[PDF] Top 20 Low-mass stars: Open problems all along their evolution
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Low-mass stars: Open problems all along their evolution
... Lyr stars have to be explained in a different ...the evolution for only 36 hrs of physical time, the results show that the physics of the core helium flash is far from full ...still open question ... See full document
10
Selected topics in the evolution of low-mass stars
... too low, or/and the physical ingredients that are used in the computation of stellar models, and especially those that depend strongly on the metallicity (such as radiative opacities), are somehow in ...with ... See full document
11
Implications of the generation of internal gravity waves by penetrative convection for the internal rotation evolution of low-mass stars
... in low-mass stars and the theoret- ical thresholds for the di ff erential ...stellar evolution code to model the evolution of the internal rotation along the stars ... See full document
5
Precision diagnostics of pulsation and evolution in helium rich low mass stars
... subdwarf stars, provid- ing spectroscopic classifications for 5055 hot subdwarfs, 540 of which are ...2122 stars with spectra in the SDSS ...helium-rich stars such as He-sdOs, RVs of such ... See full document
219
The helium burning evolution of low mass stars
... The more luminous Cepheids W vir star s are identified with stars undergoing blueward loops from the second giant branch in response to helium shell flashes or finally e volving to the b[r] ... See full document
162
Young, Low-Mass Stars: X-rays and Circumstellar Environments
... photodissociation is sufficiently large, the atmosphere can be pushed out of thermochemical equilib- rium (see, e.g., Moses, 2014; Miguel & Kaltenegger, 2014; Hu & Seager, 2014). This effect has been observed in ... See full document
248
Observational probes of helium ignition in low mass stars
... CFP evolution times derived here with results from other areas of study, such as asteroseismology, has the potential to provide highly detailed observational criteria immediately pre– and ...CFP evolution ... See full document
173
2D dynamics of the radiative core of low mass stars
... the evolution of the fluid on secular timescale, we solve as a first step the steady equation of the vortic- ity combined with the equations of energy and continu- ity using the Boussinesq approximation ([38], ... See full document
5
Simulating radio emission from low mass stars
... convective, low-mass stars is generated is far from complete; however, magnetic imaging of bright, rapidly rotating stars through Zeeman Doppler Imaging ( ZDI; Semel 1989; Donati et ...and ... See full document
8
An attempt to calibrate core overshooting using the seismic properties of low-mass stars
... the stars can be unambiguously established in most cases: 12 stars of the sample are found to be in the MS ...10 stars in the PoMS (e.g. Fig. 2b), and for only 2 stars of the sample, the ... See full document
5
Stellar astrophysics: a study of stellar physics with particular reference to low mass stars
... initial mass function and stressed the importance of the mass-luminosity relation in the determination of the low- luminosity mass ...the evolution of objects having masses around the ... See full document
183
The open flux evolution of a solar-mass star on the main sequence
... of open flux estimated by the PFSS ...modes, stars with dipolar surface fields have the most open flux and that the open flux decreases with increasing spherical harmonic degree (quadrupole, ... See full document
11
Low-Mass Stars and Their Companions
... young stars, we can measure their masses by observing the kinematics of the disk of gas and dust surrounding the star (Czekala et ...of stars with ages larger than 10 million years but not yet onto the main ... See full document
235
Revealing the Chamaeleon: Young, low mass stars surrounding eta and epsilon Cha
... sequence stars of various ...populations—the open cluster η Chamaeleontis and the nearby � Chamaeleontis Association—are ideal laboratories in which to study the formation and evolution of sparse ... See full document
15
The APACHE Project
... favorable mass ratios allow for detection of rocky, potentially habitable planets with the RV technique, thanks to the moderately large amplitudes of the RV signals (a few ...the mass range between Neptune ... See full document
8
The EBLM Project V Physical properties of ten fully convective, very low mass stars
... ten stars, and exceeds the radius predicted by the Exeter/Lyon stellar evolution ...of mass and radius is shown in Figure ...stellar evolution models (Dotter et ...very-low-mass ... See full document
19
The secondary stars in cataclysmic variables and low-mass X-ray binaries
... secondary stars in cataclysmic variables (CVs) and low-mass X-ray binaries (LMXBs), using the new catalogue of Ritter & Kolb as a starting ...reliable mass determinations of CV secondary ... See full document
15
Self consistent atmosphere modeling with cloud formation for low mass stars and exoplanets
... hence open a route for the first scientific discussions of possible life forms on nearby extrasolar ...of stars, M- L- and T-type stars (and brown dwarfs), whose orbit- ing exoplanets we already ... See full document
17
A Search for Pulsation in Young Brown Dwarfs and Very Low Mass Stars
... an open question, as the wavelength dependence of pulsation amplitudes is unknown and cannot be effectively determined with- out complex three-dimensional stellar ...late-type stars, which have been ... See full document
317
Studies of low mass interacting binary stars
... The secondary component is also found to occupy an interesting position on the HR diagram, lying near the ZAMS line, to the left of the other B-type secondary com ponents, and to the right of the W -type secondary ... See full document
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