Big Bear, Little Bear

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If bear is your spirit animal then why not get little bear tattoos to go with your nature. There can be tonnes of bear tattoo designs and ideas that we could not include in this list. Here are some more bear tattoo ideas which might allure you! Bergh, Sidney (2000). The Galaxies of the Local Group. Cambridge, UK: Cambridge University Press. p.257. ISBN 978-1-139-42965-8. Polaris, the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging in apparent magnitude from 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Kochab and 3rd-magnitude Gamma Ursae Minoris have been called the "guardians of the pole star" or "Guardians of The Pole". [3] Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star— Calvera—and H1504+65, the hottest white dwarf yet discovered, with a surface temperature of 200,000 K. Traditionally known as Pherkad, Gamma Ursae Minoris has an apparent magnitude that varies between 3.04 and 3.09 roughly every 3.4hours. [32] It and Kochab have been termed the "guardians of the pole star". [3] A white bright giant of spectral type A3II-III, [32] with around 4.8times the Sun's mass, 1,050times its luminosity and 15times its radius, [33] it is 487±8 light-years distant from Earth. [28] Pherkad belongs to a class of stars known as Delta Scuti variables [32]—short period (six hours at most) pulsating stars that have been used as standard candles and as subjects to study asteroseismology. [34] Also possibly a member of this class is Zeta Ursae Minoris, [35] a white star of spectral type A3V, [36] which has begun cooling, expanding and brightening. It is likely to have been a B3 main-sequence star and is now slightly variable. [35] At magnitude 4.95 the dimmest of the seven stars of the Little Dipper is Eta Ursae Minoris. [37] A yellow-white main-sequence star of spectral type F5V, it is 97 light-years distant. [38] It is double the Sun's diameter, 1.4times as massive, and shines with 7.4times its luminosity. [37] Nearby Zeta lies 5.00-magnitude Theta Ursae Minoris. Located 860 ± 80light-years distant, [39] it is an orange giant of spectral type K5III that has expanded and cooled off the main sequence, and has an estimated diameter around 4.8times that of the Sun. [40]

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The Ursids, a prominent meteor shower that occurs in Ursa Minor, peaks between December 18 and 25. Its parent body is the comet 8P/Tuttle. [78] See also [ edit ] Sato, Bun'ei; Omiya, Masashi; Harakawa, Hiroki; Liu, Yu-Juan; Izumiura, Hideyuki; Kambe, Eiji; Takeda, Yoichi; Yoshida, Michitoshi; Itoh, Yoichi; Ando, Hiroyasu; Kokubo, Eiichiro; Ida, Shigeru (2013). "Planetary Companions to Three Evolved Intermediate-Mass Stars: HD 2952, HD 120084, and omega Serpentis". Publications of the Astronomical Society of Japan. 65 (4): 1–15. arXiv: 1304.4328. Bibcode: 2013PASJ...65...85S. doi: 10.1093/pasj/65.4.85. S2CID 119248666. There are various proposed explanations for the name Cynosura. One suggestion connects it to the myth of Callisto, with her son Arcas replaced by her dog being placed in the sky by Zeus. [11]Calzetti, Daniela (1997). "Reddening and Star Formation in Starburst Galaxies". Astronomical Journal. 113: 162–84. arXiv: astro-ph/9610184. Bibcode: 1997AJ....113..162C. doi: 10.1086/118242. S2CID 16526015. a b Department of Astronomy (1995). "Ursa Minor". University of Wisconsin–Madison . Retrieved 27 June 2015. Watson, Christopher (4 January 2010). "Lambda Ursae Minoris". The International Variable Star Index. American Association of Variable Star Observers . Retrieved 21 June 2014. RW Ursae Minoris is a cataclysmic variable star system that flared up as a nova in 1956, reaching magnitude 6. In 2003, it was still two magnitudes brighter than its baseline, and dimming at a rate of 0.02 magnitude a year. Its distance has been calculated as 5,000±800parsecs (16,300light-years), which puts its location in the galactic halo. [56]

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NGC 6217 is a barred spiral galaxy located some 67 million light-years away, [73] which can be located with a 10cm (4in) or larger telescope as an 11th-magnitude object about 2.5° east-northeast of Zeta Ursae Minoris. [74] It has been characterized as a starburst galaxy, which means it is undergoing a high rate of star formation compared with a typical galaxy. [75] a b c d e f "Ursa Minor, Constellation Boundary". The Constellations. International Astronomical Union . Retrieved 12 May 2014. Ursa Minor, with Draco looping around it, as depicted in Urania's Mirror, [4] a set of constellation maps published in London c. 1825 Rutledge, Robert; Fox, Derek; Shevchuk, Andrew (2008). "Discovery of an Isolated Compact Object at High Galactic Latitude". The Astrophysical Journal. 672 (#2): 1137–43. arXiv: 0705.1011. Bibcode: 2008ApJ...672.1137R. doi: 10.1086/522667. S2CID 7915388. a b Kaler, James B. "Epsilon Ursae Minoris". Stars. University of Illinois . Retrieved 21 June 2014.Rogers, John H. (1998). "Origins of the Ancient Constellations: I. The Mesopotamian Traditions". Journal of the British Astronomical Association. 108: 9–28. Bibcode: 1998JBAA..108....9R.

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Watson, Christopher (4 January 2010). "W Ursae Minoris". The International Variable Star Index. American Association of Variable Star Observers . Retrieved 18 July 2015. Kaler, James B. (20 December 2013). "Pherkad". Stars. University of Illinois . Retrieved 18 May 2014.

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Russell, Henry Norris (1922). "The New International Symbols for the Constellations". Popular Astronomy. 30: 469. Bibcode: 1922PA.....30..469R. MacDonald, John (1998). The Arctic Sky: Inuit Astronomy, Star Lore, and Legend. Toronto, Ontario: Royal Ontario Museum/Nunavut Research Institute. p. 61. ISBN 978-0-88854-427-8. Albright, William F. (1972). "Neglected Factors in the Greek Intellectual Revolution". Proceedings of the American Philosophical Society. 116 (3): 225–42. JSTOR 986117. NGC 6251 – Seyfert 2 Galaxy". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg . Retrieved 21 July 2015. Eclipsing variables are star systems that vary in brightness because of one star passing in front of the other rather than from any intrinsic change in luminosity. W Ursae Minoris is one such system, its magnitude ranging from 8.51 to 9.59 over 1.7 days. [52] The combined spectrum of the system is A2V, but the masses of the two component stars are unknown. A slight change in the orbital period in 1973 suggests there is a third component of the multiple star system—most likely a red dwarf—with an orbital period of 62.2±3.9 years. [53] RU Ursae Minoris is another example, ranging from 10 to 10.66 over 0.52days. [54] It is a semidetached system, as the secondary star is filling its Roche lobe and transferring matter to the primary. [55]