stars: low-mass
Very low mass stars and brown dwarfs in Upper Scorpius using Gaia DR1 : mass function, disks, and kinematics
... very low mass objects (VLMOs) in Upper Scorpius using UKIDSS colors and optimised proper motions calculated using Gaia ...and mass estimates updated using Gaia parallaxes for early type stars ...
27
2D dynamics of the radiative core of low mass stars
... a geostrophic solution with a cylindrical di ff erential ro- tation. Such a profile is very di ff erent from the shellu- lar rotation profile assumed in 1D models. These models should therefore be used carefully in the ...
5
A Search for Pulsation in Young Brown Dwarfs and Very Low Mass Stars
... object mass. Mass accretion rates decrease into the substellar regime, according to an approximate empirical correlation M ∝ M ∗ 2 (Muzerolle et ...very low mass (Vorobyov & Basu ...higher ...
317
Variability in young very low mass stars : two surprises from spectrophotometric monitoring
... and low dispersion Spectrograph2 at European Southern Obser- ...very low mass stars can be caused by different phenomena than in more massive T Tauri stars and can persist when the disc ...
16
Stellar astrophysics: a study of stellar physics with particular reference to low mass stars
... of low mass (LM) ...LM stars is ...very low mass ...LM stars. In addition, a number of properties of dense gases at low temperatures are demonstrated in the LM ...massive ...
183
Precision diagnostics of pulsation and evolution in helium rich low mass stars
... of low mass stars linked by their un- usually low hydrogen atmospheric abundance, usually completely replaced with ...sdO) stars are low-mass core helium burning ...
219
Revealing the Chamaeleon: Young, low mass stars surrounding eta and epsilon Cha
... scopy, we have identified eight low-mass stars that were ejected from η Cha over the past 5–10 Myr. Comparison with recent N-body simulations shows our results are consistent with a dynamical origin ...
15
The EBLM Project VI The mass and radius of five low mass stars in F+M binaries discovered by the WASP survey
... achieve mass uncertainties as low as ...the mass for single interferometric stars often requires photometric calibrations for red-dwarfs ...to mass-luminoisty relations has decreased ...
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Self consistent atmosphere modeling with cloud formation for low mass stars and exoplanets
... self-consistent model atmospheres, which at the same time will make it possible to reliably quantify such exciting features as po- tential biomarkers in the atmosphere, and hence open a route for the first scientific ...
17
Observational probes of helium ignition in low mass stars
... This research provides a foundation for future targeted searches in the quest to find observational evidence of the HeF and subsequent subflashes. Currently, there are only theoretical models in this space. Combining the ...
173
Studies of low mass interacting binary stars
... The residuals to the times of minima presented in Table 5.3 were calculated wi th respect to the ephemeris given by Chou (1959), and are shown plotted in Figure 5.3. Several interpretations of the data can be made other ...
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Simulating radio emission from low mass stars
... alone. Using the Güdel – Benz relation and the observed X-ray luminosity of V374 Peg ( L X = 10 28.44 ; Hünsch et al. 1999 ) , V374 Peg ’ s radio luminosity from gyrosynchrotron emission alone should be L n , R = 10 ...
8
Young, Low-Mass Stars: X-rays and Circumstellar Environments
... Sun-like stars, but does little to constrain the atmospheric chemistry of rocky planets around low mass ...nearby, low mass planet hosting stars (“Measurements of the Ultraviolet ...
248
Probing the Milky Way
... with Low Mass Young Stars is targeting these objects, with the aim of testing specific morphological predictions of jet ...from low-mass protostars and compare this with matching-beam ...
5
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 ...
5
Correlations between the stellar, planetary, and debris components of exoplanet systems observed by Herschel
... Given that planets are the end state of the agglomeration of smaller bodies from dust to planetesimals (neglecting as a de- tail the capture of an envelope from the protoplanetary disc for gas giants), and debris discs ...
14
Dynamos and Differential Rotation: Advances at the Crossroads of Analytics, Numerics, and Observations
... however, Lorentz-force feedback quenches both the con- vection and differential rotation. Similarly, as the rotation rate is increased, cycles become more likely to a point and then past this threshold they become less ...
16
Testing substellar models with dynamical mass measurements
... [12]. However, we emphasize that this apparent over-luminosity is based on a single system whose age is estimated from the primary star HD 130948A. While this young solar analog is fortuitously amenable to multiple ...
7
Early disc accretion as the origin of abundance anomalies in globular clusters
... around low-mass ...higher mass GCs, the velocity dispersion is expected to be higher (on average) which increases the amount of volume each star sweeps ...or mass for which the model ...
14
Correlations between the stellar, planetary, and debris components of exoplanet systems observed by Herschel
... Given that planets are the end state of the agglomeration of smaller bodies from dust to planetesimals (neglecting as a de- tail the capture of an envelope from the protoplanetary disc for gas giants), and debris discs ...
14