Ken J. Shen

TL;DR: In this article, the authors show that a double white dwarf AM Canum Venaticorum (AM CVn) binaries undergoes unstable thermonuclear flashes when the orbital period is in the 3.5-25 minute range.

TL;DR: The luminosity of the progenitor system (especially the companion star) is 10–100 times fainter than previous limits on other type Ia supernova progenitors systems, allowing us to rule out luminous red giants and almost all helium stars as the mass-donating companion to the exploding white dwarf.

TL;DR: A faint type Ib supernova is reported in the halo of the nearby isolated galaxy, NGC 1032, and it is concluded that it arises from a low-mass, old progenitor, likely to have been a helium-accreting white dwarf in a binary.

TL;DR: In this paper, the authors present a new non-detection limit of the nearby SN Ia 2011fe, obtained at a time that appears to be just 4-hr after the explosion, allowing them to directly constrain the initial primary radius (Rp ).

TL;DR: In this article, a new non-detection limit of the nearby SN Ia 2011fe, obtained what appears to be just 4 hours after the explosion, was presented, allowing us to directly constrain the initial primary radius, R_p Coupled with the nondetection of a quiescent X-ray counterpart and the inferred synthesized Ni mass, we show that R_ p 10,000 gm cm^{-3}, and that the effective temperature must be less than a few x 10^5 K.