Kyoto, Japan -- The size of our universe and the bodies within it is incomprehensible for us lowly humans. The sun has a mass that is more than 330,000 that of our Earth, and yet there are stars in the universe that completely dwarf our sun.

Stars with masses more than eight times that of the sun are considered high mass stars. These form rapidly in a process that gives off stellar wind and radiation, which could not result in stars of such high mass without somehow overcoming this loss of mass, or feedback. Something is feeding these stars, but how exactly they can accumulate so much mass so quickly has remained a mystery.

Observations of enormous disk-like structures that form around a star -- accretion disks -- had been proposed as the chief way of rapidly feeding young stars. However, a team of researchers from several institutions including Kyoto University and the University of Tokyo, has discovered another possibility.

Identifying a mineral might sound straightforward: analyze its chemistry, compare it to known minerals and voilà. But for geologists, this process can be a time-consuming puzzle requiring specialized expertise and a lot of manual calculation. Now, a team of researchers at Rice University’s Department of Earth, Environmental and Planetary Sciences has developed MIST — Mineral Identification by Stoichiometry — the first online tool capable of automatically identifying hundreds of different mineral species from their chemical composition using a carefully designed rules-based algorithm.

For the first time, astrophysicists detected a supernova embedded in a wind rich with silicon, sulfur and argon. Observations suggest the massive star lost its outer hydrogen and helium layers long before exploding. Discovery offers direct evidence of the long-theorized inner shell structure of massive stars.