Sentences with phrase «subgiant of»
Star A is probably a yellow - orange subgiant of spectral and luminosity type G0 IV).
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Star A is probably a yellow - orange subgiant of spectral and luminosity type G0 IV (NASA Stars and Exoplanet Database; and Garrison and Beattie, 1998).
Not exact matches
It appears to be a subgiant star that is evolving off the main sequence, as it begins to fuse the increasing amounts of helium «ash» mixed with hydrogen at its core.
Schlaufman, K. C. & Winn, J. N. Evidence for the tidal destruction of hot Jupiters by subgiant stars.
Altair has the New Suspected Variable designation NSV 24910 and is unusually bright for its spectral type and so may be becoming a subgiant star that is beginning to evolve off the main sequence, as it begins to fuse the increasing amounts of helium «ash» mixed with hydrogen at its core.
Evolutionary analysis of the host star suggests that KELT - 10b is unlikely to survive beyond the current subgiant phase, due to a concomitant in - spiral of the planet over the next $ \ sim $ 1 Gyr.
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.
As a subgiant star subject to pulsations which affect careful measurements of variations in radial velocity caused by the gravitational pull of substellar companions, astronomers would find it very difficult to detect any Earth - type planet around Beta Hydri using present methods.
© Torben Krogh & Mogens Winther, (Amtsgymnasiet and EUC Syd Gallery, student photo used with permission) HD 181433 is an orange - red star (similar to Epsilon Eridani at left center of meteor) that may have already evolved into a subgiant, but is probably not yet a giant, star.
HD 181433 may be a subgiant rather than a main - sequence, orange - red dwarf star (Sousa et al, 2008; and ARICNS), but is probably not an giant, star (SIMBAD) of spectral and luminosity type K3 - 5 V - III.
According to Professor Jim Kaler at the University of Illinois» Department of Astronomy, Rana started life as a main sequence F8 dwarf (somewhat hotter and brighter than Sol with slightly greater mass) around 7.5 billion years ago, but core hydrogen fusion has ceased causing the star to expand and cool as an active subgiant before becoming much brighter and larger «as a true giant star» through core helium fusion.
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.
Achernar is a blue - white main sequence star of spectral and luminosity type B3 Vpe (Hiltner et al, 1969), that previously had been classed as bright as a subgiant.
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.
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).
As a subgiant star subject to pulsations which affect careful measurements of radial velocity, astronomers would find it very difficult to detect any Earth - type planet arond this star using present methods.
A comparison with stellar properties in the planet - candidate catalog by Batalha et al. shows that radii for subgiants and giants obtained from spectroscopic follow - up are systematically too low by up to a factor of 1.5, while the properties for unevolved stars are in good agreement.
Abstract: Photometric observations made by the NASA Kepler Mission have led to a dramatic increase in the number of main - sequence and subgiant stars with detected solar - like oscillations.
We analyze our data using two Teff scales, the spectroscopic values from DR13 and those derived from SDSS griz... ▽ More (Abridged) We present the first APOKASC catalog of spectroscopic and asteroseismic data for 415 dwarfs and subgiants.
Asteroseismic analysis provides robust values for the mass and radius of HD 179070, 1.34 -LCB- \ pm -RCB- 0.06 M -LCB- \ circ -RCB- and 1.86 -LCB- \ pm -RCB- 0.04 R -LCB- \ circ -RCB- respectively, as well as yielding an age of 2.84 -LCB- \ pm -RCB- 0.34 Gyr for this F5 subgiant.
Life on an Earth - like planet, however, may have developed closer to the star before it evolved and began heating up out of the main sequence into a subgiant, thereby shifting its habitable zone outwards away from the star.
Abstract: (Abridged) We present the first APOKASC catalog of spectroscopic and asteroseismic data for 415 dwarfs and subgiants.
The primary component in the system is a spectroscopic binary with the stellar classification of B2 IV, matching the spectrum of a blue - white subgiant star.
The system is composed of a blue - white giant with the stellar classification of B9III - IV and a visual magnitude of 5.33, a white subgiant belonging to the stellar class A0IVMn with an apparent magnitude of 5.63, and a star with a magnitude of 8.5 separated from the second component by 37.7 arc seconds.
Dr. Baliunas has manuscripts in preparation (no coauthors) in the area of Ca II chromospheric surface magnetic activity and variability in F - G dwarfs and subgiants in M67.