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Trumpler 16

Coordinates:Sky map10h45m10s,−59° 43′ 00″
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Trumpler 16
The inner region of theCarina Nebulaas seen in near-infrared. Trumpler 16 is the cluster of stars at the left, aroundEta Carinae(the brightest star in the image).
Observation data (J2000epoch)
Right ascension10h45m10s[1]
Declination−59° 43′ 00″[1]
Distance9,270ly(2,842pc)[1]
Apparent magnitude(V)5.0[1]
Physical characteristics
Other designationsCr234,C 1043-594,Cl VDBH 105,OCl 829.0,[KPR2004b] 265,[KPS2012] MWSC 1850[1]
Associations
ConstellationCarina
See also:Open cluster,List of open clusters

Trumpler 16(Tr 16) is a massiveopen clusterthat is home to some of the most luminous stars in theMilky Waygalaxy. It is situated within theCarina Nebulacomplex in theCarina–Sagittarius Arm,located approximately 9,270ly(2,842pc) from Earth.[1]The cluster has one star visible to the naked eye fromthe tropicssouthward,Eta Carinae.

Description

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Its most luminous members areEta CarinaeandWR 25,with both havingluminositiesseveral million times that of the Sun, and there are three other extreme stars with O3spectral classes.[2]BothEta CarinaeandWR 25arebinaries,with the primary stars contributing most of the luminosity, but with companions which are themselves more massive and luminous than most stars. Totalling all wavelengths,Eta Carinaeis estimated to be the more luminous of the two, 4,600,000 times the Sun's luminosity (absolute bolometric magnitude−12) compared toWR 25at 2,400,000 times the Sun's luminosity (absolute bolometric magnitude −11.2). However,Eta Carinaeappears by far the brightest object, both because it is brighter in visual wavelengths and because it is embedded in nebulosity which exaggerates the luminosity.WR 25is very hot and emits most of its radiation atultravioletwavelengths.

Prominent stars
Star name MJ number Effective temperature (K) Absolute magnitude Bolometric magnitude Mass (M☉) Spectral type Ref.
η Car(HD 93308) 35200+37200 −8.6 −12 100+30 LBV+O [3][4][5]
WR 25(HD 93162) 245 50100 −6.98 −11.2 98 O2.5If*/WN6+OB [6][7]
HD 93250 383 46000 −6.14 −10.5 83 O4IV(fc) [8][9]
V560 Car(HD 93205) 342 51300+38000 −5.87 + −4.32 −10.4 + −7.9 40+17 O3.5Vf+O8V [10][11][7]
HD 303308 480 51300 −5.9 −10.4 93 O3V [12]
HD 93204 340 46100 −5.4 −9.6 59 O5V [12]
CPD-59 2600 380 43600 −5.5 −9.6 55 O6V [12]
CPD-59 2641 535 43600 −5.2 −9.3 49 O6V [12]
ALS 15210 257 47800 −4.3 −8.7 44 O4I [12]
CPD-59 2603 408 41000 −5.2 −9.1 43 O7V [12]
CPD-59 2636 517 38500 −5.2 −8.9 37 O8V [12]
CPD-59 2626 484 41000 −4.8 −8.7 37 O7V [12]
HD 93343 512 41000 −4.7 −8.6 37 O7V [12]
V731 Car (CPD-59 2635) 516 37200 −5 −8.6 33 O8.5V [12]
CPD-59 2591 359 38500 −4 −7.7 27 O8V [12]
HD 305518 117 34700 −4.8 −8.2 27 O9.5V [12]

Carina OB1

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Trumpler 16 and Trumpler 14 are the most prominent star clusters inCarina OB1,a giant stellar association in theCarina spiral arm.Another cluster withinCarina OB1,Collinder228,is thought to be an extension ofTrumpler 16appearing visually separated only because of an interveningdust lane.The spectral types of the stars indicate thatTrumpler 16formed by a single wave of star formation. Because of the extreme luminosity of the stars formed, their stellar winds push away the clouds of dust, similar to thePleiades.In a few million years, after the brightest stars have exploded assupernovae,the cluster will slowly die away.Trumpler 16includes most of the stars in the eastern portion of theCarina OB1association.[13]

Gaia Data Release 2

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Gaia Data Release 2provides parallaxes for many stars considered to be members of Trumpler 16. It finds that the four hottest O-class stars in the region have very similar parallaxes with a mean value of0.383±0.017mas.Many of the other supposed members show significantly different parallaxes and may be foreground or background objects. Therefore, the distance of Trumpler 16 is assumed to be around 2,600 pc, significantly further than the accurately-known distance of η Carinae.[14]

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  • Carina OB1 association, with the area of Trumpler 16 indicated
    Carina OB1association, with the area of Trumpler 16 indicated
  • Some of the stars in Tr 16: WR 25 and ALS 15210 are the brightest and third-brightest respectively in this image, the second-brightest is merely a foreground object.
    Some of the stars in Tr 16:WR 25and ALS 15210 are the brightest and third-brightest respectively in this image, the second-brightest is merely a foreground object.

See also

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References

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  1. ^abcdef"Trumpler 16".SIMBAD.Centre de données astronomiques de Strasbourg.Retrieved2 December2016.
  2. ^Wolk, Scott J.; Broos, Patrick S.; Getman, Konstantin V.; Feigelson, Eric D.; Preibisch, Thomas; et al. (May 2011). "The Chandra Carina Complex Project View of Trumpler 16".The Astrophysical Journal Supplement.194(1). 12.arXiv:1103.1126.Bibcode:2011ApJS..194...12W.doi:10.1088/0067-0049/194/1/12.S2CID13951142.
  3. ^Groh, Jose H.; Hillier, D. John; Madura, Thomas I.; Weigelt, Gerd (2012)."On the influence of the companion star in Eta Carinae: 2D radiative transfer modelling of the ultraviolet and optical spectra".Monthly Notices of the Royal Astronomical Society.423(2): 1623.arXiv:1204.1963.Bibcode:2012MNRAS.423.1623G.doi:10.1111/j.1365-2966.2012.20984.x.S2CID119205238.
  4. ^Smith, Nathan; Frew, David J. (2011)."A revised historical light curve of Eta Carinae and the timing of close periastron encounters".Monthly Notices of the Royal Astronomical Society.415(3): 2009–19.arXiv:1010.3719.Bibcode:2011MNRAS.415.2009S.doi:10.1111/j.1365-2966.2011.18993.x.S2CID118614725.
  5. ^Mehner, A.; De Wit, W.-J.; Asmus, D.; Morris, P. W.; Agliozzo, C.; Barlow, M. J.; Gull, T. R.; Hillier, D. J.; Weigelt, G. (2019). "Mid-infrared evolution of η Carinae from 1968 to 2018".Astronomy & Astrophysics.630:L6.arXiv:1908.09154.Bibcode:2019A&A...630L...6M.doi:10.1051/0004-6361/201936277.S2CID202149820.
  6. ^Sota, A.; Maíz Apellániz, J.;Morrell, N. I.;Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J.; Oskinova, L. M. (2019). "The Galactic WN stars revisited. Impact of Gaia distances on fundamental stellar parameters".Astronomy & Astrophysics.A57:625.arXiv:1904.04687.Bibcode:2019A&A...625A..57H.doi:10.1051/0004-6361/201834850.S2CID104292503.
  7. ^abSota, 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.S2CID118847528.
  8. ^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.Bibcode:2004A&A...415..349R.doi:10.1051/0004-6361:20034594.
  9. ^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.S2CID55658165.
  10. ^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"(PDF).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.S2CID16221731.
  11. ^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.S2CID16834579.
  12. ^abcdefghijklMassey, P.;Degioia-Eastwood, K.;Waterhouse, E. (2001). "The Progenitor Masses of Wolf-Rayet Stars and Luminous Blue Variables Determined from Cluster Turnoffs. II. Results from 12 Galactic Clusters and OB Associations".The Astronomical Journal.121(2): 1050–1070.arXiv:astro-ph/0010654.Bibcode:2001AJ....121.1050M.doi:10.1086/318769.S2CID53345173.
  13. ^Carraro, G.; Romaniello, M.; Ventura, P.; Patat, F. (May 2004). "The star cluster Collinder 232 in the Carina complex and its relation to Trumpler 14/16".Astronomy and Astrophysics.418(2): 525–537.arXiv:astro-ph/0401144.Bibcode:2004A&A...418..525C.doi:10.1051/0004-6361:20034335.S2CID17507621.
  14. ^Davidson, Kris; Helmel, Greta; Humphreys, Roberta M. (2018)."Gaia, Trumpler 16, and Eta Carinae".Research Notes of the American Astronomical Society.2(3): 133.arXiv:1808.02073.Bibcode:2018RNAAS...2..133D.doi:10.3847/2515-5172/aad63c.S2CID119030757.

Further reading

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