3 Camelopardalis is a visual binary with the two components separated by 3.7". The brighter of the pair is also a single-lined spectroscopic binary with an orbital period of 121 days.[11]
The primary component, 3 Camelopardalis Aa, is an orange
K-typegiant with a mean
apparent magnitude of +5.07. It rotates once every 121 days, matching the orbital period with its close companion. It was thought to be a short period
Cepheid variable[12] when it was first investigated, but has since been classified as a probable
RS Canum Venaticorum variable. The total amplitude of its variations is less than 0.1 magnitudes.[6]
The spectroscopic companion has not been observed directly and its cannot be detected in the spectrum. It is inferred on the basis of
radial velocity variations in its brighter companion. Assuming a circular orbit, it has a mass of 2.37 M☉.
^Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27.
Bibcode:
2000A&A...355L..27H.
^
abcEker, Z; Ak, N. Filiz; Bilir, S; Doğru, D; Tüysüz, M; Soydugan, E; Bakış, H; Uğraş, B; Soydugan, F; Erdem, A; Demircan, O (2008). "A catalogue of chromospherically active binary stars (third edition)". Monthly Notices of the Royal Astronomical Society. 389 (4): 1722.
arXiv:0805.4517.
Bibcode:
2008MNRAS.389.1722E.
doi:
10.1111/j.1365-2966.2008.13670.x.
S2CID17747763.
^
abHoffleit, D.; Warren, W. H. (1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H. 5050.
Bibcode:
1995yCat.5050....0H.
^Karataș, Yüksel; Bilir, Selçuk; Eker, Zeki; Demircan, Osman; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R.; Lowrance, Patrick; Kirkpatrick, J. Davy; Burgasser, Adam J. (2004). "Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution". Monthly Notices of the Royal Astronomical Society. 349 (3): 1069–1092.
arXiv:astro-ph/0404219.
Bibcode:
2004MNRAS.349.1069K.
doi:
10.1111/j.1365-2966.2004.07588.x.
S2CID15290475.
^MacRae, D. A. (1975). "David Dunlap Observatory, University of Toronto, Richmond Hill, Ontario, Canada. Observatory report". Bulletin of the American Astronomical Society. 7: 39.
Bibcode:
1975BAAS....7...39M.
3 Camelopardalis is a visual binary with the two components separated by 3.7". The brighter of the pair is also a single-lined spectroscopic binary with an orbital period of 121 days.[11]
The primary component, 3 Camelopardalis Aa, is an orange
K-typegiant with a mean
apparent magnitude of +5.07. It rotates once every 121 days, matching the orbital period with its close companion. It was thought to be a short period
Cepheid variable[12] when it was first investigated, but has since been classified as a probable
RS Canum Venaticorum variable. The total amplitude of its variations is less than 0.1 magnitudes.[6]
The spectroscopic companion has not been observed directly and its cannot be detected in the spectrum. It is inferred on the basis of
radial velocity variations in its brighter companion. Assuming a circular orbit, it has a mass of 2.37 M☉.
^Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27.
Bibcode:
2000A&A...355L..27H.
^
abcEker, Z; Ak, N. Filiz; Bilir, S; Doğru, D; Tüysüz, M; Soydugan, E; Bakış, H; Uğraş, B; Soydugan, F; Erdem, A; Demircan, O (2008). "A catalogue of chromospherically active binary stars (third edition)". Monthly Notices of the Royal Astronomical Society. 389 (4): 1722.
arXiv:0805.4517.
Bibcode:
2008MNRAS.389.1722E.
doi:
10.1111/j.1365-2966.2008.13670.x.
S2CID17747763.
^
abHoffleit, D.; Warren, W. H. (1995). "VizieR Online Data Catalog: Bright Star Catalogue, 5th Revised Ed. (Hoffleit+, 1991)". VizieR On-line Data Catalog: V/50. Originally Published in: 1964BS....C......0H. 5050.
Bibcode:
1995yCat.5050....0H.
^Karataș, Yüksel; Bilir, Selçuk; Eker, Zeki; Demircan, Osman; Liebert, James; Hawley, Suzanne L.; Fraser, Oliver J.; Covey, Kevin R.; Lowrance, Patrick; Kirkpatrick, J. Davy; Burgasser, Adam J. (2004). "Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution". Monthly Notices of the Royal Astronomical Society. 349 (3): 1069–1092.
arXiv:astro-ph/0404219.
Bibcode:
2004MNRAS.349.1069K.
doi:
10.1111/j.1365-2966.2004.07588.x.
S2CID15290475.
^MacRae, D. A. (1975). "David Dunlap Observatory, University of Toronto, Richmond Hill, Ontario, Canada. Observatory report". Bulletin of the American Astronomical Society. 7: 39.
Bibcode:
1975BAAS....7...39M.