Big Bear, Little Bear

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There are plenty of different species of bears in the wildlife that come in various shapes, sizes and colours. Bears can be found in almost every corner of the world.

Big Bear Little Bear - Etsy UK Big Bear Little Bear - Etsy UK

Robert Brown, Researches into the origin of the primitive constellations of the Greeks, Phoenicians and Babylonians (1899), Olcott, William Tyler (2012) [1911]. Star Lore of All Ages: A Collection of Myths, Legends, and Facts Concerning the Constellations of the Northern Hemisphere. New York, New York: Courier Corporation. p.377. ISBN 978-0-486-14080-3.Watson, Christopher (4 January 2010). "RU Ursae Minoris". The International Variable Star Index. American Association of Variable Star Observers . Retrieved 18 July 2015. Otero, Sebastian Alberto (16 November 2009). "RR Ursae Minoris". The International Variable Star Index. American Association of Variable Star Observers . Retrieved 18 May 2014. According to Diogenes Laërtius, citing Callimachus, Thales of Miletus "measured the stars of the Wagon by which the Phoenicians sail". Diogenes identifies these as the constellation of Ursa Minor, which for its reported use by the Phoenicians for navigation at sea were also named Phoinikē. [6] [7] The original "bear" is thus Ursa Major, and Ursa Minor was admitted as the second, or "Phoenician Bear" (Ursa Phoenicia, hence Φοινίκη, Phoenice) a b Department of Astronomy (1995). "Ursa Minor". University of Wisconsin–Madison . Retrieved 27 June 2015.

Big Bear, Little Bear by David Bedford | Goodreads Big Bear, Little Bear by David Bedford | Goodreads

Alpha Ursae Minoris – Classical Cepheid (Delta Cep Type)". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg . Retrieved 19 August 2014. O'Meara, Stephen James (2007). Steve O'Meara's Herschel 400 Observing Guide. Cambridge, UK: Cambridge University Press. p.227. ISBN 978-0-521-85893-9. NGC 6251 is an active supergiant elliptical radio galaxy more than 340 million light-years away from Earth. It has a Seyfert 2 active galactic nucleus, and is one of the most extreme examples of a Seyfert galaxy. This galaxy may be associated with gamma-ray source 3EG J1621+8203, which has high-energy gamma-ray emission. [76] It is also noted for its one-sided radio jet—one of the brightest known—discovered in 1977. [77] Meteor showers [ edit ] Overcome with grief, he began to cry. Zeus heard him weeping and realised what had happened. He didn’t want Hera to hear Arcas and find out what had happened. So he turned both mother and son into constellations. Eta Ursae Minoris". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg . Retrieved 30 July 2014.NGC 6251 – Seyfert 2 Galaxy". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg . Retrieved 21 July 2015. Bianchini, A.; Tappert, C.; Canterna, R.; Tamburini, F.; Osborne, H.; Cantrell, K. (2003). "RW Ursae Minoris (1956): An Evolving Postnova System". Publications of the Astronomical Society of the Pacific. 115 (#809): 811–18. Bibcode: 2003PASP..115..811B. doi: 10.1086/376434. a b "Epsilon Ursae Minoris – Variable of RS CVn type". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg . Retrieved 21 June 2014. Albright, William F. (1972). "Neglected Factors in the Greek Intellectual Revolution". Proceedings of the American Philosophical Society. 116 (3): 225–42. JSTOR 986117. Located close to Polaris is Lambda Ursae Minoris, a red giant of spectral type M1III. It is a semiregular variable varying between magnitudes 6.35 and 6.45. [46] The northerly nature of the constellation means that the variable stars can be observed all year: The red giant R Ursae Minoris is a semiregular variable varying from magnitude 8.5 to 11.5 over 328days, while S Ursae Minoris is a long-period variable that ranges between magnitudes 8.0 and 11 over 331days. [47] Located south of Kochab and Pherkad towards Draco is RR Ursae Minoris, [3] a red giant of spectral type M5III that is also a semiregular variable ranging from magnitude 4.44 to 4.85 over a period of 43.3days. [48] T Ursae Minoris is another red-giant variable star that has undergone a dramatic change in status—from being a long-period (Mira) variable ranging from magnitude 7.8 to 15 over 310–315 days, to being a semiregular variable. [49] The star is thought to have undergone a shell helium flash—a point where the shell of helium around the star's core reaches a critical mass and ignites—marked by its abrupt change in variability in 1979. [50] Z Ursae Minoris is a faint variable star that suddenly dropped 6magnitudes in 1992 and was identified as one of a rare class of stars— R Coronae Borealis variables. [51]