Variable stars in large magellanic cloud globular clusters II NGC 1786

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

The underlying reason for this is the establishment of a permanent photometric all-sky tracking of variable stars as a service to the astronomical community at large while at the

(c) Possible sources of Hα emission other than accretion are chromospheric activity, whose contribution is two orders of magnitude less than what we measure, Hα emission along the

Therefore, considering that the distribution of compact and large H II regions does not seem to depend on the galactocentric radius, that the observed scatter in metallicity is due

The RR values found in the VPR 2015 form’s indicators confirm that in contexts where protection of the victim is demanded based on the risk, the majority of risk indica- tors can

A comparison between the radio and X-ray populations in Orion shows that the radio detections so far have been strongly biased to the brighter X-ray stars. This supports the

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

Our results suggest that the conductance and thermopower of C 60 -terminated molecules are still quite sensitive to the binding geometry and we expect a large spread of values