BD Camelopardalis is anS star andsymbiotic star in the constellationCamelopardalis. It is a 5thmagnitude star, and is visible to thenaked eye under good observing conditions. It was recognized as aspectroscopic binary star in 1922, and its orbital solution published in 1984;[16] it has a 596-day orbital period. A spectroscopic composition analysis was done of the red giant primary star in 1986.[17]
Although the star's spectrum shows the spectral features of zirconium oxide which definespectral class S, BD Cam shows notechnetium lines in its spectrum. It is believed to be an "extrinsic" S star, one whoses-process element excesses originate in a binary companion star.
At times BD Cam is the brightest S star in the visible sky, because other bright S stars areMira variables or other types of variable star with large changes in apparent brightness. Its own brightness variability in the visible part of the spectrum is modest.
On the basis of the measurement of radial velocities of the line components it is concluded that the helium emission originates in the vicinity of the inner Lagrangian point of the system, indicating a gas motion from the red giant primary, directed to the secondary, with a velocity of about 5 km/s. At the same time, there is a high-velocity, hot wind outwards from the primary red giant with a velocity of about 50 km/s.
— Shcherbakov, A. G. and Tuominen, I.
However, HR 1105 appears to have a highly variable UV companion. In 1982, no UV flux was discerned for this system, but by 1986 C IV was strong, increasing by a factor of 3 in 1987 with prominent lines of Si III, C III, O III, Si IV, and N V.
— Ake, Thomas B., III; Johnson, Hollis R. and Perry, Benjamin F., Jr.
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^Yamashita, Y. (1967). "MK Spectral Types of Bright M-Type Stars".Publications of the Dominion Astrophysical Observatory Victoria.13: 47.Bibcode:1967PDAO...13...47Y.
^Samus, N. N.; Durlevich, O. V.; et al. (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.
^abcKhalatyan, A.; Anders, F.; Chiappini, C.; Queiroz, A. B. A.; Nepal, S.; Dal Ponte, M.; Jordi, C.; Guiglion, G.; Valentini, M.; Torralba Elipe, G.; Steinmetz, M.; Pantaleoni-González, M.; Malhotra, S.; Jiménez-Arranz, Ó.; Enke, H.; Casamiquela, L.; Ardèvol, J. (2024). "Transferring spectroscopic stellar labels to 217 million Gaia DR3 XP stars with SHBoost".Astronomy and Astrophysics.691: A98.arXiv:2407.06963.Bibcode:2024A&A...691A..98K.doi:10.1051/0004-6361/202451427.
^Kukarkin, B. V.; Kholopov, P. N.; Fedorovich, V. P.; Kireyeva, N. N.; Kukarkina, N. P.; Medvedeva, G. I.; Perova, N. B. (March 1977)."62nd Name-List of Variable Stars"(PDF).Information Bulletin on Variable Stars.1248: 1.Bibcode:1977IBVS.1248....1K. Retrieved29 December 2024.
Ake Thomas B., III; Johnson, Hollis R.; Perry Benjamin F., Jr. (1988). "Companions to peculiar red giants: HR 363 and HR 1105".In ESA, A Decade of UV Astronomy with the IUE Satellite.1:245–248.Bibcode:1988ESASP.281a.245A.