The title supergiant, as applied to a star, does not have a single concrete definition. The term giant star was first coined by Hertzsprung when it became apparent that the majority of stars fell into two distinct regions of the Hertzsprung–Russell diagram. One region contained larger and more...
Nearly all blue supergiant stars shimmer in brightness and now we know why: waves along their surface due to internal convection currents. Waves Along the Surface Begin Deep Within Star Source:Dr Tamara Rogers / Newcastle University Stars have been objects of endless fascination for humans since ou...
VY Canis Majoris, the largest star in the night sky, is huge compared to the sun. Why do red supergiants appear red? The color of stars depends primarily on the temperature of the surface of the star. Color is a property of light that depends on the wavelength of that light. Hotter ...
For RSGs, the heavy lifting has already been done by the stellar interior, as a significant fraction of the luminosity of the star has gone into making a bigger radius. “It is kind of like walking with a nearly full glass of water vs a glass that is only 1% full (O star)–even a...
DesignationDynamicsEffective temperatureLuminosity KinematicsMagnetic fieldAbsolute magnitudeMassMetallicityRotationStarlightVariablePhotometric system Color indexHertzsprung–Russell diagramColor–color diagram Star systems Binary ContactCommon envelope Eclipsing Symbiotic Multiple Cluster ...
Some features of the color-magnitude diagram and the shape of the integrated luminosity function suggest star formation lasting up to 10 Myr. These ages are much larger than those which follow from models for the expansion of LMC4 and their prediction of subsequent star formation....
This is also the first time astronomers were able to measure the size of a dying star in the early universe. This was based on the supernova’s brightness and rate of cooling, both of which depend on the size of the progenitor star. Hubble observations show that the red ...
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By UBV -photometry and spectroscopy the color excess has been estimated: E B-V = 0.50–0.54. Joint photometric and spectral data analysis allows us to assume that the star variability is caused by stellar wind variations.doi:10.1134/S1063773712020016V. P. Arkhipova...
A much longer period (P = 1601 d), that allows us to classify this star as a long secondary period variable star (LSPV) has been also detected. The B - Land U - B color variations related to the long secondary period (LSP) are similar to those related to the shorter periods, ...