Sentences with phrase «sequence dwarf star»

Sol is a yellow - orange, main sequence dwarf star (G2 V — see spectrum).

HD 111232 is a yellow - orange main sequence dwarf star of spectral and luminosity type G5 V, but it has been classed as orange as a G8.

HD 40307 is an orange - red main - sequence dwarf star of spectral and luminosity type K2.5 V (Mayor et al, 2008).

Alpha Mensae is a yellow - orange main sequence dwarf star of spectral and luminosity type G5 - 6 V, with about 87 percent of Sol's mass, 84 to 91 percent of its diameter (Perrin and Karoji, 1987, page 236; and Johnson and Wright, 1983, page 659), and around 80 percent of its luminosity.

Star «B» is a red red sequence dwarf star of spectral and luminosity type M2 V.

This star is a yellow - orange main sequence dwarf star of spectral and luminosity type G8 Ve.

This star is a yellow - orange main sequence dwarf star of possibly spectral and luminosity type G V (Nikolic et al, 1997; and Hill et al, 1989), or later spectral type.

Star A is a main sequence dwarf star of spectral and luminosity type F5 V (NASA Stars and Exoplanet Database).

Epsilon Indi is a orange - red main sequence dwarf star of spectral and luminosity type K4 - 5 Ve.

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).

In March 2005, astronomers seeking ancient stars announced the discovery of HE 1327 - 2326, a subgiant or main - sequence dwarf star with extremely low metallicity — an iron abundance -LRB-[Fe / H] = -5.4 + / - 0.2) that is only about 1/250, 000 th of Sol's and a factor of two lower than that of giant star HE 0107 - 5240 (which is discussed in detail below).

Star b is a main sequence dwarf star of spectral and luminosity type G8 V (Fekel and Tomkin, 1983).

Unlike Sol, it is a slightly bluish, white main sequence dwarf star of spectral and luminosity type A0 - 1 Vm.

Tau Boötis A is a yellowish main sequence dwarf star of spectral and luminosity type F7 V, although it has also been classified as a F6 IV subgiant.

This star is a yellow - orange main sequence dwarf star of spectral and luminosity type G0 V, with roughly the same mass as Sol (Irwin et al, 1992), as much as 1.45 times its diameter (George G. Gatewood, 1994, page 143), and less than 1.1 times its luminosity.

Star «B» is a red main sequence dwarf star of spectral and luminosity type M2 V, with about one fifth of Sol's mass, 58 percent of its diameter, and 84/10, 000 th of its luminosity.

37 Geminorum (Gem) is a yellow - orange main sequence dwarf star of spectral and luminosity type G0 V.

70 Virginis is a yellow - orange main sequence dwarf star of spectral and luminosity type G5 Va, but has been previously classified from G2.5 to G4.

This star is a yellowish main sequence dwarf star of spectral and luminosity type F5 - G1 Vn (Nikolic et al, 1997; based on Frans van't Veer, 1971; and Kurpinska and van't Veer, 1970; versus Hill et al, 1989, page 89).

Lambda Serpentis is a main sequence dwarf star of spectral and luminosity type G0 V, but it is listed as a possible subgiant in some catalogues.

This star is a very dim, red main sequence dwarf star of spectral and luminosity type M4 V (SIMBAD Astronomical Database).

This star is probably a yellow - orange main sequence dwarf star of spectral and luminosity type G2 V (Tinney et al, 2011), but it has been classed as orange as a G5.

Gamma Pavonis is a yellowish - white main sequence dwarf star of spectral and luminosity type F6 - 8 V.

Zeta Doradus is a main sequence dwarf star of spectral and luminosity type F7 V but has been classed as white as F6 and as yellow as F9 (Lagrange et al, 2009, page 14 for HD 33262; Trilling et al, 2008, page 26; NASA Stars and Exoplanet Database; and SIMBAD).

According to Emeritus Professor Jim Kaler, Beta Hydri entered the main sequence a dwarf star at the cooler end of class F (probably around spectral class F8) but now appears to be a subgiant star that is evolving off the main sequence, as it begins to fuse increasing amounts of helium «ash» mixed with hydrogen at its core.

Beta Hydri is a yellow - orange main sequence dwarf star of spectral and luminosity type G2 IV.

Star A is a main sequence dwarf star of spectral and luminosity type F7 - 8 V (Wittenmyer et al, 2006, page 178; Bonavita and Desidera, 2007, HD 16895 in Table 8; and NASA Stars and Exoplanet Database) but has been classed as yellow as F9 (Baize and Petit, 1989, page 505.

The star may even be suspected of being a dim subdwarf (sd / VI)-- like Groombridge 1830 or Kapteyn's Star — rather than a main - sequence dwarf star (V).

HR 483 B is an «intermediate mass,» red main sequence dwarf star of spectral and luminosity type M V (Henry et al, 1992).

HR 483 A is a yellow - orange main sequence dwarf star of spectral and luminosity type G1.5 V.

Star A is a yellowish main sequence dwarf star of spectral and luminosity type F8 V, with 1.31 times the mass of Sol (McArthur et al, 2010), 1.6 times its diameter, and 3.4 times its luminosity.

Star A is an orange - red, main sequence dwarf star of spectral and luminosity type K1 - 2 V - VI, Bouchy et al, 2005) but was previously catalogued as yellow as G5.

107 Piscium is a orange - red main sequence dwarf star of spectral and luminosity type K1 V.

54 Piscium is an orange - red main - sequence dwarf star of spectral and luminosity type K0 + V.

Star b is a main sequence dwarf star of spectral and luminosity type M1 - 2 Ve Duquennoy and Mayor, 1991, page 489 for Gl 107 B).

This is a red main sequence dwarf star of spectral and luminosity type M3.5 V.

Iota Persei is a yellow - orange main sequence dwarf star of spectral and luminosity type G0 V. Bigger and brighter than Sol, the star may have as much as 1.3 times Sol's mass, around 1.08 times its diameter (Pasinetti - Fracassini et al, 2001; Blackwell and Lynas - Gray, 1994; and Johnson and Wright, 1983, page 653), and 2.2 times its luminosity.

Delta Trianguli A is a yellow - orange main sequence dwarf star of spectral and luminosity type G0.5 Ve.

Vega is a slightly bluish, white main sequence dwarf star of spectral and luminosity type A0 V, like Sirius.

Moreover, the star's discovery suggest that even relatively low - mass Population III stars could have formed and survived until today, still shining faintly below easy detectability as main sequence dwarf stars in distant reaches of the galactic halo.

Subdwarfs, such as nearby Kapteyn's Star (M0VI or M0sd) as well as Groombridge 1830, are dimmer more bluish than younger main - sequence dwarf stars (Wing et al, 1976).

Not exact matches

On April 23, NASA's Swift satellite detected the strongest, hottest, and longest - lasting sequence of stellar flares ever seen from a nearby red dwarf star.

Superflares have also been observed in a group of dim main - sequence, reddish M dwarfs known as flare stars.

This star is a main sequence, orange - red or red dwarf (K7 - M0 Vp), with peculiar metal - weak spectrum for CA I, CA II, and CR triplet (Christopher J. Corbally, S.J., 1984).

Recently, Hallinan et al. (2015) reported simultaneous radio and optical spectroscopic observations (obtained with the Karl G. Jansky Very Large Array (VLA) radio telescope and the Double Spectrograph (DBSP) on the 5.1 - m Hale telescope, respectively) of auroral emissions of an object at the end of the stellar main sequence (i.e. at the boundary between stars and brown dwarfs).

A main sequence star that is dimmer and redder than the Sun (spectral type K and M — red dwarfs) could have plants that absorb more red and infrared wavelengths.

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).

It appears to be a main sequence red dwarf star of spectral and luminosity type M4.5 V. Because of its small mass and great distance from the primary (Star A), Upsilon Andromedae B appears to have a negligible effect on the radial velocity measurements used to determine that Star A has at least three large planets (Lowrance et al, 20star of spectral and luminosity type M4.5 V. Because of its small mass and great distance from the primary (Star A), Upsilon Andromedae B appears to have a negligible effect on the radial velocity measurements used to determine that Star A has at least three large planets (Lowrance et al, 20Star A), Upsilon Andromedae B appears to have a negligible effect on the radial velocity measurements used to determine that Star A has at least three large planets (Lowrance et al, 20Star A has at least three large planets (Lowrance et al, 2002).

This much dimmer companion star is a main sequence, orange - red dwarf (K0 - 1 V).

Star A is a main sequence, orange - red dwarf of spectral and luminosity type K3 V.