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In a great opinion piece published by the Woodrow Wilson School of Princeton University, the authors describe setting a price on carbon as the best way to curb emissions and drive development of renewable energy.
Taking into account that fact that renewables are often not competitive on price alone and not even touching upon the existing or perceived fossil-fuel subsidies, the fact that the cost of carbon emissions is neglected in any policy or economic evaluation is of great concern.
For a company in the Philippines quoting a coal-project being cheaper than a geothermal project as key argument not to pursue the latter, showcases clearly that the future cost of the emissions from a coal plant to the economy and a nation as a whole is not sufficiently taken into consideration. Putting a price on carbon emissions not only levels the playing field, but takes into account the real cost of fossil-fuel based electricity generation. Dark energy is a mysterious force that pervades all space, acting as a "push" to accelerate the Universe's expansion. These supernovae are currently the best way to measure dark energy because they are visible across intergalactic space.
The best way of measuring dark energy just got better, thanks to a new study of Type Ia supernovae led by Ryan Foley of the Harvard-Smithsonian Center for Astrophysics. The new tool also will help astronomers to firm up the cosmic distance scale by providing more accurate distances to faraway galaxies.
Type Ia supernovae are used as standard candles, meaning they have a known intrinsic brightness. Even when astronomers correct for this effect, their measurements still show some scatter, which leads to inaccuracies when calculating distances and therefore the effects of dark energy.


Foley discovered that after correcting for how quickly Type Ia supernovae faded, they show a distinct relationship between the speed of their ejected material and their color: the faster ones are slightly redder and the slower ones are bluer. Previously, astronomers assumed that redder explosions only appeared that way because of intervening dust, which would also dim the explosion and make it appear farther than it was. The discovery provides a better physical understanding of Type Ia supernovae and their intrinsic differences. Headquartered in Cambridge, Mass., the Harvard-Smithsonian Center for Astrophysics (CfA) is a joint collaboration between the Smithsonian Astrophysical Observatory and the Harvard College Observatory. Despite being 70 percent of the Universe, dark energy was only discovered in 1998 by two teams observing Type Ia supernovae. Also, they can function as "standard candles" in distant galaxies since the intrinsic brightness is known.
He has found a way to correct for small variations in the appearance of these supernovae, so that they become even better standard candles. Studies looking for ways to make more accurate corrections have had limited success until now.
Trying to correct for this, they would incorrectly calculate that the explosion was closer than it appeared. It also will allow cosmologists to improve their data analysis and make better measurements of dark energy - an important step on the road to learning what this mysterious force truly is, and what it means for the future of the cosmos.


CfA scientists, organized into six research divisions, study the origin, evolution and ultimate fate of the universe. We accept all space related events in our calendar and all it takes is about 5 minutes for your to fill out the online event form.
Just as drivers estimate the distance to oncoming cars at night from the brightness of their headlights, measuring the apparent brightness of a supernova yields its distance (fainter is farther). He presented his findings in a press conference at the 217th meeting of the American Astronomical Society. More importantly, it went back to "first principles" and reexamined the assumption that Type Ia supernovae are one average color. In particular, there is a known correlation between how quickly the supernova brightens and dims (its light curve) and the intrinsic peak brightness.



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