Sentences with phrase «bolometric luminosity»

Most revealing, HD 156668 only has around 27 percent of Sol's bolometric luminosity (NASA Star and Exoplanet Database, derived from Kenneth R. Lang, 1980).

The star has almost a half (49 + / - 0.014 percent) of Sol's mass (Endl et al, 2008), 52 to 53 percent of its diameter (NASA Star and Exoplanet Database, derived from Kenneth R. Lang, 1980; Pasinetti - Fracassini et al, 2001; and Johnson and Wright, 1983, page 655), and less than 0.8 percent of its visual and 3.5 ± 0.3 of its bolometric luminosity (NASA Star and Exoplanet Database, derived from Kenneth R. Lang, 1980).

It has around 1.2 to 1.4 times Sol's mass, around 1.7 times Sol's diameter, and 3.51 (+ / - 0.10) times its bolometric luminosity (North et al, 2009; and Eggenberger and Carrier, 2006).

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).

This range in Teff is compatible with all observational constraints, including near - infrared photometry and bolometric luminosity.

The star has 15.7 ± 1.9 percent of Sol's mass, 21.1 (± 0.97 percent of its diameter, and under 0.02 percent of its visual and over 0.328 percent of its bolometric luminosity (Rogers and Seager, 2009).

Based on an interpolation table, the star's has around 2.10 of Sol's mass (NASA Stars and Exoplanet Database; and David F. Gray, 1992), 1.58 times its diameter (Akeson et al, 2009), and around 11.5 times its visual luminosity and 13.4 times its theoretical bolometric luminosity (Akeson et al, 2009; NASA Stars and Exoplanet database; and Kenneth R. Lang, 1980).

Lacaille 9352 may have 50 to 58 of Sol's mass (Demory et al, 2009, Table 4; RECONS; and NASA Star and Exoplanet Database, interpolation table of Henry and McCarthy, 1993), less than half (43 to 46 percent) of its diameter (Demory et al, 2009, Table 4; and NASA Star and Exoplanet Database, derived from the power law formula of Kenneth R. Lang, 1980), 1.1 percent of its visual luminosity and 3.5 percent of its bolometric luminosity (NASA Star and Exoplanet Database, derived from the exponential formula of Kenneth R. Lang, 1980), and only about one tenth to 60 percent of Sol's abundance of elements heavier than hydrogen («metallicity»)(Demory et al, 2009, Table 4).

The star may have around 1.01 to 1.28 times Sol's mass (Yoichi Takeda, 2007; Valenti and Fischer, 2005; Klaus Fuhrmann, 1998, page 166; and NASA Stars and Exoplanet Database; and David F. Gray, 1992), around 1.33 to 1.39 times Sol's diameter (Klaus Fuhrmann, 1998, page 166; NASA Stars and Exoplanet database; and Kenneth R. Lang, 1980); and around 1.9 to 2.2 times its bolometric luminosity (Klaus Fuhrmann, 1998, page 166 for absolute bolometric magnitude; NASA Stars and Exoplanet database; and Kenneth R. Lang, 1980).

This star is a white - yellow main sequence dwarf star of spectral and luminosity type F6 V, with almost 1.3 times Sol's mass (NASA Star and Exoplanet Database; and David F. Gray, 1992), 1.2 5o 1.3 times its diameter (von Belle and von Braun, 2009, HD 30652 in Table 4, page 7; Perrin and Karoji, 1987; NASA Star and Exoplanet Database; and Kenneth R. Lang, 1980), and over 2.6 times of its bolometric luminosity (NASA Star 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).

The star has about 70 to 77 percent of Sol's mass (RECONS; and NASA Star and Exoplanet Database, interpolated from David F. Gray, 1992), 68 to 76 percent of its diameter (Johnson and Wright, 1983, page 701; and NASA Star and Exoplanet Database, derived using the power law formula from Kenneth R. Lang, 1980), and about 14.7 percent of its visual luminosity and 20.4 percent of its theoretical bolometric luminosity, correcting for infrared output (NASA Star and Exoplanet Database, derived using exponential formula from 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 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 has almost a half (48 to 49 percent) of Sol's mass (Zechmeister et al, 2009, from Delfosse et al, 2000; and NASA Star and Exoplanet Database, derived from Henry and McCarthy, 1993), 48 to 57 percent of its diameter (NASA Star and Exoplanet Database, derived from Kenneth R. Lang, 1980; and Johnson and Wright, 1983, page 673), and percent of its visual and around 3.3 + / - 0.2 of its bolometric luminosity and McCarthy, 1993), 48 to 57 percent of its diameter (NASA Star and Exoplanet Database, derived from Kenneth R. Lang, 1980).

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.

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).

It may have around 85 percent of Sol's mass (Howard et al, 2010, for HD 97658 on Table 1, page 3), 73 percent of its diameter (Howard et al, 2010, for HD 97658 on Table 1, page 3), and 34 percent of its bolometric luminosity (Howard et al, 2010, for HD 97658 on Table 1, page 3; and the NASA Star and Exoplanet Database, derived from the exponential formula of Kenneth R. Lang, 1980).

This cool and dim, main sequence red dwarf (M1.5 Vne) may have about 37.5 to 48.6 percent of Sol's mass (Howard et al, 2014; RECONS; and Berger et al, 2006, Table 5, based on Delfosse et al, 2000), 34 to 39 percent of its diameter (Howard et al, 2014), and some 2.2 percent of its luminosity and 2.9 percent of its theoretical bolometric luminosity (Howard et al, 2014), correcting for infrared output (NASA Star and Exoplanet Database, derived using exponential formula from 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).

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).

Not exact matches

On January 13, 2003, a team of astronomers (including Ralf - Dieter Scholz, Mark McCaughrean, Nicolas Lodieu, and Bjoern Kuhlbrodt) announced the discovery of a brown dwarf companion «b» — now re-designated «ba» — to this nearby star with a total (bolometric) luminosity of just 0.002 percent that of the Sun (ESO and AIP joint press release and API press release in German — more below).

If this is the case, it would explain both the low value of the total bolometric flare energy (as the absolute luminosity of the superflare stars and thus the total bolometric flare energy would be larger) and the S index (as the light entering the fibre would likely be contaminated and the observed emission in the H and K lines would therefore be relatively small).