HD 93129 is found at the centre of the massive Trumpler 14open cluster in the Carina Nebula star forming region. It is too far away for its distance to have been accurately determined using the annual parallax method, but accurate distances for η Carinae and the Homunculus Nebula, modelling of clusters, and astrophysical data about other stars assumed to be within the same region, all lead to a distance around 2,300 parsecs.[5] HD 93129 Aa is the closest O2 supergiant to Earth.[13]
That volume of space is home to many other massive and luminous stars. HD 93128, yet another O3.5 main sequence star, is only 24' away within Trumpler 14, and HD 93250 and HD 93205 are two more O3.5 stars in the larger Trumpler 16 cluster around η Carinae. There are also three Wolf-Rayet stars, an O4 supergiant, many other class O stars, and the unique η Carinae itself.[10]
Systemedit
Image of the star clusterTrumpler 14 with HD 93129 A being the brightest star in the image, and HD 93129 B close but clearly resolved
HD 93129 consists of two clearly resolved components, HD 93129 A and HD 93129 B, and HD 93129 A itself is made up of two much closer stars.
HD 93129 A has been resolved into two components. The spectrum is dominated by the brighter component, although the secondary is only 0.9 magnitudes fainter. HD 93129 Aa is an O2 supergiant and Ab is an O3.5 main sequence star.[14] Their separation has decreased from 55 mas in 2004 to only 27 mas in 2013, but an accurate orbit is not available.[13]
HD 93129 B is an O3.5 main-sequence star 3 arc-seconds away from the closer pair. It is about 1.5 magnitudes fainter than the combined HD 93129 A, and approximately the same brightness as HD 93129 Ab.[1][3]
A further 5 fainter stars within 5 arc-seconds have been detected, between five and seven magnitudes fainter at infrared wavelengths.[13]
Propertiesedit
All three stars of HD 93129 are among the most luminous in the galaxy;[5] 1,480,000 L☉ for the supergiant primary and 575,000 L☉ for each of the other two stars. They are also among the hottest, with the supergiant at 42,500 K and the other two at 52,000 K. The stars have masses calculated to be between 70 M☉ and 110 M☉.
HD 93129Aa has left the main sequence and its age is estimated to be around 900,000 years. The existence of the zero-age main sequence stars within Trumpler 14 suggest its age may be less than 600,000 years.[7]
^ abcdefHøg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862. ISBN0333750888.
^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.
^ abcdefVazquez, R. A.; Baume, G.; Feinstein, A.; Prado, P. (1996). "Investigation on the region of the open cluster TR 14". Astronomy and Astrophysics Supplement. 116: 75. Bibcode:1996A&AS..116...75V.
^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. 211 (1): 10. arXiv:1312.6222. Bibcode:2014ApJS..211...10S. doi:10.1088/0067-0049/211/1/10. S2CID 118847528.
^ abcdCohen, D. H.; Gagné, M.; Leutenegger, M. A.; MacArthur, J. P.; Wollman, E. E.; Sundqvist, J. O.; Fullerton, A. W.; Owocki, S. P. (2011). "Chandra X-ray spectroscopy of the very early O supergiant HD 93129A: Constraints on wind shocks and the mass-loss rate". Monthly Notices of the Royal Astronomical Society. 415 (4): 3354–3364. arXiv:1104.4786. Bibcode:2011MNRAS.415.3354C. doi:10.1111/j.1365-2966.2011.18952.x. S2CID 8258609.
^Maíz Apellániz, J.; Sota, A.; Arias, J. I.; Barbá, R. H.; Walborn, N. R.; Simón-Díaz, S.; Negueruela, I.; Marco, A.; Leão, J. R. S.; Herrero, A.; Gamen, R. C.; Alfaro, E. J. (2016). "The Galactic O-Star Spectroscopic Survey (GOSSS). III. 142 Additional O-type Systems". The Astrophysical Journal Supplement Series. 224 (1): 4. arXiv:1602.01336. Bibcode:2016ApJS..224....4M. doi:10.3847/0067-0049/224/1/4. S2CID 55658165.
^ abcdPenny, Laura R.; Gies, Douglas R.; Hartkopf, William I.; Mason, Brian D.; Turner, Nils H. (1993). "The frequency of binary stars in the young cluster Trumpler 14". Publications of the Astronomical Society of the Pacific. 105: 588. Bibcode:1993PASP..105..588P. doi:10.1086/133200.
^ abcNelan, Edmund P.; Walborn, Nolan R.; Wallace, Debra J.; Moffat, Anthony F. J.; Makidon, Russell B.; Gies, Douglas R.; Panagia, Nino (2004). "Resolving OB Systems in the Carina Nebula with the Hubble Space Telescope Fine Guidance Sensor". The Astronomical Journal. 128 (1): 323–329. Bibcode:2004AJ....128..323N. doi:10.1086/420716. S2CID 121115585.
^ abcdRepolust, T.; Puls, J.; Herrero, A. (2004). "Stellar and wind parameters of Galactic O-stars. The influence of line-blocking/blanketing". Astronomy and Astrophysics. 415: 349–376. Bibcode:2004A&A...415..349R. doi:10.1051/0004-6361:20034594.
^ abcdSmith, Nathan (2006). "A census of the Carina Nebula - I. Cumulative energy input from massive stars". Monthly Notices of the Royal Astronomical Society. 367 (2): 763–772. arXiv:astro-ph/0601060. Bibcode:2006MNRAS.367..763S. doi:10.1111/j.1365-2966.2006.10007.x. S2CID 14060690.
^ abDel Palacio, Santiago; Bosch-Ramon, Valentí; Romero, Gustavo E.; Benaglia, Paula (2016). "A model for the non-thermal emission of the very massive colliding-wind binary HD 93129A". Astronomy & Astrophysics. 591: A139. arXiv:1604.07294. Bibcode:2016A&A...591A.139D. doi:10.1051/0004-6361/201628264. S2CID 55216290.
^ abcdVink, Jorick S; Davies, B; Harries, T. J; Oudmaijer, R. D; Walborn, N. R (2009). "On the presence and absence of disks around O-type stars". Astronomy and Astrophysics. 505 (2): 743. arXiv:0909.0888. Bibcode:2009A&A...505..743V. doi:10.1051/0004-6361/200912610. S2CID 16636438.
^ abcSana, H.; Le Bouquin, J.-B.; Lacour, S.; Berger, J.-P.; Duvert, G.; Gauchet, L.; Norris, B.; Olofsson, J.; Pickel, D.; Zins, G.; Absil, O.; De Koter, A.; Kratter, K.; Schnurr, O.; Zinnecker, H. (2014). "Southern Massive Stars at High Angular Resolution: Observational Campaign and Companion Detection". The Astrophysical Journal Supplement. 215 (1): 15. arXiv:1409.6304. Bibcode:2014ApJS..215...15S. doi:10.1088/0067-0049/215/1/15. S2CID 53500788.
^Benaglia, P.; Koribalski, B. (2004). "Radio observations of HD 93129A: The earliest O star with the highest mass loss?". Astronomy & Astrophysics. 416 (1): 171–178. arXiv:astro-ph/0312003. Bibcode:2004A&A...416..171B. doi:10.1051/0004-6361:20034138. S2CID 18416034.
93129, triple, star, system, carina, nebula, with, three, components, being, class, stars, amongst, most, luminous, stars, milky, dominant, member, trumpler, star, cluster, young, star, cluster, within, carina, stellar, association, that, harbors, other, super. 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 HD 93129HD 93129 surrounded by the lesser stars of Trumpler 14Credit NASA amp ESA Jesus Maiz Apellaniz Instituto de Astrofisica de Andalucia Observation dataEpoch J2000 Equinox J2000Constellation CarinaRight ascension 10h 43m 57 5s 1 Declination 59 32 51 3 1 Apparent magnitude V 6 90 2 7 310 1 8 84 3 CharacteristicsASpectral type O2If 4 O2If O3 5V 5 U B color index 0 81 3 B V color index 0 25 3 BEvolutionary stage main sequenceSpectral type O3 5 V f z 6 U B color index 0 79 3 B V color index 0 23 3 AstrometryRadial velocity Rv 0 4 7 4 7 km sProper motion m RA 5 0 1 mas yr Dec 17 0 1 mas yrDistance2 300 5 pcAbsolute magnitude MV A 6 5 6 1 5 2 B 4 9 8 DetailsAaMass110 8 M Radius22 5 9 R Luminosity1 480 000 10 L Surface gravity log g 3 71 9 cgsTemperature42 500 9 KRotational velocity v sin i 130 9 km sAge0 9 0 2 0 4 7 MyrAbMass70 8 M Radius13 1 11 R Luminosity575 000 10 L Temperature44 000 11 KBMass52 12 M Radius13 12 R Luminosity575 000 10 L Surface gravity log g 3 92 12 cgsTemperature44 000 12 KRotational velocity v sin i 112 7 km sOther designationsCD 58 3528 Trumpler 14 1 CCDM J10440 5933 WDS J10440 5933A TYC 8626 2805 1 ALS 15862 LS 1820B ALS 19309Database referencesSIMBADHD 93129HD 93129 AHD 93129 B Contents 1 Location 2 System 3 Properties 4 See also 5 References 6 External linksLocation edit nbsp The Carina Nebula with h Carinae on the left and Trumpler 14 just right of centerHD 93129 is found at the centre of the massive Trumpler 14 open cluster in the Carina Nebula star forming region It is too far away for its distance to have been accurately determined using the annual parallax method but accurate distances for h Carinae and the Homunculus Nebula modelling of clusters and astrophysical data about other stars assumed to be within the same region all lead to a distance around 2 300 parsecs 5 HD 93129 Aa is the closest O2 supergiant to Earth 13 That volume of space is home to many other massive and luminous stars HD 93128 yet another O3 5 main sequence star is only 24 away within Trumpler 14 and HD 93250 and HD 93205 are two more O3 5 stars in the larger Trumpler 16 cluster around h Carinae There are also three Wolf Rayet stars an O4 supergiant many other class O stars and the unique h Carinae itself 10 System edit nbsp Image of the star cluster Trumpler 14 with HD 93129 A being the brightest star in the image and HD 93129 B close but clearly resolvedHD 93129 consists of two clearly resolved components HD 93129 A and HD 93129 B and HD 93129 A itself is made up of two much closer stars HD 93129 A has been resolved into two components The spectrum is dominated by the brighter component although the secondary is only 0 9 magnitudes fainter HD 93129 Aa is an O2 supergiant and Ab is an O3 5 main sequence star 14 Their separation has decreased from 55 mas in 2004 to only 27 mas in 2013 but an accurate orbit is not available 13 HD 93129 B is an O3 5 main sequence star 3 arc seconds away from the closer pair It is about 1 5 magnitudes fainter than the combined HD 93129 A and approximately the same brightness as HD 93129 Ab 1 3 A further 5 fainter stars within 5 arc seconds have been detected between five and seven magnitudes fainter at infrared wavelengths 13 Properties editAll three stars of HD 93129 are among the most luminous in the galaxy 5 1 480 000 L for the supergiant primary and 575 000 L for each of the other two stars They are also among the hottest with the supergiant at 42 500 K and the other two at 52 000 K The stars have masses calculated to be between 70 M and 110 M HD 93129Aa has left the main sequence and its age is estimated to be around 900 000 years The existence of the zero age main sequence stars within Trumpler 14 suggest its age may be less than 600 000 years 7 See also editTrumpler 14 Mystic Mountain List of most massive starsReferences edit a b c d e f Hog E Fabricius C Makarov V V Urban S Corbin T Wycoff G Bastian U Schwekendiek P Wicenec A 2000 The Tycho 2 catalogue of the 2 5 million brightest stars Astronomy and Astrophysics 355 L27 Bibcode 2000A amp A 355L 27H doi 10 1888 0333750888 2862 ISBN 0333750888 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 a b c d e f Vazquez R A Baume G Feinstein A Prado P 1996 Investigation on the region of the open cluster TR 14 Astronomy and Astrophysics Supplement 116 75 Bibcode 1996A amp AS 116 75V Sota A Maiz Apellaniz J Morrell N I Barba 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 211 1 10 arXiv 1312 6222 Bibcode 2014ApJS 211 10S doi 10 1088 0067 0049 211 1 10 S2CID 118847528 a b c d Cohen D H Gagne M Leutenegger M A MacArthur J P Wollman E E Sundqvist J O Fullerton A W Owocki S P 2011 Chandra X ray spectroscopy of the very early O supergiant HD 93129A Constraints on wind shocks and the mass loss rate Monthly Notices of the Royal Astronomical Society 415 4 3354 3364 arXiv 1104 4786 Bibcode 2011MNRAS 415 3354C doi 10 1111 j 1365 2966 2011 18952 x S2CID 8258609 Maiz Apellaniz J Sota A Arias J I Barba R H Walborn N R Simon Diaz S Negueruela I Marco A Leao J R S Herrero A Gamen R C Alfaro E J 2016 The Galactic O Star Spectroscopic Survey GOSSS III 142 Additional O type Systems The Astrophysical Journal Supplement Series 224 1 4 arXiv 1602 01336 Bibcode 2016ApJS 224 4M doi 10 3847 0067 0049 224 1 4 S2CID 55658165 a b c d Penny Laura R Gies Douglas R Hartkopf William I Mason Brian D Turner Nils H 1993 The frequency of binary stars in the young cluster Trumpler 14 Publications of the Astronomical Society of the Pacific 105 588 Bibcode 1993PASP 105 588P doi 10 1086 133200 a b c Nelan Edmund P Walborn Nolan R Wallace Debra J Moffat Anthony F J Makidon Russell B Gies Douglas R Panagia Nino 2004 Resolving OB Systems in the Carina Nebula with the Hubble Space Telescope Fine Guidance Sensor The Astronomical Journal 128 1 323 329 Bibcode 2004AJ 128 323N doi 10 1086 420716 S2CID 121115585 a b c d Repolust T Puls J Herrero A 2004 Stellar and wind parameters of Galactic O stars The influence of line blocking blanketing Astronomy and Astrophysics 415 349 376 Bibcode 2004A amp A 415 349R doi 10 1051 0004 6361 20034594 a b c d Smith Nathan 2006 A census of the Carina Nebula I Cumulative energy input from massive stars Monthly Notices of the Royal Astronomical Society 367 2 763 772 arXiv astro ph 0601060 Bibcode 2006MNRAS 367 763S doi 10 1111 j 1365 2966 2006 10007 x S2CID 14060690 a b Del Palacio Santiago Bosch Ramon Valenti Romero Gustavo E Benaglia Paula 2016 A model for the non thermal emission of the very massive colliding wind binary HD 93129A Astronomy amp Astrophysics 591 A139 arXiv 1604 07294 Bibcode 2016A amp A 591A 139D doi 10 1051 0004 6361 201628264 S2CID 55216290 a b c d Vink Jorick S Davies B Harries T J Oudmaijer R D Walborn N R 2009 On the presence and absence of disks around O type stars Astronomy and Astrophysics 505 2 743 arXiv 0909 0888 Bibcode 2009A amp A 505 743V doi 10 1051 0004 6361 200912610 S2CID 16636438 a b c Sana H Le Bouquin J B Lacour S Berger J P Duvert G Gauchet L Norris B Olofsson J Pickel D Zins G Absil O De Koter A Kratter K Schnurr O Zinnecker H 2014 Southern Massive Stars at High Angular Resolution Observational Campaign and Companion Detection The Astrophysical Journal Supplement 215 1 15 arXiv 1409 6304 Bibcode 2014ApJS 215 15S doi 10 1088 0067 0049 215 1 15 S2CID 53500788 Benaglia P Koribalski B 2004 Radio observations of HD 93129A The earliest O star with the highest mass loss Astronomy amp Astrophysics 416 1 171 178 arXiv astro ph 0312003 Bibcode 2004A amp A 416 171B doi 10 1051 0004 6361 20034138 S2CID 18416034 External links edithttp jumk de astronomie big stars hd 93129a shtml Retrieved from https en wikipedia org w index php title HD 93129 amp oldid 1187186584, wikipedia, wiki, book, books, library,
