HD 73882 is a visual binary system with the components separated by0.6″ and a combined spectral class of O8.[8] One of stars is aneclipsing binary system. The period of variability is listed as both 2.9199 days and 20.6 days, possibly due to the secondary being aspectroscopic binary star.[9][10]
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 every1.5 d,[12] but there are thought to be both primary and secondary minima with the actual orbital period being2.92 d.[9] Additional radial velocity variations with a period of20.6 d have also been found, suggesting that one of the components is aspectroscopic 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]
The star system, located behind theVela Supernova Remnant,[14] is obscured by the translucent nebulaGum 14 [it], located near theVela 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 nebulaNGC 2626. The nebulae are rich in hydrogen (including deuterated hydrogen)[15] and also contain detectable amounts ofsodium,carbon monoxide, and other carbon compounds,[3] includingpolycyclic aromatic hydrocarbons,[16] andthiols.[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]
^"Light Curve".Hipparcos ESA. ESA. Retrieved17 February 2022.
^"NX Velorum",International Variable Star Index, retrieved2022-01-03
^abSnow, 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,S2CID119349223
^abcSota, 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,S2CID118847528
^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,S2CID53500788
^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.
^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
^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,S2CID16667758
^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
