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HD 73882

Coordinates: Sky map 08h 39m 09.5341s, −40° 25′ 09.2608″
From Wikipedia, the free encyclopedia
HD 73882

A light curve for NX Velorum, plotted from Hipparcos data[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Vela
Right ascension 08h 39m 09.5341s
Declination −40° 25′ 09.2608″
Apparent magnitude (V) 7.19 - 7.29[2]
Characteristics
Evolutionary stage subgiant
Spectral type O8.5IV[3]
Apparent magnitude (g) 7.356[4]
Variable type eclipsing[5]
Astrometry
Radial velocity (Rv)3.56±0.13[6] km/s
Proper motion (μ) RA: -4.71±0.05 mas/yr[4]
Dec.: 3.44±0.06 mas/yr[4]
Parallax (π)1.34 ± 0.06 mas[4]
Distance2,400 ± 100 ly
(750 ± 30 pc)
Absolute magnitude (MV)2.46±0.17[7]
Details
Metallicity [Fe/H]−0.60±0.10[6] dex
Other designations
2MASS J08390953-4025092, CD-39 4631, HIP 42433, GSC 07666-01830, PPM 313370, NX Vel
HD 73882A: TYC 7666-1830-1, Gaia DR2 5528383187882877312
HD 73882B: TYC 7666-1830-2, Gaia DR2 5528383192183392768
Database references
SIMBADdata

HD 73882 is a visual binary system with the components separated by 0.6″ and a combined spectral class of O8.[8] One of stars is an eclipsing binary system. The period of variability is listed as both 2.9199 days and 20.6 days, possibly due to the secondary being a spectroscopic binary star.[9][10]

The system lies in the constellation of Vela about 2,400 light years away from the Sun and is a member of the open cluster Ruprecht 64.[11]

Components

[edit]

The apparent magnitudes of the visible components A and B are 7.8 and 8.8 respectively. The primary, A, is thought to be the eclipsing binary. It shows eclipses every 1.5 d,[12] but there are thought to be both primary and secondary minima with the actual orbital period being 2.92 d.[9] Additional radial velocity variations with a period of 20.6 d have also been found, suggesting that one of the components is a spectroscopic binary.[9]

The spectral types of the individual components are not known. The observed combined spectral type is variously given as O8.5V, O9III, or O8.5IV.[13] The spectrum is presumed to be dominated by the primary pair which are more than a magnitude brighter than the secondary. The eclipsing components are likely to be two similar stars since the primary and secondary eclipses are almost identical. One source gives the combined mass of the eclipsing pair as 26.6 M☉ and the mass of the secondary as 2.31 M☉, with an orbital period of about 643 years, but this is highly speculative with no reliable orbits available and even the number of components uncertain.[12]

Circumstellar nebula

[edit]

The star system, located behind the Vela Supernova Remnant,[14] is obscured by the translucent nebula Gum 14 [it], located near the Vela Molecular Ridge nebulae complex. The nebula is illuminated by this star system and probably has a close physical association with it, together with brighter reflection nebula NGC 2626. The nebulae are rich in hydrogen (including deuterated hydrogen)[15] and also contain detectable amounts of sodium, carbon monoxide, and other carbon compounds,[3] including polycyclic aromatic hydrocarbons,[16] and thiols.[17] The nebula associated with the HD 73882 is one of the few exhibiting emission from compounds containing three carbon atoms.[18] The nebula has unusually low levels of oxygen compared to the average interstellar medium.[19]

References

[edit]
  1. ^ "Light Curve". Hipparcos ESA. ESA. Retrieved 17 February 2022.
  2. ^ "NX Velorum", International Variable Star Index, retrieved 2022-01-03
  3. ^ a b Snow, T. P.; Rachford, B. L.; Tumlinson, J.; Shull, J. M.; Welty, D. E.; Blair, W. P.; Ferlet, R.; Friedman, S. D.; Gry, C.; Jenkins, E. B.; Lecavelier, A.; Lemoine, M.; Morton, D. C.; Savage, B. D.; Sembach, K. R.; Vidal-Madjar, A.; York, D. G.; Andersson, B-G; Feldman, P. D.; Moos, H. W. (1999), "[ITAL]Far Ultraviolet Spectroscopic Explorer[/ITAL] Observations of Molecular Hydrogen in Translucent Interstellar Clouds: The Line of Sight toward HD 73882", The Astrophysical Journal, 538: L65–L68, arXiv:astro-ph/0005090, doi:10.1086/312791, S2CID 119349223
  4. ^ a b c 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.
  5. ^ Samus, N. N.; et al. (2017), "General Catalogue of Variable Stars", Astronomy Reports, 5.1, 61 (1): 80–88, Bibcode:2017ARep...61...80S, doi:10.1134/S1063772917010085, S2CID 125853869, retrieved 2021-11-27
  6. ^ a b De Cia, Annalisa; Jenkins, Edward B.; Fox, Andrew J.; Ledoux, Cédric; Ramburuth-Hurt, Tanita; Konstantopoulou, Christina; Petitjean, Patrick; Krogager, Jens-Kristian (2021), "Large metallicity variations in the Galactic interstellar medium", Nature, 597 (7875): 206–208, arXiv:2109.03249, Bibcode:2021Natur.597..206D, doi:10.1038/s41586-021-03780-0, PMID 34497395, S2CID 237439613
  7. ^ Bagnulo, Stefano; Cox, Nick L. J.; Cikota, Aleksandar; Siebenmorgen, Ralf; Voshchinnikov, Nikolai V.; Patat, Ferdinando; Smith, Keith T.; Smoker, Jonathan V.; Taubenberger, Stefan; Kaper, Lex; Cami, Jan; the LIPS collaboration (2017), "Large Interstellar Polarisation Survey (LIPS)", Astronomy & Astrophysics, 608: A146, arXiv:1710.02439, doi:10.1051/0004-6361/201731459, S2CID 119431016
  8. ^ Shull, J. Michael; Danforth, Charles W. (2019), "Distances to Galactic OB Stars: Photometry versus Parallax", The Astrophysical Journal, 882 (2): 180, arXiv:1907.13148, Bibcode:2019ApJ...882..180S, doi:10.3847/1538-4357/ab357d, S2CID 199000762
  9. ^ a b c Sota, A.; Apellániz, J. Maíz; Morrell, N. I.; Barbá, R. H.; Walborn, N. R.; Gamen, R. C.; Arias, J. I.; Alfaro, E. J. (2013), "The Galactic O-Star Spectroscopic Survey (Gosss). Ii. Bright Southern Stars", The Astrophysical Journal Supplement Series, 211 (1): 10, arXiv:1312.6222, Bibcode:2014ApJS..211...10S, doi:10.1088/0067-0049/211/1/10, S2CID 118847528
  10. ^ 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 Series, 215 (1): 15, arXiv:1409.6304, Bibcode:2014ApJS..215...15S, doi:10.1088/0067-0049/215/1/15, S2CID 53500788
  11. ^ Kharchenko, N. V.; Piskunov, A. E.; Röser, S.; Schilbach, E.; Scholz, R.-D. (2005), "Astrophysical parameters of Galactic open clusters", Astronomy and Astrophysics, 438 (3): 1163–1173, arXiv:astro-ph/0501674, Bibcode:2005A&A...438.1163K, doi:10.1051/0004-6361:20042523, S2CID 9079873
  12. ^ a b Tokovinin, Andrei (2018-03-01). "The Updated Multiple Star Catalog". The Astrophysical Journal Supplement Series. 235 (1): 6. arXiv:1712.04750. Bibcode:2018ApJS..235....6T. doi:10.3847/1538-4365/aaa1a5. ISSN 0067-0049. S2CID 119047709.
  13. ^ Skiff, B. A (2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009-2016)". VizieR On-line Data Catalog: B/Mk. Originally Published in: Lowell Observatory (October 2014). 1. Bibcode:2014yCat....1.2023S.
  14. ^ Kameswara Rao, N.; Lambert, David L.; Reddy, Arumalla B. S.; Gupta, Ranjan; Muneer, S.; Singh, Harinder P. (2017), "Unveiling Vela - Time Variability of Interstellar Lines in the Direction of the Vela Supernova Remnant II. Na D and Ca II", Monthly Notices of the Royal Astronomical Society: stx139, arXiv:1701.04349, doi:10.1093/mnras/stx139
  15. ^ Ferlet, R.; André, M.; Hébrard, G.; Lecavelier Des Etangs, A.; Lemoine, M.; Pineau Des Forêts, G.; Roueff, E.; Rachford, B. L.; Shull, J. M.; Snow, T. P.; Tumlinson, J.; Vidal-Madjar, A.; York, D. G.; Moos, H. W. (2000), "[ITAL]Far Ultraviolet Spectroscopic Explorer[/ITAL] Observations of the HD Molecule toward HD 73882", The Astrophysical Journal, 538: L69–L72, arXiv:astro-ph/0006039, doi:10.1086/312799, S2CID 16667758
  16. ^ Shaw, Gargi; Ferland, G. J. (2021), "Role of Polycyclic Aromatic Hydrocarbons on the Cosmic-Ray ionization rate in the Galaxy", The Astrophysical Journal, 908 (2): 138, arXiv:2101.03732, Bibcode:2021ApJ...908..138S, doi:10.3847/1538-4357/abdab2, S2CID 231573427
  17. ^ Zhao, D.; Galazutdinov, G. A.; Linnartz, H.; Krełowski, J. (2015), "Mercapto radical (SH) in translucent interstellar clouds", Astronomy & Astrophysics, 579: L1, Bibcode:2015A&A...579L...1Z, doi:10.1051/0004-6361/201526488, hdl:1887/48698
  18. ^ Schmidt, M. R.; Krełowski, J.; Galazutdinov, G. A.; Zhao, D.; Haddad, M. A.; Ubachs, W.; Linnartz, H. (2014), "Detection of vibronic bands of C3 in a translucent cloud towards HD 169454", Monthly Notices of the Royal Astronomical Society, 441 (2): 1134–1146, arXiv:1403.7280, Bibcode:2014MNRAS.441.1134S, doi:10.1093/mnras/stu641
  19. ^ Zuo, Wenbo; Li, Aigen; Zhao, Gang (2021), "Interstellar Extinction and Elemental Abundances: Individual Sight Lines", The Astrophysical Journal Supplement Series, 257 (2): 63, arXiv:2111.03903, Bibcode:2021ApJS..257...63Z, doi:10.3847/1538-4365/ac2cc3, S2CID 243847325
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