S Sagittae is a Classical Cepheid variable that varies from magnitude 5.24 to 6.04 in 8.38 days . It is a yellow-white supergiant that varies between spectral types F6Ib and G5Ib.
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HD 231701 is a yellow-white main sequence star hotter and larger than our Sun, which was found to have a planet in 2007.15 Sagittae is a solar analog that has a brown dwarf substellar companion.
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Observations were requested by the American Association of Variable Star Observers ( AAVSO ) during the 2011 outburst phase to help classify the object, and to see if it is an infrequently outbursting normal dwarf nova like WZ Sagittae or a recurrent nova.
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Sagittal otoliths ( sagittae ) are bilaterally symmetrical, with each fish having one right and one left . Separating recovered otoliths into right and left, therefore, allows one to infer a minimum number of prey individuals ingested for a given fish species.
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"' 15 Sagittae B "'is a high-mass substellar L dwarf of spectral class L4 ?1.5, only a few Jupiter masses below the limit for stars, in a long-period orbit around the primary star.
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Ptolemy saw the constellation's brightest star Gamma Sagittae as marking the arrow's head, while Bayer saw Gamma, Eta and Theta as depicting the arrow's shaft . Gamma Sagittae is a red giant of spectral type M0III, and magnitude 3.47.
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Ptolemy saw the constellation's brightest star Gamma Sagittae as marking the arrow's head, while Bayer saw Gamma, Eta and Theta as depicting the arrow's shaft . Gamma Sagittae is a red giant of spectral type M0III, and magnitude 3.47.
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The WZ Sagittae-type dwarf nova DY CMi ( also known as VSX J074727.6 + 065050 ) flared up to magnitude 11.4 over January and February 2008 before dropping eight magnitudes to around 19.5 over approximately 80 days . It is a remote binary star system where a white dwarf and low mass star orbit each other close enough for the former star to draw material off the latter and form an accretion disc.
