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.
The star is currently located at declination 69° 47' 18" North (RA 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
Kappa Draconis is a classical Be star, displaying Balmer emission lines in its spectrum.[9] It is spinning rapidly with a projected rotational velocity of 170km/s.[7] 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.[10] The main Be star is orbited by another stellar companion, on a circular orbit with a period of 61.555 days.[6]
Chinese name
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.[11] 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.),[12] representing 少尉 (Shǎowèi), meaning Second Chief Judge[13]
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
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. S2CID189844885.
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. doi:10.1051/0004-6361:20034241. S2CID119007669.
"kap Dra". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2012-02-06.
Banerjee, Gourav; etal. (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. S2CID237503492.
(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, ISBN978-986-7332-25-7.
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