Early 56Ni decay gamma rays from SN2014J suggest an unusual explosion.

Type Ia supernovae result from binary systems that include a carbon-oxygen white dwarf, and these thermonuclear explosions typically produce 0.5 solar mass of radioactive (56)Ni. The (56)Ni is commonly believed to be buried deeply in the expanding supernova cloud. In SN2014J, we detected the lines at 158 and 812 kiloelectron volts from (56)Ni decay (time ~8.8 days) earlier than the expected several-week time scale, only ~20 days after the explosion and with flux levels corresponding to roughly 10% of the total expected amount of (56)Ni. Some mechanism must break the spherical symmetry of the supernova and at the same time create a major amount of (56)Ni at the outskirts. A plausible explanation is that a belt of helium from the companion star is accreted by the white dwarf, where this material explodes and then triggers the supernova event.

A novel class of oral direct renin inhibitors: highly potent 3,5-disubstituted piperidines bearing a tricyclic p3-p1 pharmacophore.

A small library of fragments comprising putative recognition motifs for the catalytic dyad of aspartic proteases was generated by in silico similarity searches within the corporate compound deck based on rh-renin active site docking and scoring filters. Subsequent screening by NMR identified the low-affinity hits 3 and 4 as competitive active site binders, which could be shown by X-ray crystallography to bind to the hydrophobic S3-S1 pocket of rh-renin. As part of a parallel multiple hit-finding approach, the 3,5-disubstituted piperidine (rac)-5 was discovered by HTS using a enzymatic assay. X-ray crystallography demonstrated the eutomer (3S,5R)-5 to be a peptidomimetic inhibitor binding to a nonsubstrate topography of the rh-renin prime site. The design of the potent and selective (3S,5R)-12 bearing a P3(sp)-tethered tricyclic P3-P1 pharmacophore derived from 3 is described. (3S,5R)-12 showed oral bioavailability in rats and demonstrated blood pressure lowering activity in the double-transgenic rat model.

Sub-luminous type Ia supernovae from the mergers of equal-mass white dwarfs with mass approximately 0.9M[symbol: see text].

Type Ia supernovae are thought to result from thermonuclear explosions of carbon-oxygen white dwarf stars. Existing models generally explain the observed properties, with the exception of the sub-luminous 1991bg-like supernovae. It has long been suspected that the merger of two white dwarfs could give rise to a type Ia event, but hitherto simulations have failed to produce an explosion. Here we report a simulation of the merger of two equal-mass white dwarfs that leads to a sub-luminous explosion, although at the expense of requiring a single common-envelope phase, and component masses of approximately 0.9M[symbol: see text]. The light curve is too broad, but the synthesized spectra, red colour and low expansion velocities are all close to what is observed for sub-luminous 1991bg-like events. Although the mass ratios can be slightly less than one and still produce a sub-luminous event, the masses have to be in the range 0.83M[symbol: see text] to 0.9M[symbol: see text].