HD 93205

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HD 93205
Carina Nebula by ESO.jpg
Cercle rouge 100%25.svg
Location of HD 93205 (circled), southwest of Eta Carinae, the brightest star in the image
Observation data
Epoch J2000       Equinox J2000
Constellation Carina
Right ascension 10h 44m 33.739s [1]
Declination −59° 44′ 15.43″ [1]
Apparent magnitude  (V)7.75 [2]
Characteristics
Spectral type O3.5Vf + O8V [3]
U−B color index −0.91 [2]
B−V color index +0.05 [2]
Variable type Ellipsoidal [4]
Astrometry
Radial velocity (Rv)3.6 km/s
Proper motion (μ)RA: −6.619 [1]   mas/yr
Dec.: 2.947 [1]   mas/yr
Parallax (π)0.4308 ± 0.0248  mas [1]
Distance 7,600 ± 400  ly
(2,300 ± 100  pc)
Absolute magnitude  (MV)−5.87 + −4.32 [5]
Orbit [6]
Period (P)6.0803 days
Eccentricity (e)0.370
Inclination (i)60 [7] °
Semi-amplitude (K1)
(primary)		132.6 km/s
Semi-amplitude (K2)
(secondary)		313.6 km/s
Details
Mass 40 - 60 [6]   M☉
Radius 9.2 [7]   R☉
Luminosity 1,160,000 [5]   L☉
Temperature 51,300 [5]   K
secondary
Mass 17 - 25.3 [6]   M☉
Radius 7.0 [7]   R☉
Luminosity112,000 [5]   L☉
Temperature 38,000 [5]   K
Age < 2 [6]   Myr
Other designations
V560  Car, CD−59°3294, HD  93205, SAO  238418
Database references
SIMBAD data
Light curve for V560 Carinae, plotted from Hipparcos data V560CarLightCurve.png
Light curve for V560 Carinae, plotted from Hipparcos data

HD 93205, or V560 Carinae, is a binary stellar system, in the Carina Nebula (NGC 3372) in the constellation Carina. It consists of two massive O-stars that revolve around each other in 6 days.

The more massive member of the pair is an O3.5 main sequence star. The spectrum shows some ionised nitrogen and helium emission lines, indicating some mixing of fusion products to the surface and a strong stellar wind. The mass calculated from apsidal motion of the orbits is 40 to 60 M☉. This is somewhat lower than expected from evolutionary modelling of a star with its observed parameters. [6]

The less massive member is an O8 main sequence star of approximately 20 M☉. [7] It moves in its orbit at a speed of over 300 km/s and is considered to be a relativistic binary, which causes the apses of the orbit to change in a predictable way. [5]

In 1985, Arnout van Genderen et al. reported that the star appeared to be "variable in brightness". [9] Eleonora A. Antokhina et al. confirmed the star's variability in the year 2000, and presented an extensive analysis of the light curve. [7] The star was given its variable star designation, V560 Carinae, in 2001. [10] The closeness of the two stars causes them to become deformed, and this means that the observed brightness of the system varies slightly every six days during its orbit. The total amplitude of the variation is only 0.02 magnitudes. [4]

It is generally considered as a member of the open cluster Trumpler 16. [11] Among its neighbors are some of the most massive and luminous stars in the galaxy, like Eta Carinae, HD 93250 and the binary WR 25. It lies five arc-minutes from Eta Carinae.

Related Research Articles

<span class="mw-page-title-main">V533 Carinae</span> Star in the constellation Carina

V533 Carinae is a A-type supergiant and a Alpha Cygni variable star with a mean apparent magnitude of +4.59 in the constellation Carina. It is located at a distance of about 13,000 light years. It is visible to the naked eye outside of brightly-lit urban areas.

<span class="mw-page-title-main">HD 93129</span> Triple star system in the constellation Carina

HD 93129 is a triple star system in the Carina Nebula, with all three components being hot O class stars amongst the most luminous stars in the Milky Way. It is the dominant member of the Trumpler 14 star cluster, a young star cluster within the Carina OB1 stellar association that harbors other super-luminous stars, like Eta Carinae and WR 25.

<span class="mw-page-title-main">Y Carinae</span> Star in the constellation Carina

Y Carinae is a Classical Cepheid variable, a type of variable star, in the constellation Carina. Its apparent magnitude varies from 7.53 to 8.48.

<span class="mw-page-title-main">EZ Canis Majoris</span> Binary star system in the constellation Canis Major

EZ Canis Majoris is binary system in the constellation of Canis Major. The primary is a Wolf-Rayet star and it is one of the ten brightest Wolf-Rayet stars, brighter than apparent magnitude 7.

<span class="mw-page-title-main">HD 93250</span> Highly luminous binary star system in the constellation Carina

HD 93250 is a highly luminous hot blue binary star in the Carina Nebula in the constellation Carina.

<span class="mw-page-title-main">4U 1700-37</span>

4U 1700-37 is one of the stronger binary X-ray sources in the sky, and is classified as a high-mass X-ray binary. It was discovered by the Uhuru satellite. The "4U" designation refers to the fourth Uhuru catalog.

<span class="mw-page-title-main">HR Carinae</span> Star in the constellation Carina

HR Carinae is a luminous blue variable star located in the constellation Carina. It is surrounded by a vast nebula of ejected nuclear-processed material because this star has a multiple shell expanding atmosphere. This star is among the most luminous stars in the Milky Way. It has very broad emission wings on the Balmer lines, reminiscent from the broad lines observed in the spectra of O and Wolf–Rayet stars. A distance of 5 kpc and a bolometric magnitude of −9.4 put HR Car among the most luminous stars of the galaxy.

<span class="mw-page-title-main">S Monocerotis</span> Star in the constellation Monoceros

S Monocerotis, also known as 15 Monocerotis, is a massive multiple and variable star system located in the constellation Monoceros. It is the brightest star in the Christmas Tree open cluster in the area catalogued as NGC 2264.

<span class="mw-page-title-main">WR 22</span> Binary star in the constellation Carina

WR 22, also known as V429 Carinae or HR 4188, is an eclipsing binary star system in the constellation Carina. The system contains a Wolf-Rayet (WR) star that is one of the most massive and most luminous stars known, and is also a bright X-ray source due to colliding winds with a less massive O class companion. Its eclipsing nature and apparent magnitude make it very useful for constraining the properties of luminous hydrogen-rich WR stars.

<span class="mw-page-title-main">RT Carinae</span> Star in the constellation Carina

RT Carinae, also known as CD-58 3538, is a red supergiant and a variable star, located 7,000 light years away in the constellation Carina. It is in the Carina Nebula. The average apparent magnitude of +8.55, too faint to be visible to the naked eye.

<span class="mw-page-title-main">WR 25</span> Binary star system in the constellation Carina

WR 25 is a binary star system in the turbulent star-forming region of the Carina Nebula, about 6,800 light-years from Earth. It contains a Wolf-Rayet star and a hot luminous companion and is a member of the Trumpler 16 cluster. The name comes from the Catalogue of Galactic Wolf–Rayet Stars.

<span class="mw-page-title-main">WR 24</span> Wolf-Rayet star in the constellation Carina

WR 24 is a Wolf-Rayet star in the constellation Carina. It is one of the most luminous stars known. At the edge of naked eye visibility it is also one of the brightest Wolf Rayet stars in the sky.

<span class="mw-page-title-main">WR 148</span> Binary star in the constellation of Cygnus

WR 148 is a spectroscopic binary in the constellation Cygnus. The primary star is a Wolf–Rayet star and one of the most luminous stars known. The secondary has been suspected of being a stellar-mass black hole but may be a class O main sequence star.

<span class="mw-page-title-main">Trumpler 16</span> Massive open cluster in the constellation Carina

Trumpler 16 is a massive open cluster that is home to some of the most luminous stars in the Milky Way galaxy. It is situated within the Carina Nebula complex in the Carina–Sagittarius Arm, located approximately 9,270 ly (2,842 pc) from Earth. The cluster has one star visible to the naked eye from the tropics southward, Eta Carinae.

<span class="mw-page-title-main">QZ Carinae</span> Star system in the constellation Carina

QZ Carinae is a multiple star system in the constellation Carina. It is the brightest member of the loose open cluster Collinder 228 and one of the brightest stars in the Carina Nebula. The apparent magnitude is variable from +6.16 to +6.49 with a period of 6 days.

HD 93403 is a spectroscopic binary containing two highly luminous hot blue stars. It is 10,000 light years away in the Carina Nebula in the constellation Carina. It appears to have spectral type O5.5III, but this is composed of two spectra from a blue supergiant and blue main sequence star of spectral type O5.5I and O7V respectively. The two stars orbit every 15 days with a separation that varies from 93 R☉ to 149 R☉. The binary is shedding mass at the high rate of 0.0005 M☉ per year.

<span class="mw-page-title-main">HD 65750</span> Star in the constellation Carina

HD 65750, also known as V341 Carinae is a bright red giant star in the constellation Carina. It is surrounded by a prominent reflection nebula, known as IC 2220, nicknamed the Toby Jug Nebula.

<span class="mw-page-title-main">V528 Carinae</span> Star in the constellation Carina

V528 Carinae is a variable star in the constellation Carina.

<span class="mw-page-title-main">HD 151932</span> Star in the constellation of Scorpius

HD 151932, also known as WR 78, is a Wolf-Rayet star located in the constellation Scorpius, close to the galactic plane. Its distance is around 1,300 parsecs away from the Earth. Despite being a blue-colored Wolf-Rayet star, it is extremely reddened by interstellar extinction, so its apparent magnitude is brighter for longer-wavelength passbands. HD 151932 lies about 22′ west of the open cluster NGC 6231, the center of the OB association Scorpius OB1; it is not clear whether it is a part of the association or not. With an apparent magnitude of about 6.5, it is one of the few Wolf-Rayet stars that can be seen with the naked eye.

<span class="mw-page-title-main">Collinder 228</span>

Collinder 228 is an open cluster within the southern part of the Carina Nebula NGC 3372, about 25' south of η Carinae. It is probably composed of stars which recently formed from the material in the nebula. QZ Carinae is the brightest member of Collinder 228 with an apparent magnitude between 6.16–6.49 .

References

  1. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. 1 2 3 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  3. ↑ Sota, A.; Maíz Apellániz, J.; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J. (2014). "The Galactic O-Star Spectroscopic Survey (GOSSS). II. Bright Southern Stars". The Astrophysical Journal Supplement Series. 211 (1): 84. arXiv: 1312.6222 . Bibcode:2014ApJS..211...10S. doi:10.1088/0067-0049/211/1/10. S2CID   118847528. 10.
  4. 1 2 Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  5. 1 2 3 4 5 6 Morrell, N. I.; Barbá, R. H.; Niemela, V. S.; Corti, M. A.; Albacete Colombo, J. F.; Rauw, G.; Corcoran, M.; Morel, T.; Bertrand, J.-F.; Moffat, A. F. J.; St-Louis, N. (2001). "Optical spectroscopy of X-Mega targets - II. The massive double-lined O-type binary HD 93205". Monthly Notices of the Royal Astronomical Society. 326 (1): 85–94. arXiv: astro-ph/0105014 . Bibcode:2001MNRAS.326...85M. doi: 10.1046/j.1365-8711.2001.04500.x . S2CID   16221731.
  6. 1 2 3 4 5 Benvenuto, O. G.; Serenelli, A. M.; Althaus, L. G.; Barbá, R. H.; Morrell, N. I. (2002). "Calculation of the masses of the binary star HD 93205 by application of the theory of apsidal motion". Monthly Notices of the Royal Astronomical Society. 330 (2): 435–442. arXiv: astro-ph/0110662 . Bibcode:2002MNRAS.330..435B. doi: 10.1046/j.1365-8711.2002.05083.x . S2CID   16834579.
  7. 1 2 3 4 5 Antokhina; et al. (2000). "Light Curve Solution of HD 93205 (O3 V + O8 V) Containing the Earliest Known Star in a Well-studied Binary". The Astrophysical Journal . 529 (1): 463–476. Bibcode:2000ApJ...529..463A. doi: 10.1086/308228 . S2CID   117107602.
  8. ↑ "Hipparcos Tools Interactive Data Access". Hipparcos. ESA. Retrieved 8 December 2021.
  9. ↑ van Genderen, A. M.; Alphenaar, P.; van der Bij, M. D. P.; Deul, E. R.; van Driel, W.; van Heerde, G. M.; de Lange, L.; van Leeuwen, F.; Meys, J. J. M.; Oppe, J.; The, P. S.; Wiertz, M. J. J. (August 1985). "An investigation of the micro-variations of highly luminous OBA type stars .I". Astronomy and Astrophysics, Suppl. Ser. 61: 213–220. Bibcode:1985A&AS...61..213V . Retrieved 11 January 2025.
  10. ↑ Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V. (July 2001). "The 76th Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 5135: 1–67. Bibcode:2001IBVS.5135....1K . Retrieved 11 January 2025.
  11. ↑ Shull, J. Michael; Darling, Jeremy; Danforth, Charles W. (2021). "Gaia EDR3 Parallax Distances to the Great Carina Nebula and Its Star Clusters (Trumpler 14, 15, 16)". The Astrophysical Journal. 914 (1): 18. arXiv: 2103.07922 . Bibcode:2021ApJ...914...18S. doi: 10.3847/1538-4357/abf4d8 . S2CID   232233703.
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