Kappa Draconis
Kappa Draconis, Latinized from κ Draconis, is a blue giant star located in the northern circumpolar constellation of Draco. At an apparent magnitude of 3.88, it is barely visible to the naked eye when artificial lighting from cities is present. Nevertheless, it is a powerful star, approximately five time as massive as the Sun. It is about 460 light-years away, and is 1,400 times brighter than the Sun.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Draco |
| Right ascension | 12h 33m 28.94206s[1] |
| Declination | +69° 47′ 17.6331″[1] |
| Apparent magnitude (V) | 3.82[2] |
| Characteristics | |
| Spectral type | B6 IIIe[3] |
| U−B color index | −0.61[2] |
| B−V color index | −0.11[2] |
| Astrometry | |
| Radial velocity (Rv) | −11.4[4] km/s |
| Proper motion (μ) | RA: −58.162[1] mas/yr Dec.: +11.802[1] mas/yr |
| Parallax (π) | 7.1387 ± 0.3291 mas[1] |
| Distance | 460 ± 20 ly (140 ± 6 pc) |
| Absolute magnitude (MV) | −1.95 + 2.4[5] |
| Orbit[5] | |
| Period (P) | 61.5496 ± 0.0058 d |
| Semi-major axis (a) | 0.487 ± 0.021 au |
| Eccentricity (e) | 0 |
| Inclination (i) | 130.0 ± 3.4° |
| Longitude of the node (Ω) | 118.0 ± 1.3° |
| Semi-amplitude (K1) (primary) | 6.90±0.15 km/s |
| Details | |
| κ Dra A | |
| Mass | 3.65 ± 0.48[5] M☉ |
| Radius | 5.85 ± 0.18[5] R☉ |
| Luminosity | 1178 ± 151[5] L☉ |
| Surface gravity (log g) | 3.5[6] cgs |
| Temperature | 13982 ± 392[5] K |
| Metallicity [Fe/H] | −0.65[7] dex |
| Rotational velocity (v sin i) | 200 ± 12[5] km/s |
| κ Dra B | |
| Mass | 0.426 ± 0.043[5] M☉ |
| Radius | 0.69 ± 0.07[5] R☉ |
| Luminosity | 33 ± 17[5] L☉ |
| Temperature | 16700 ± 2000[5] K |
| Rotational velocity (v sin i) | 35 ± 10[5] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
The star is currently located at declination +69° 47′ 18″ (right ascension 12h 33m 29.0s), but due to the effects of precession, Kappa Draconis was the nearest star to the north celestial pole visible to the naked eye from 1793 BC to approximately 1000 BC, though it was 6° removed from perfect alignment, making it only an approximate pole star, similar to the roughly 7° variance from perfect alignment of the much brighter (magnitude 2.08) star Kochab, at the same time during Earth's precession.[citation needed]
Properties Edit
Kappa Draconis is a classical Be star, displaying Balmer emission lines in its spectrum.[10] It is spinning rapidly with a projected rotational velocity of 170 km/s.[6] The star is thought to be just entering its red giant phase, having exhausted the supply of hydrogen in its core. Over the next several thousand years, the star will expand, becoming more powerful but with a much cooler surface temperature. Tens of thousands of years from now, Kappa Draconis will appear much brighter, probably shining with a reddish hue.[citation needed]
Kappa Draconis is a single-lined spectroscopic binary.[11] The main Be star is orbited by another stellar companion, on a circular orbit with a period of 61.555 days.[12] The General Catalogue of Variable Stars lists Kappa Draconis as a Gamma Cassiopeiae type star, a type of eruptive irregular variable star, whose visual magnitude varies from 3.82 to 4.01.[13] However Balona and Dziembowsk classify it as a Zeta Ophiuchi star, a type of pulsating variable star, with a primary period of 10.4 hours.[14]
Chinese name Edit
In Chinese, 紫微右垣 (Zǐ Wēi Yòu Yuán), meaning Right Wall of Purple Forbidden Enclosure, refers to an asterism consisting of κ Draconis, α Draconis, λ Draconis, 24 Ursae Majoris, 43 Camelopardalis, α Camelopardalis and BK Camelopardalis.[15] Consequently, the Chinese name for κ Draconis itself is 紫微右垣二 (Zǐ Wēi Yòu Yuán èr, English: the Second Star of Right Wall of Purple Forbidden Enclosure.),[16] representing 少尉 (Shǎowèi), meaning Second Chief Judge[17]
References Edit
- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c Crawford, D. L.; Barnes, J. V.; Golson, J. C. (1971), "Four-color, H-beta, and UBV photometry for bright B-type stars in the northern hemisphere", The Astronomical Journal, 76: 1058, Bibcode:1971AJ.....76.1058C, doi:10.1086/111220
- ^ Balona, L. A.; Dziembowski, W. A. (October 1999), "Excitation and visibility of high-degree modes in stars", Monthly Notices of the Royal Astronomical Society, 309 (1): 221–232, Bibcode:1999MNRAS.309..221B, doi:10.1046/j.1365-8711.1999.02821.x
- ^ Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Carnegie Institute of Washington D.C. Bibcode:1953GCRV..C......0W.
- ^ a b c d e f g h i j k l Klement, Robert; Baade, Dietrich; Rivinius, Thomas; Gies, Douglas R.; Wang, Luqian; Labadie-Bartz, Jonathan; Dos Santos, Pedro Ticiani; Monnier, John D.; Carciofi, Alex C.; Mérand, Antoine; Anugu, Narsireddy; Schaefer, Gail H.; Bouquin, Jean-Baptiste Le; Davies, Claire L.; Ennis, Jacob; Gardner, Tyler; Kraus, Stefan; Setterholm, Benjamin R.; Labdon, Aaron (2022). "Dynamical Masses of the Primary be Star and Secondary sdB Star in the Single-lined Binary κ Dra (B6 IIIe)". The Astrophysical Journal. 940 (1): 86. arXiv:2210.03090. Bibcode:2022ApJ...940...86K. doi:10.3847/1538-4357/ac98b8. S2CID 252735283.
- ^ a b Saad, S. M.; Kubát, J.; Koubský, P.; Harmanec, P.; Škoda, P.; Korčáková, D.; Krtička, J.; Šlechta, M.; Božić, H.; Ak, H.; Hadrava, P.; Votruba, V. (2004). "Properties and nature of Be stars. XXIII. Long-term variations and physical properties of κ Dra". Astronomy & Astrophysics. 419 (2): 607–621. arXiv:astro-ph/0401491. Bibcode:2004A&A...419..607S. doi:10.1051/0004-6361:20034241. S2CID 119007669.
- ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
- ^ "kap Dra". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-02-06.
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ Banerjee, Gourav; et al. (January 2021), "Optical spectroscopy of Galactic field classical Be stars", Monthly Notices of the Royal Astronomical Society, 500 (3): 3926–3943, arXiv:2011.08622, Bibcode:2021MNRAS.500.3926B, doi:10.1093/mnras/staa3469.
- ^ Hutter, D. J.; Tycner, C.; Zavala, R. T.; Benson, J. A.; Hummel, C. A.; Zirm, H. (2021). "Surveying the Bright Stars by Optical Interferometry. III. A Magnitude-limited Multiplicity Survey of Classical Be Stars". The Astrophysical Journal Supplement Series. 257 (2): 69. arXiv:2109.06839. Bibcode:2021ApJS..257...69H. doi:10.3847/1538-4365/ac23cb. S2CID 237503492.
- ^ Saad, S. M.; Kubát, J.; Hadrava, P.; Harmanec, P.; Koubský, P.; Škoda, P.; Šlechta, M.; Korčáková, D.; Yang, S. (2005). "Spectrum Disentangling and Orbital Solution for κ Dra". Astrophysics and Space Science. 296 (1–4): 173–177. Bibcode:2005Ap&SS.296..173S. doi:10.1007/s10509-005-4438-7. S2CID 189844885.
- ^ "Query= kap Dra". General Catalog of Variable Stars. Sternberg Astronomical Institute. Retrieved 19 December 2022.
- ^ Balona, L. A.; Dziembowski, W. A. (October 1999). "Excitation and visibility of high-degree modes in stars". Monthly Notices of the Royal Astronomical Society. 309 (1): 221–232. Bibcode:1999MNRAS.309..221B. doi:10.1046/j.1365-8711.1999.02821.x.
- ^ (in Chinese) 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, ISBN 978-986-7332-25-7.
- ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 11 日
- ^ English-Chinese Glossary of Chinese Star Regions, Asterisms and Star Name 2008-09-24 at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
External links Edit
- by Jim Kaler