C. Simon Jeffery

TL;DR: In this article, the authors examined three sets of assumptions concerning the distribution of debris material between a disc and a corona, and showed that a model comprising both fast accretion to form a (hot) corona andslow accretion from a (cold) debris disc can reproduce the observed distribution of helium-rich subdwarfs in terms of their surface temperatures, gravities, nitrogen and carbon.

TL;DR: In this article, the proper motions, radial velocities, rotational velocity, and chemical abundances of the central six stars of Tycho's supernova remnant (SN 1572) were measured using the Hubble Space Telescope and HIRES spectroscopy.

TL;DR: In this paper, a "destroyed-disc" model was introduced to simulate the effect of direct disc ingestion into the expanding envelope of a white dwarfs (WDs) in order to guide calculations of the post-merger evolution of carbon-oxygen + helium (CO+He) WD binaries.

TL;DR: The most massive He-rich subdwarf O (sdO) stars develop a strong He-burning shell and evolve to become He-Rich giants as discussed by the authors, which represents a third evolution channel for the latter, in addition to the CO+He white dwarf merger and the very late thermal pulse channels proposed previously.

TL;DR: In this article, the authors investigated three possible channels for helium white-dwarf + red-giant mergers, and found that only a high-mass helium white dwarf subducted into a low core-mass red giant can make an early-type R star.