The main plot is a visual band light curve for QR Vulpeculae, adapted from Pavlovski et al. (1983),[11] showing a sudden brightening. The inset plot, adapted from Lefèvre et al. (2009),[12] shows the periodic variability.
HD 192685 varies slightly in brightness and is classified as a γ Cassiopeiae variable.[2]
From October to December 1982 the Hydrogen alpha absorption line increased in emission strength by 30%.[11] The line is partially filled by redshifted emission.[13]
HD 192685 has excess infrared emissions (12-100 μm) which are interpreted to be free-free radiation in the gas surrounding the star.[14]
Companions
It has at least one companion with separation 0.55" and magnitude 7.55,[15] and may also be a long-period spectroscopic binary.[16]
Samus, N. N.; Durlevich, O. V.; etal. (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.
Mermilliod, J. C. (2006). "VizieR Online Data Catalog: Homogeneous Means in the UBV System (Mermilliod 1991)". VizieR On-line Data Catalog: II/168. Originally Published in: Institut d'Astronomie. 2168. Bibcode:2006yCat.2168....0M.Vizier catalog entry
Pavlovski, K.; Bozic, H.; Harmanec, P.; Horn, J.; Koubsky, P. (14 November 1983). "Sudden Brightening of the Recently Discovered Be Star HR 7739". Information Bulletin on Variable Stars. 2431 (1): 1. Bibcode:1983IBVS.2431....1P. ISSN0374-0676.
Green, Daniel W. E. (July 14, 1982). "2 Vul AND HR 7739". IAU Circular. IAU Central Bureau for Astronomical Telegrams. 3710. Retrieved 11 December 2012.
Cote, J. (July 1987). "B and A type stars with unexpectedly large colour excesses at IRAS wavelengths". Astronomy and Astrophysics. 181 (1): 83. Bibcode:1987A&A...181...77C. ISSN0004-6361.
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