White dwarf stars are the final evolutionary stage of the vast majority of stars, including our Sun. Since the coolest white dwarfs are very old objects, the present population of white dwarfs contains a wealth of information on the evolution of stars from birth to death, and on the star fo...
We analyse evolutionary tracks at young ages for low mass stars with masses m :S 1.4 M0 and brown dwarfs down to one mass of Jupiter. We analyse current theoretical uncertainties due to initial conditions. Simple tests on initial conditions show the high uncertainties of models at ages ,;S ...
which otherwise obscured the past history of these cancer clones (Fig.2a). However, many normal and BBL samples collected at the same time enabled the analysis of the early history
Sternberg Astronomical Institute CCD observations ASAS-3 catalog quadratic light elements O-C diagram instability strip data reduction Eddington-Plakidis method NSV 9159/ A9730G delta Cep, W Vir, RV Tau, and delta Sct stars A9710C Stellar interiors, evolution, nucleosynthesis, and ages/ NSV 9159...
Intelligent life may be so hard to produce that our universe may need to evolve an entire galaxy of stars to develop one intelligent planet, on average. Evolution on Earth has seemed equally wasteful and violent, if we focus on all the species that have disappeared, rather than the ...
For instance, we show that for a cluster where 10^5 Mo have been transformed into stars, the dispersion of EW(Hb) is about 18% within the 90% confidence levels at ages between 3.5 and 5 Myrs. 展开 关键词: GALAXIES:EVOLUTION DOI: 10.1086/301507 被引量: 146 ...
extensive debate about the best approaches for gene age inference in the last years, please follow myupdated discussion about the gene age inference literature. WithGenEra, we addressed all previously raised issues and we encourage users to runGenErawhen aiming to infer gene ages for furthermyTAI...
The evolution of binaries containing low-mass donors (<=2 M) and degenerate accretors (i.e., white dwarfs [0.7 M] or neutron stars [1.4 M]) is systematically investigated over a wide expanse of parameter space. The donors are assumed to have metallicities in the range of 0.0001<=Z<=0....
Central compact objects (CCOs) constitute a population of radio-quiet,slowly-spinning ($\\ge$100 ms) young neutron stars with anomalously high thermalX-ray luminosities. Their spin-down properties imply weak dipole magneticfields ($\\sim$$10^{10-11}$ G) and characteristic ages much greater ...
stars: AGB and post-AGBEvolutionary population synthesis models for a wide range of metallicities, ages, star formation histories, initial mass functions and horizontal branch morphologies, including blue morphologies at high metallicity, are computed. The model output comprises spectral energy ...