Sentences with phrase «estimated bolometric»

Based on its estimated bolometric luminosity, the distance from HR 4523 A where an Earth - type planet would be «comfortable» with liquid water is centered around 0.88 AU — between the orbital distance of Venus and Earth in the Solar System, with an orbital period about 330 days, or about 90 percent of an Earth year.

Not exact matches

According to various estimates, the star has about 1.7 times Sol's mass (RECONS), 1.8 times its equatorial diameter (JPL press release, 2001; T. Moon, 1985; Morossi and Malagnini, 1985, page 369; and Johnson and Wright, 1983, page 695), and about 10.7 times its visual luminosity and 9.845 its bolometric luminosity (NASA Star and Exoplanet Database, derived from of Kenneth R. Lang, 1980).

The star may have around 1 to 1.4 times Sol's mass (Wittenmyer et al, 2006, page 178; Valenti and Fischer, 2005; Allende Prieto et al, 1999, page 30, Table 1 for HR 799; Bonavita and Desidera, 2007, HD 16895 in Table 8; and NASA Stars and Exoplanet Database; and David F. Gray, 1992), around 1.24 times Sol's diameter based on a power - law estimate (NASA Stars and Exoplanet database; and Kenneth R. Lang, 1980); and around 2.2 times its theoretical bolometric luminosity (NASA Stars and Exoplanet database; and Kenneth R. Lang, 1980).

61 Virginis is a yellow - orange main sequence dwarf of spectral and luminosity type G5 - 6 V, with about 92 to 96 percent of Sol's mass (95 percent using the isochrone mass estimate of Valenti and Fischer, 2005; and NASA Star and Exoplanet Database, based on David F. Gray, 1992), 94 to 98 percent of its diameter (96 percent for Valenti and Fischer, 2005; Johnson and Wright, 1983, page 677; and NASA Star and Exoplanet Database, derived from the exponential formula of Kenneth R. Lang, 1980), and around 78 percent of its visual luminosity and nearly 81 percent of its theoretical bolometric luminosity, with infrared radiation (Sousa et al, 2008; Valenti and Fischer, 2005; NASA Star and Exoplanet Database, based on Kenneth R. Lang, 1980).

The star has recently been estimated to have as high as 85 percent Sol's mass (Tinney et al, 2011; and Kovacs and Foy, 1978), and it may have around 92 to 96 percent of its diameter (NASA Star and Exoplanet Database, derived using the power law formula of Kenneth R. Lang, 1980) and about 78 percent of its bolometric luminosity (NASA Star and Exoplanet Database, derived using the exponential formula of Kenneth R. Lang, 1980).

The star may have around 1.25 to 1.33 times Sol's mass (Jancart et al, 2005, page 14 under HIP 109176; Nordström et al, 2004; Boden et al, 1999; NASA Stars and Exoplanet Database; and David F. Gray, 1992; and Fekel and Tomkin, 1983), around 1.4 to 1.5 times Sol's diameter based on a power - law estimate (van Belle and von Braun, 2009, page 7, Table 4; NASA Stars and Exoplanet database; and Kenneth R. Lang, 1980); and around 3.3 times its theoretical bolometric luminosity (NASA Stars and Exoplanet database; and Kenneth R. Lang, 1980).

The star has a mass that is six to eight times greater than Sol's (see Petr Harmanec, 1988; and James Kaler), 14.4 (+ / - 0.4, polar) to 24.0 (+ / - 0.8, equatorial) times its diameter (ESO; and Domicano de Souza et al, 2003), and 1,070 times its visual luminosity and at least 2,900 to 5,400 times its bolometric luminosity (depending on the estimate of ultraviolet radiation).

Sensitive to estimate's of the star's abundance of «metals» (elements heavier than hydrogen), Star A appears to have 1.6 to 1.7 times Sol's mass (van Belle et al, 2007; Guenther et al, 2005; D.B. Guenther, 2004; and Carrier et al, 2004), about 2.7 times Sol's diameter (van Belle et al, 2007; Fracassini et al, 1994; and Johnson and Wright, 1983, page 679), and around 8.9 times Sol's bolometric luminosity (van Belle et al, 2007; and Thévenin et al, 2005).