Text Box: The star explosion that expels all or most of the star’s mass with extreme luminosity is what we have occasionally come to marvel in the firmament as the supernova. What triggers and powers this abrupt and cataclysmic demise of a bright and active star? 
This has been one of the most nagging and contentious questions in the list in fundamental astrophysics. 
Not surprisingly, a simple and viable answer is now found in the new light.
Text Box: Says geochemist Douglas Hammond of the University of Southern California (USC) in Los Angeles: "Everybody always assumes radioactive decay to be totally independent of temperature, pressure, and chemical form. It seems there are some exceptions." ...
When Fritz Bosch and his colleagues at the Gesellschaft für Schwerionenforschung in Darmstadt, Germany, stripped away all the electrons from rhenium nuclei, something that might happen in a star's harsh interior, its half-life plummeted from 42 billion years to 33 years [that's from 42, 000,000,000 to a mere 33]. But, until now, researchers have detected only tiny variations (or none at all) in the decay rate of beryllium and other atoms under Earth-like conditions...
Tweaking the Clock of Radioactive Decay, Richard A. Kerr, Science 286, 882-883 (29 October 1999)
        Back to Part 1 of 2
A Synopsis The Cosmos The Spin
ADDENDA The Cosmological Redshift The Neutrino
Two-Slit Tests The Galaxy Nuclear Reactions
NASA Tests Gravity The Sun
KamLAND Test Anti-Gravity The Pulsar
UCLA Test Relativity Superconductivity
Q and A Mass-Energy Fusion Energy
 Eugene Sittampalam
 1 December 2007