3 Camelopardalis

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3 Camelopardalis
3CamLightCurve.png
A light curve for 3 Camelopardalis, plotted from TESS data [1]
Observation data
Epoch J2000       Equinox J2000
Constellation Camelopardalis
Right ascension 04h 39m 54.682s [2]
Declination +53° 04′ 46.33″ [2]
Apparent magnitude  (V)5.073 [3]
Characteristics
Spectral type K0III [4]
U−B color index 0.89 [5]
B−V color index 1.07 [5]
Variable type suspected RS CVn [6]
Astrometry
Radial velocity (Rv)−40.50 [7]  km/s
Proper motion (μ)RA: −5.68±0.66 [2]   mas/yr
Dec.: −15.00±0.60 [2]   mas/yr
Parallax (π)7.72 ± 0.70  mas [2]
Distance 420 ± 40  ly
(130 ± 10  pc)
Absolute magnitude  (MV)−0.82 [4]
Orbit [8]
PrimaryAa
CompanionAb
Period (P)121 days
Eccentricity (e)0.02
Semi-amplitude (K1)
(primary)		28.20 km/s
Details
Aa
Mass 3.3 [9]   M☉
Radius 24.1 [9]   R☉
Luminosity 259 [9]   L☉
Surface gravity (log g)2.49 [10]   cgs
Temperature 4,715 [9]   K
Metallicity −0.21 [10]
Rotation 121 days [9]
Rotational velocity (v sin i)6.7 [4]  km/s
Ab
Mass 2.37 [11]   M☉
B
Mass 0.65 [11]   M☉
Other designations
HR  1467, HD  29317, BD+52°865, HIP  21727, SAO  24743, GC 5658, ADS  3359, CCDM 04399+5305
Database references
SIMBAD data
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.)

3 Camelopardalis is a spectroscopic and visual binary in the constellation Camelopardalis. It is approximately 496 light years from Earth.

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-type giant 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☉.

The visual companion is a 12th magnitude star.

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References

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  3. ↑ 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.
  4. 1 2 3 Eker, 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. S2CID   17747763.
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  6. 1 2 NSV 1681
  7. ↑ 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. S2CID   15290475.
  8. ↑ Pourbaix, D; Tokovinin, A. A; Batten, A. H; Fekel, F. C; Hartkopf, W. I; Levato, H; Morrell, N. I; Torres, G; Udry, S (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy & Astrophysics. 424 (2): 727–732. arXiv: astro-ph/0406573 . Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213. S2CID   119387088.
  9. 1 2 3 4 5 Gondoin, P (2007). "The rotation-activity correlation among G and K giants in binary systems". Astronomy & Astrophysics. 464 (3): 1101–1106. Bibcode:2007A&A...464.1101G. doi: 10.1051/0004-6361:20066751 .
  10. 1 2 Soubiran, Caroline; Le Campion, Jean-François; Brouillet, Nathalie; Chemin, Laurent (2016). "The PASTEL catalogue: 2016 version". Astronomy & Astrophysics. 591: A118. arXiv: 1605.07384 . Bibcode:2016A&A...591A.118S. doi:10.1051/0004-6361/201628497. S2CID   119258214.
  11. 1 2 3 Tokovinin, A (2008). "Comparative statistics and origin of triple and quadruple stars". Monthly Notices of the Royal Astronomical Society. 389 (2): 925–938. arXiv: 0806.3263 . Bibcode:2008MNRAS.389..925T. doi:10.1111/j.1365-2966.2008.13613.x. S2CID   16452670.
  12. ↑ 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.
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