AN OVERVIEW OF THE ROTATIONAL BEHAVIOR OF METAL POOR STARS

No obstante, como esta enfermedad afecta a cada persona de manera diferente, no todas las opciones de cuidado y tratamiento pueden ser apropiadas para cada individuo.. La forma

Finally, the IMF of a stellar sample mainly com- posed of discy YSOs from MC09 combined with some additional X-ray stars is utilized to estimate the total number of stars inside

Table 4 summarizes typical values for the equivalent widths and their relative variabilities, the minimum and maximum values, the percentage of objects showing line variations, and

The separation into in-situ and accreted stars indicates that the negative slope partly origi- nates from the in-situ stars, but the steepening of the gradi- ents in the outer

parameters of the binary orbit and the masses of the neutron stars can be measured with very high precision by accurate timing measurements.... The Masses of the Neutron Stars in

That is, local MS stars located at a dis- tance shorter than ∼2.5 kpc are not affected by the presence of the star-forming region G61.48 +0.09, but more distant MS stars have

Second, the sample of less massive (M  ≤ 1.5 M  ) giant stars with planets covers the same mass range as the MS pro- genitors and subgiant stars where the metal signature has

Figure 12 shows the current stellar age distribution (SAD; normalised to the mass of the whole galaxy) for Selene’s disc stars in the four scaled regions (solid black line). We