CONTAMINATION BY SUPERNOVAE IN GLOBULAR CLUSTERS

Credit: ALMA (ESO/NAOJ/NRAO)/Alexandra Angelich (NRAO/AUI/NSF)

Only a small amount of the supernovae products remains trapped within globular clusters and this "catch" only occurs in the most massive cases (mass cluster ≥ 10^6 solar masses).
In smaller clusters instead there is no contamination by supernovae (supernova explosions produce heavier elements such as iron, gold, etc.). A group of astrophysicists has shown that the shock wave and the metals produced by supernovae disperse outside the cluster. This inhibits the gas contamination used by the first stellar generation (a new stellar generation can arise from the "recycled gas" expelled by supernovae). Only the material ejected by the supernova at the center of a massive cluster remain trapped (the ejected material moves in a high-density medium and remains locked) and it is available to a stellar population of second generation.

To know more
http://arxiv.org/abs/1511.02918
http://iopscience.iop.org/article/10.1088/2041-8205/814/1/L8/pdf

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Astrophysics collection (March 11, 2016)

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ORBITAL PERIODS OF THE PLANETS

For orbital period generally we refer to the sidereal period, that is the temporal cycle that it takes an object to make a full orbit, relative to the stars. This is the orbital period in an inertial (non-rotating) frame of reference (365,25 days for the earth).

A BINARY ORIGIN FOR A CENTRAL COMPACT OBJECT (CCO)?

Figure: False-Colour X-ray and infrared emission image from the core of the infrared shell. The RGB colours correspond to Chandra X-ray 0.2-10 keV (blue), IRAC infrared 8 μm (green), and HPACS 70 μm (red) data. The intensity scale is logarithmic for all channels. Overlaid are equal brightness levels from the MIPS 24 μm band. Note that around the CCO the infrared emission is suppressed in the 70 μm band and enhanced in the 24 μm band suggesting higher dust temperature. Credit: Doroshenko et al 2016 Central compact objects (CCOs) are thought to be young isolated neutron stars that were born during the preceding core-collapse supernova explosion.

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