolution generally involves dramatic mass loss, sometimes leaving a planetary nebula, and leaving an increasingly hot exposed stellar interior. If there is sufficient helium and hydrogen remaining, these small but extremely hot stars have an O-type spectrum. They increase in temperature until shell burning and mass loss ceases, then they cool into white dwarfs.

At certain masses or chemical makeups, or perhaps as a result of binary interactions, some of these lower-mass stars become unusually hot during the horizontal branch or AGB phases. There may be multiple reasons, not fully understood, including stellar mergers or very late thermal pulses re-igniting post-AGB stars. These appear as very hot OB stars, but only moderately luminous and below the main sequence. There are both O (sdO) and B (sdB) hot subdwarfs, although they may develop in entirely different ways. The sdO-type stars have fairly normal O spectra but luminosities only around a thousand times the Sun.

## Examples

O-type stars are rare but luminous, so they are easy to detect and there are a number of naked eye examples.

The central star of NGC 6826 is a low-mass O6 star.

NGC 2392 (O6)
IC 418 (O7fp)
NGC 6826 (O6fp)
Planetary nebulas'
central stars

29 Canis Majoris
Alnitak
Alpha Camelopardalis
Cygnus X-1
Tau Canis Majoris
Zeta Puppis
Supergiants

Giants Alnitak is a triple star system with an O9.7 supergiant and an O9 giant as well as a B0 giant. These stars illuminate the nearby Flame Nebula.

Main page: Astronomy:Blue giant
Iota Orionis
LH 54-425
Meissa
Plaskett's star
Xi Persei
Mintaka
HD 164492 A

Subdwarfs

HD 49798 (sdO6p)

Main-sequence The brightest star in the Trapezium cluster is O7V star θ 1 Orionis C. The other three are B0.5 and B1 main-sequence stars.

Main page: Astronomy:O-type main-sequence star
9 Sagittarii
10 Lacertae
AE Aurigae
BI 253
Delta Circini
HD 93205 (V560 Carinae)
Mu Columbae
Sigma Orionis
Theta1 Orionis C
VFTS 102
Zeta Ophiuchi

## Location

The O-type star in Cepheus B, HD 217086, illuminates the molecular cloud with ultraviolet radiation, driving it back while compressing it, triggering the formation of new stars.

### Spiral arms

O-type main-sequence stars tend to appear in the arms of spiral galaxies. This is because, as a spiral arm moves through space, it compresses any molecular clouds in its way. The initial compression of these molecular clouds leads to the formation of stars, some of which are O- and B-type stars. Also, as these stars have shorter lifetimes, they cannot move great distances before their death and so they stay in or relatively near to the spiral arm in which they formed. On the other hand, less massive stars live longer and thus are found throughout the galactic disc, including in between the spiral arms.

### O/OB associations

Stellar associations are groups of stars that are gravitationally unbound from the beginning of their formation. The stars in stellar associations are moving from one another so rapidly that gravitational forces cannot keep them together. In young stellar associations, most of the light comes from O- and B-type stars, so such associations are called OB associations.

### Molecular clouds

The birth of an O-type star in a molecular cloud has a destructive effect on the cloud, but also may trigger the formation of new stars. O-type stars emit copious amounts of ultraviolet radiation, which ionizes the gas in the cloud and pushes it away.[15] O-type stars also have powerful stellar winds, with velocities of thousands of kilometers per second, which can blow a bubble in the molecular cloud around the star.[16] O-type stars explode as supernovae when they die, releasing vast amounts of energy, contributing to the disruption of a molecular cloud.[17] These effects disperse the remaining molecular material in a star-forming region, ultimately stopping the birth of new stars, and possibly leaving behind a young open cluster.

Nevertheless, before the cloud is disrupted, the sweeping up of material by an expanding bubble (called collect and collapse) or the compression of existing cloudlets (called radiation driven implosion) may lead to the birth of new stars. Evidence of triggered star-formation has been observed in a number of star-forming regions, such as Cepheus B and the Elephant's Trunk nebula (where it may account for 14–25% of stars formed).[18] [19]

## Footnotes

1. ↑ The 4 visibly bright O-type stars are Gamma Velorum, Alnitak (Zeta Orionis), Mintaka (Delta Orionis), and Zeta Puppis.
2. ↑ The corona present in other spectral types are also exhibited by O-type main-sequence stars, however the coronae of O-type main-sequence stars extend out much further and generate stellar winds many times stronger. The intense radiation and solar winds from O-type main-sequence stars are strong enough to strip away the atmospheres from planets that form inside the radius of the habitable zone of the star via photoevaporation.[citation needed]

## References

1. ↑ Walborn, N.R.; Fitzpatrick, E.L. (1990). "Contemporary optical spectral classification of the OB stars – A digital atlas". Publications of the Astronomical Society of the Pacific 102: 379. doi:10.1086/132646. Bibcode: 1990PASP..102..379W.
2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Walborn, N.R.; Howarth, I.D.; Lennon, D.J.; Massey, P.; Oey, M.S.; Moffat, A.F.J. et al. (2002). "A new spectral classification system for the earliest O stars: Definition of type O2". The Astronomical Journal 123 (5): 2754. doi:10.1086/339831. Bibcode: 2002AJ....123.2754W. http://discovery.ucl.ac.uk/9632/1/9632.pdf.
3. ↑ Markova, N.; Puls, J.; Scuderi, S.; Simon-Diaz, S.; Herrero, A. (2011). "Spectroscopic and physical parameters of Galactic O-type stars. I. Effects of rotation and spectral resolving power in the spectral classification of dwarfs and giants". Astronomy & Astrophysics 530: A11. doi:10.1051/0004-6361/201015956. Bibcode: 2011A&A...530A..11M.
4. ↑ Arias, Julia I.; Walborn, Nolan R.; Simón Díaz, Sergio; Barbá, Rodolfo H.; Maíz Apellániz, Jesús; Sabín-Sanjulián, Carolina et al. (2016). "Spectral classification and properties of the OVz stars in the Galactic O Star Spectroscopic Survey (GOSSS)". The Astronomical Journal 152 (2): 31. doi:10.3847/0004-6256/152/2/31. Bibcode: 2016AJ....152...31A.
5. ↑ 5.0 5.1 Maíz Apellániz, J.; Sota, A.; Arias, J.I.; Barbá, R.H.; Walborn, N.R.; Simón-Díaz, S.; Negueruela, I.; Marco, A. et al. (2016). "The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 additional O-type systems". The Astrophysical Journal Supplement Series 224 (1): 4. doi:10.3847/0067-0049/224/1/4. Bibcode: 2016ApJS..224....4M.III.+142+additional+O-type+systems&rft.jtitle=The+Astrophysical+Journal+Supplement+Series&rft.aulast=Maíz+Apellániz&rft.aufirst=J.&rft.au=Maíz+Apellániz, J.&rft.au=Sota, A.&rft.au=Arias, J.I.&rft.au=Barbá, R.H.&rft.au=Walborn, N.R.&rft.au=Simón-Díaz, S.&rft.au=Negueruela, I.&rft.au=Marco, A.&rft.au=Leã+o, J.R.S.&rft.date=2016&rft.volume=224&rft.issue=1&rft.pages=4&rft_id=info:doi/10.3847/0067-0049/224/1/4&rft_id=info:bibcode/2016ApJS..224....4M&rfr_id=info:sid/en.wikibooks.org:Astronomy:O-type_star">
6. ↑ 6.0 6.1 Weidner, Carsten; Vink, Jorick (2010). "The masses, and the mass discrepancy of O-type stars". Astronomy & Astrophysics 524: A98. doi:10.1051/0004-6361/201014491. Bibcode: 2010A&A...524A..98W.
7. ↑ Aller, A.; Miranda, L.F.; Ulla, A.; Vázquez, R.; Guillén, P.F.; Olguín, L. et al. (2013). "Detection of a multi-shell planetary nebula around the hot subdwarf O-type star 2MASS J19310888+4324577". Astronomy & Astrophysics 552: A25. doi:10.1051/0004-6361/201219560. Bibcode: 2013A&A...552A..25A.
8. ↑ 8.0 8.1 8.2 8.3 Meynet, G.; Maeder, A. (2003). "Stellar evolution with rotation". Astronomy & Astrophysics 404 (3): 975–990. doi:10.1051/0004-6361:20030512. Bibcode: 2003A&A...404..975M.
9. ↑ Walborn, N.R. (1971). "Some extremely early O stars near η Carinae". The Astrophysical Journal 167: L31. doi:10.1086/180754. Bibcode: 1971ApJ...167L..31W.η+Carinae&rft.jtitle=The+Astrophysical+Journal&rft.aulast=Walborn&rft.aufirst=N.R.&rft.au=Walborn, N.R.&rft.date=1971&rft.volume=167&rft.pages=L31&rft_id=info:doi/10.1086/180754&rft_id=info:bibcode/1971ApJ...167L..31W&rfr_id=info:sid/en.wikibooks.org:Astronomy:O-type_star">
10. ↑ Kroupa, Pavel; Weidner, Carsten; Pflamm-Altenburg, Jan; Thies, Ingo; Dabringhausen, Jörg; Marks, Michael; Maschberger, Thomas (2013). "The stellar and sub-stellar initial mass function of simple and composite populations". Planets, Stars, and Stellar Systems. pp. 115–242. doi:10.1007/978-94-007-5612-0_4. ISBN 978-94-007-5611-3.
11. ↑ Yu, S.; Li, L. (2009). "Hot subdwarfs from the stable Roche lobe overflow channel". Astronomy and Astrophysics 503 (1): 151. doi:10.1051/0004-6361/200809454. Bibcode: 2009A&A...503..151Y.
12. ↑ Ledrew, Glenn (February 2001). "The real starry sky". Journal of the Royal Astronomical Society of Canada 95: 32. Bibcode: 2001JRASC..95...32L.
13. ↑ Mamajek, Eric, ed. "Number densities of stars of different types in the solar vicinity". University of Rochester. http://www.pas.rochester.edu/~emamajek/memo_star_dens.html.
14. ↑ Landstreet, John D.; Bagnulo, Stefano; Fossati, Luca; Jordan, Stefan; O'Toole, Simon J. (2012). "The magnetic fields of hot subdwarf stars". Astronomy & Astrophysics 541: A100. doi:10.1051/0004-6361/201219178. Bibcode: 2012A&A...541A.100L.
15. ↑ Dale, J.E. (2013). "Ionizing feedback from massive stars in massive clusters – III. Disruption of partially unbound clouds". Monthly Notices of the Royal Astronomical Society 430 (1): 234–246. doi:10.1093/mnras/sts592. Bibcode: 2013MNRAS.430..234D.
16. ↑ Dale, K.V. (2008). "The effect of stellar winds on the formation of a protocluster". Monthly Notices of the Royal Astronomical Society 391 (2): 2–13. doi:10.1111/j.1365-2966.2008.13802.x. Bibcode: 2008MNRAS.391....2D.
17. ↑ Dekel, A.; Krumholz, M.R. (2013). "Steady outflows in giant clumps of high-z disc galaxies during migration and growth by accretion". Monthly Notices of the Royal Astronomical Society 432 (1): 455–467. doi:10.1093/mnras/stt480. Bibcode: 2013MNRAS.432..455D.
18. ↑ Getman, K.V. (2009). "Protoplanetary disk evolution around the triggered star-forming region Cepheus B". Astrophysical Journal 699 (2): 1454–1472. doi:10.1088/0004-637X/699/2/1454. Bibcode: 2009ApJ...699.1454G.
19. ↑ Getman, K. V. (2012). "The Elephant Trunk Nebula and the Trumpler 37 cluster: Contribution of triggered star formation to the total population of an HII region". Monthly Notices of the Royal Astronomical Society 426 (4): 2917–2943. doi:10.1111/j.1365-2966.2012.21879.x. Bibcode: 2012MNRAS.426.2917G.

* v
* t
* e

Stars

Formation|

* Accretion
* Molecular cloud
* Bok globule
* Young stellar object
* Protostar
* Pre-main-sequence
* Herbig Ae/Be
* T Tauri
* FU Orionis
* Herbig–Haro object
* Hayashi track
* Henyey track

Evolution|

* Main sequence
* Red-giant branch
* Horizontal branch
* Red clump
* Asymptotic giant branch
* Blue loop
* Protoplanetary nebula
* Planetary nebula
* PG1159
* Dredge-up
* Instability strip
* Luminous blue variable
* Blue straggler
* Stellar population
* Supernova
* Superluminous supernova / Hypernova

Spectral
classification|

* Early
* Late
* Main sequence
* O
* B
* A
* F
* G
* K
* M
* Brown dwarf
* WR
* OB
* Subdwarf
* O
* B
* Subgiant
* Giant
* Blue
* Red
* Yellow
* Bright giant
* Supergiant
* Blue
* Red
* Yellow
* Hypergiant
* Yellow
* Carbon
* S
* CN
* CH
* White dwarf
* Chemically peculiar
* Am
* Ap/Bp
* HgMn
* Helium-weak
* Barium
* Extreme helium
* Lambda Boötis
* Lead
* Technetium
* Be
* Shell
* B[e]

Remnants|

* White dwarf
* Helium planet
* Black dwarf
* Neutron
* Radio-quiet
* Pulsar
* Binary
* X-ray
* Magnetar
* Stellar black hole
* X-ray binary
* Burster

Hypothetical|

* Blue dwarf
* Green
* Black dwarf
* Exotic
* Boson
* Electroweak
* Strange
* Preon
* Planck
* Dark
* Dark-energy
* Quark
* Q
* Black
* Gravastar
* Frozen
* Quasi-star
* Thorne–Żytkow object
* Iron
* Blitzar

Stellar
nucleosynthesis|

* Deuterium burning
* Lithium burning
* Proton–proton chain
* CNO cycle
* Helium flash
* Triple-alpha process
* Alpha process
* Carbon burning
* Neon burning
* Oxygen burning
* Silicon burning
* S-process
* R-process
* Fusor
* Nova
* Symbiotic
* Remnant
* Luminous red nova

Structure|

* Core
* Convection zone
* Microturbulence
* Oscillations
* Radiation zone
* Atmosphere
* Photosphere
* Starspot
* Chromosphere
* Corona
* Stellar wind
* Bubble
* Bipolar outflow
* Accretion disk
* Asteroseismology
* Helioseismology
* Eddington luminosity
* Kelvin–Helmholtz mechanism

Properties|

* Designation
* Dynamics
* Effective temperature
* Luminosity
* Kinematics
* Magnetic field
* Absolute magnitude
* Mass
* Metallicity
* Rotation
* Starlight
* Variable
* Photometric system
* Color index
* Hertzsprung–Russell diagram
* Color–color diagram

Star systems|

* Binary
* Contact
* Common envelope
* Eclipsing
* Symbiotic
* Multiple
* Cluster
* Open
* Globular
* Super
* Planetary system

Earth-centric
observations|

* Sun
* Solar System
* Sunlight
* Pole star
* Circumpolar
* Constellation
* Asterism
* Magnitude
* Apparent
* Extinction
* Photographic
* Radial velocity
* Proper motion
* Parallax
* Photometric-standard

Lists|

* Proper names
* Arabic
* Chinese
* Extremes
* Most massive
* Highest temperature
* Largest volume
* Smallest volume
* Brightest
* Historical
* Most luminous
* Nearest
* Nearest bright
* With exoplanets
* Brown dwarfs
* White dwarfs
* Milky Way novae
* Supernovae
* Candidates
* Remnants
* Planetary nebulae
* Timeline of stellar astronomy

Related articles|

* Substellar object
* Brown dwarf
* Sub-brown dwarf
* Planet
* Galactic year
* Galaxy
* Guest
* Gravity
* Intergalactic
* Starfield
* Tidal disruption event

'Category:Stars * '

0.00

(0 votes)

Original source: https://en.wikipedia.org/wiki/O-type star. Read more

|

Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:O-type_star&oldid=376281"
*[v]: View this template
*[t]: Discuss this template
*[e]: Edit this template