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An O-type main-sequence star (O V) is a main-sequence (core hydrogen-burning) star of spectral type O and luminosity class V. These stars have between 15 and 90 times the mass of the Sun and surface temperatures between 30,000 and 50,000 K. They are between 40,000 and 1,000,000 times as luminous as the Sun.

Spectral standard stars

Properties of typical O-type main-sequence stars[1][2]

Spectral type	Mass (M☉)	Radius (R☉)	Luminosity (L☉)	Effective temperature (K)	Color index (B − V)
O3V	120.00	15.00	1,400,000	44,900	−0.330
O4V	85.31	13.43	1,073,019	42,900	−0.326
O5V	60.00	12.00	790,000	41,400	−0.323
O6V	43.71	10.71	540,422	39,500	−0.321
O7V	30.85	9.52	317,322	37,100	−0.318
O8V	23.00	8.50	170,000	35,100	−0.315
O9V	19.63	7.51	92,762	33,300	−0.312

The "anchor" standards which define the MK classification grid for O-type main-sequence stars, i.e. those standards which have not changed since the early 20th century, are S Monocerotis (O7 V) and 10 Lacertae (O9 V).[3]

The Morgan–Keenan–Kellerman (MKK) "Yerkes" atlas from 1943 listed O-type standards between O5 and O9, but only split luminosity classes for the O9s.[4] The two MKK O9 V standards were Iota Orionis and 10 Lacertae. The revised Yerkes standards ("MK") presented listed in Johnson & Morgan (1953)[5] presented no changes to the O5 to O8 types, and listed 5 O9 V standards (HD 46202, HD 52266, HD 57682, 14 Cephei, 10 Lacertae) and 3 O9.5 V standards (HD 34078, Sigma Orionis, Zeta Ophiuchi). An important review on spectral classification by Morgan & Keenan (1973)[6] listed "revised MK" standards for O4 to O7, but again no splitting of standards by luminosity classes. This review also listed main-sequence "dagger standards" of O9 V for 10 Lacertae and O9.5 V for Sigma Orionis.

O-type luminosity classes for subtypes earlier than O5 were not defined with standard stars until the 1970s. The spectral atlas of Morgan, Abt, & Tapscott (1978)[7] defined listed several O-type main-sequence (luminosity class "V") standards: HD 46223 (O4 V), HD 46150 (O5 V), HD 199579 (O6 V), S Monocerotis (O7 V), HD 46149 (O8 V), and HD 46202 (O9 V). Walborn & Fitzpartrick (1990)[8] provided the first digital atlas of spectra for OB-type stars, and included a main-sequence standard for O3 V (HDE 303308). Spectral class O2 was defined in Walborn et al. (2002), with the star BI 253 acting as the O2 V primary standard (actually type "O2 V((f*))"). They also redefined HDE 303308 as an O4 V standard, and listed new O3 V standards (HD 64568 and LH 10-3058).[9]

Properties

These are rare objects; it is estimated that there are no more than 20,000 class O stars in the entire Milky Way,[10] around one in 10,000,000 of all stars. Class O main sequence stars are between 15 and 90 M_☉ and have surface temperatures between 30,000 and 50,000 K. Their bolometric luminosities are between 30,000 and 1,000,000 L_☉. Their radii are more modest at around 10 R_☉. Surface gravities are around 10,000 times that of the Earth, relatively low for a main sequence star. Visual absolute magnitudes range from about −4, 3,400 times brighter than the sun, to about −5.8, 18,000 times brighter than the sun.[11][12]

Class O stars are very young, no more than a few million years old, and in our galaxy they all have high metallicities, around twice that of the sun.[11] O-type main sequence stars in the Large Magellanic Cloud, with lower metallicity, have noticeably higher temperatures, with the most obvious cause being lower mass loss rates.[13] The most luminous class O stars have mass loss rates of more than a millionth M_☉ each year, although the least luminous lose far less. Their stellar winds have a terminal velocity around 2,000 km/s.[14]

Prominent O-class main sequence stars

• θ Muscae is a naked-eye Wolf-Rayet star, but the majority of the visible light is produced by an O-class main sequence companion and an OB supergiant.
• 9 Sagittarii is a spectroscopic binary containing O3.5 and O5–5.5 main sequence stars, making for the brightest star visible within the Lagoon Nebula.
• μ Columbae is a naked-eye O9.5 main sequence star.
• θ¹ Orionis C is the brightest star in the Trapezium cluster in the Orion nebula, an O6 main sequence star with a fainter spectroscopic companion.
• ζ Ophiuchi is an O9.5 main sequence star, the brightest in the sky at 3rd magnitude.

See also

• Star count, survey of stars
• Wolf-Rayet stars

References

На других языках

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[de] Hauptreihenstern der Spektralklasse O

Hauptreihensterne der Spektralklasse O (oder auch O-Sterne der Leuchtkraftklasse V) sind die größten, heißesten und auch massereichsten (15 bis 90-fache Sonnenmasse) Sterne der Hauptreihe und befinden sich links oben im Hertzsprung-Russell-Diagramm. Die meisten massereichen Sterne gehören in ihrer Anfangsphase dieser Sternklasse an.

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- [en] O-type main-sequence star

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[ru] Звёзды главной последовательности спектрального класса O

Звезды главной последовательности спектрального класса O (O V) — карликовые звезды главной последовательности, использующие водород в качестве «топлива», спектрального класса O и класса светимости V. Эти звезды имеют массу в 15-90 раз больше массы Солнца и температуры поверхности от 30 000 К до 50 000 К. Звезды O-класса чрезвычайно яркие: от 40 000 до 1 000 000 раз больше светимостей Солнца и голубые по цвету. Поскольку звезды главной последовательности называются карликовыми звёздами, то этот класс звёзд можно также назвать голубыми карликами (не путать с называемым так же голубым карликом — гипотетическим классом звёзд массой от 0,5 солнечной и ниже).

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