This issue includes material about the messengers from nuclear physics processes which underlie formation of all the elements heaver than helium in the universe, and which make stars and supernovae shine. ‘Radioactivities’ is the common theme, with the papers originating from an interdisciplinary workshop discussing the diversified views on radioactive isotopes in astrophysics.

No evidence was found in nanodiamond stardust for the former presence of extinct ²⁶Al or ⁴⁴Ti. Observed overabundances of r-process-only ¹⁹⁸Pt are in line with previously found excesses of heavy Xe and Te isotopes. As an alternative to dedicated scenarios, we have explored the r-process as a possible explanation.

Many neutron stars and runaway stars apparently come from the same regions on the sky. This suggests that they share the same birth places. To identify these birth places, we attempt to find NS-runaway pairs that could be possible former companions that were disrupted in a supernova. If nearby and recent, the remains are still visible in emission of radioisotopes.

The complementary technique of neutron activation and subsequent accelerator mass spectrometry (AMS) measurement was for the first time applied to studying ¹⁴C production from ¹³C(n,γ) and ¹⁴N(n,p). New data for these neutron poisons obtained for neutron energies between 25 and 178 keV are slightly lower than previous results and evaluations suggest.

We present colour transformations for the conversion of WISE magnitudes to the BVI_c, gri, and JHK_s photometric systems for red clump stars. The selected samples were used to obtain metallicity-dependent and free-of-metallicity transformations. These transformations can be used in the studies of the Galactic structure.

Expanding upon Pimbblet's 2011 analysis of career h-indices for members of the Astronomical Society of Australia, we provide additional citation metrics which are geared to quantifying the current performance of all professional astronomers in Australia.

We monitored the Ca ii lines of HD 179949 at the McDonald Observatory to observe planet induced emission (PIE) as an effect of star–planet interaction. Detailed statistical analysis revealed fluctuations in the Ca ii K core consistent with previous studies. We also confirmed the reality and temporal evolution of the phase shift of the maximum of star–planet interaction.

We analysed GSC 02038-00293's light curve and modelled its light variation at out-of-eclipse phases using the phoebe and spotmodel programs. The analyses indicated that there are two migrating active longitudes for the active component. The amplitude at out-of-eclipse phases varies in a sinusoidal way with a period of 8.9 yr, while the mean brightness is dramatically decreasing.

In this article, we investigate the behavior of orbits in an axially symmetric galactic-type potential. Our numerical calculations suggest that in this potential, there are two kinds of orbits: (i) escaping and (ii) trapped, which do not escape at all. Among the chaotic orbits, there are orbits that escape fast and also orbits that remain trapped for vast time intervals.

A coronal jet ejection from a sunspot light bridge is presented. It is confirmed that the jet has its root near the light bridge. This suggests that the jet may be a result of reconnection between the main sunspot and the light bridge.