giant stars
New spectroscopic binary companions of giant stars and updated metallicity distribution for binary systems
... solar-type stars red- der than B − V = 0.625 are more frequent around stars with [Fe / H] ...of stars in the combined sample (13 systems), and therefore with the largest error ...planet-hosting ...
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Prospects for asteroseismic inference on the envelope helium abundance in red giant stars
... Since the models do not supply uncertainties with the frequencies, artificial uncertainties were added. We initially gave each second difference an uncertainty of 0 . 044 µ Hz. This was based on the uncertainties of the ...
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Infrared colours and inferred masses of metal poor giant stars in the Keplerfield
... 7,432 stars that meet our photometric giant star ...(6%) stars that we identify as likely giant stars (from photometry), but APOGEE does not report a ...photometrically-selected ...
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Asteroseismology of red giant stars: The potential of dipole modes
... red giant of 5 R , a rotation splitting that increases as the g-character of the mode increases, producing a “V” shape variation of rotation splitting around the pressure-dominated ...red giant ...
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Constraining stellar physics from red-giant stars in binaries – stellar rotation, mixing processes and stellar activity
... heartbeat stars from eclipsing binaries is unpractical and unnecessarily narrowing down sample ...oscillating stars in binaries can be identified from the phase modulation of coherent modes [45, ...
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Bad prospects for the detection of giant stars' tidal disruption: effect of the ambient medium on bound debris
... and/or giant stars. Consequently, although disruptions of evolved stars have been proposed as a useful probe of black holes with masses 10 8 M , we argue that the associated flares are likely less ...
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The Pan-Pacific planet search. III. Five companions orbiting giant stars
... Sun-like stars in the solar neighbourhood, but their sample did not include evolved stars, and it remains unclear how the orbital parameters of a binary system are affected by a component’s ...
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Precise radial velocities of giant stars. I. Stable stars
... radial velocity is plotted as a function of B −V color. The major- ity of the bluer stars show smaller variations in the radial velocity than the redder ones. This increase of the radial velocity vari- ability ...
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Modelling of Red Giant Stars: The state-of-the-art
... MS stars, the SFC theory yields results very similar to those derived from a solar calibrated MLT regarding the exten- sion of the convective zones, temperature gradients, and energy fluxes, whereas for RGB ...
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On the oscillation spectrum of a magnetized core in a giant star
... the giant stars observed by the Kepler mission, a feature that has been explained by the presence of magnetic fields in the core of these stars (Fuller et ...a giant star modeled by a stably ...
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From K giants to G dwarfs: stellar lifetime effects on metallicity distributions derived from red giants
... all giant stars that are present, it still does not account for the fact, demonstrated here, that their MDFs may still be biased by the over- or under-representation of stars of differing ...
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Spectrum synthesis of evolved stars
... metal-poor stars provides an opportunity to investigate the properties of objects which were probably formed during the early evolution of the ...Dwarf stars, in which no products of nuclear processing are ...
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Accretion disks formed from tidally-disrupted companions inside AGB stars
... distribution, we modified the profiles in accordance with Ohlmann (2016) for hy- drodynamical stability. With the modified profiles we contructed an AstroBEAR module to simulate an accretion disk inside the stellar ...
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Asteroseismology of hot B subdwarf stars
... Branch stars (also known as hot B subdwarfs or sdB stars) offer strong opportunities to study, through asteroseismology, the structure and internal dynamics of stars in this intermediate stage of ...
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Weighing in on the masses of retired A stars with asteroseismology : K2 observations of the exoplanet host star HD 212771
... sequence stars and cool subgiants) and red-giant stars (for a review, see Chaplin & Miglio ...These stars exhibit solar-like oscillations, which are stochastically excited and ...
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Wagstaff, Graham (2018): Convective and atmospheric boundaries of asymptotic giant branch stars. Dissertation, LMU München: Fakultät für Physik
... mass stars up until the last TP, although even then it is often the case that convergence becomes an issue as the star loses the remainder of its convective envelope, forming the central stars of planetary ...
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Financial Intermediation and Economic Growth: Bank Credit Maturity and Its Determinants
... of stars, relative to the “fixed” background stars, perpendicular to the observer’s line of ...background stars and gave them a special term: ...nearby stars are determined using simple ...
157
The eleventh and twelfth data releases of the Sloan Digital Sky Survey : final data from SDSS III
... MARVELS data collection began in 2008 October and ended in 2012 July. The majority of MARVELS stars were observed 20 – 40 times ( Figure 1 ) with typical exposure times of 50 – 60 minutes. These exposure times ...
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Energetic properties of stellar pulsations across the Hertzsprung-Russell diagram
... Scuti stars or ZZ Ceti white dwarfs, the transport by convection in these layers can be e ff ective and the pulsation-convection coupling should be taken appropriately into ...
6
Asymptotic Giant Branch Stars and presolar grains
... New attempts were also presented, aimed at modelling quantitatively extramixing phe- nomena suitable to explain the isotopic admixture of oxygen (and carbon) in advanced evo- lutionary phases of low mass stars. We ...
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