Stars: evolution
Hydromagnetic equilibria and their evolution in neutron stars
... Abstract. The strongest known magnetic fields are found in neutron stars. I briefly discuss how they are inferred from observations, as well as the evidence for their time-evolution. I go on to show how these ...
11
Stable magnetic equilibria and their evolution in the upper main sequence, white dwarfs, and neutron stars
... neutron stars appear to be subject to pro- cesses that can erode the stable stratification and therefore cause an MHD-stable field to decay on time scales shorter than their observable ...the evolution is ...
10
Magnetic field evolution in neutron stars: one dimensional multi fluid model
... tron stars approach a magnetohydrostatic quasi-equilibrium on a timescale not much longer than the Alfvén time, which is of the order of ...early evolution is mimicked by a artificial friction force term ...
15
BINARIES MIGRATING IN A GASEOUS DISK: WHERE ARE THE GALACTIC CENTER BINARIES?
... the stars is increased by about one order of magnitude for ε = ...the stars is severely under-resolved, in contrast to the results presented with our fiducial softening length, and that the resulting ...
19
Deep census of variable stars in a VLT/VIMOS field in Carina
... Variable stars provide important information about the nature and evolution of stars in various regions of our ...binary stars provide us information about the masses and radii of stars ...
12
Simulations of star formation in a gaseous disc around Sgr A* a failed Active Galactic Nucleus
... For longer cooling times, that is, β 1, disc fragmentation is less vigorous, creating fewer stars and leading to a more top-heavy IMF. In this case, while the gaseous mass is still comparable to the stellar mass ...
13
Instability of magnetic equilibria in barotropic stars
... stratified stars, numerical magnetohydrodynamics simulations have shown that arbi- trary initial magnetic fields evolve into stable equilibrium configurations, usually containing nearly axisymmetric, linked ...
11
Gauging the Helium Abundance of the Galactic Bulge RR Lyrae Stars
... variable stars, with ages typically > 11 Gyr ( ...Lyrae stars are typical members of Galactic globular clusters and the fi eld of the Galactic halo but have also been found in large numbers toward the ...
5
Stellar evolution and variability in the pre ZAHB phase
... tuations, stars are fed into the pre-ZAHB phase at an essen- tially constant ...some stars might have an assigned age that is older than their maximum calculated pre- ZAHB lifetime; these stars are ...
8
Formation of multiple populations in globular clusters: another possible scenario
... massive stars (super-AGB and/or AGB stars). As a result, the newborn stars belonging to the fourth generation (4G) will have a chemical composition that is a mixture of products from the three ...
15
Massive stars in the SDSS IV/APOGEE SURVEY I OB stars
... massive stars, from O-type dwarfs to their evolved counterparts ( blue super-giants, hyper-giants, and / or Wolf-Rayet stars ) is of utmost importance to understand star formation and further ...
11
Constraints on Helium Enhancement in the Globular Cluster M3 (Ngc 5272): The Horizontal Branch Test
... HB stars in ...HB stars in M13 (NGC 6205) have a similar helium abundance as in ...more stars in both clusters would certainly prove of interest to derive more conclusive ...
6
Deep multi survey classification of variable stars
... In this work, we have presented a CNN architecture to classify variable stars, tested on light curves integrated from various surveys. The proposed model can learn from the se- quence of differences between ...
54
Automatic survey invariant classification of variable stars
... We extract features from the lightcurves using the Feature Analysis for Time Series (FATS) Python package (Nun et al., 2015). In addition to the two top features according to the importance ranking presented by Nun et ...
79
Intergalactic stellar populations in intermediate redshift clusters
... The current state-of-the-art results indicate, for exam- ple, that while AGN feedback reduces the discrepancy be- tween models and observations, the ICL fractions observed in a reasonably representative sample of ...
10
Obscured clusters III Follow up observations of Mercer 23
... The stars in our spectroscopic study ranged in magnitudes from 7th to greater than ...the stars for the slit position containing Objects 9, 10 and 11 were relatively dim, we pushed the on-source integration ...
11
Clustering based feature learning on variable stars
... Most of the automatic classification tools coming from the Machine Learning commu- nity are very effective in the sense that they can produce high accuracy results and work very fast in the classification stage (after ...
78
The double sub giant branch of NGC 6656 (M 22): a chemical characterization
... AGB stars of higher masses. However, stars with initial masses >3 M will evolve in 300 Myr, which would agree with our derived upper limit on the age difference of the two SGBs in M ...
18
On a New Theoretical Framework for RR Lyrae Stars II Mid infrared Period Luminosity Metallicity Relations
... To explore the detailed physics behind these remarkable properties, Marconi et al. ( 2015 ) used new, time- and metal- dependent convective hydrodynamic models to derive a theoretical calibration for the period – ...
19
Automatic classification of poorly sampled variable stars
... Automatic classification of lightcurves success depends on two important and sepa- rated aspects of the process. First is the type of classifier being used. There are many different supervised classification algorithms ...
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