Category Astronomy/Space

Are we alone? Setting some limits to our planet’s uniqueness

Illustration of the Drake equation and the Frank equation. In 1961, astrophysicist Frank Drake developed an equation to estimate the number of advanced civilizations likely to exist in the Milky Way galaxy. The Drake equation (top row) has proven to be a durable framework for research, and space technology has advanced scientists' knowledge of several variables. But it is impossible to do anything more than guess at variables such as L, the probably longevity of other advanced civilizations. In new research, Adam Frank and Woodruff Sullivan offer a new equation (bottom row) to address a slightly different question: What is the number of advanced civilizations likely to have developed over the history of the observable universe? Frank and Sullivan's equation draws on Drake's, but eliminates the need for L. Credit: Image courtesy of University of Rochester

Illustration of the Drake equation and the Frank equation. In 1961, astrophysicist Frank Drake developed an equation to estimate the number of advanced civilizations likely to exist in the Milky Way galaxy. The Drake equation (top row) has proven to be a durable framework for research, and space technology has advanced scientists’ knowledge of several variables. But it is impossible to do anything more than guess at variables such as L, the probably longevity of other advanced civilizations...

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Don’t Touch: How Scientists Study the Reactions Inside Stars

Left: Chart of nuclides and important astrophysical reactions. Right: SOHO-EIT image from 14 September 1997 showing a huge eruptive prominence in the resonance line of singly ionized helium (He II) at 304 Angstroms in the extreme ultraviolet. The material in the eruptive prominence is at temperatures of 60,000 - 80,000 K, much cooler than the surrounding corona, which is typically at temperatures above 1 million K. Credit: Image courtesy of Texas A&M Cyclotron Institute and NASA

Left: Chart of nuclides and important astrophysical reactions. Right: SOHO-EIT image from 14 September 1997 showing a huge eruptive prominence in the resonance line of singly ionized helium (He II) at 304 Angstroms in the extreme ultraviolet. The material in the eruptive prominence is at temperatures of 60,000 – 80,000 K, much cooler than the surrounding corona, which is typically at temperatures above 1 million K. Credit: Image courtesy of Texas A&M Cyclotron Institute and NASA

How old is the universe? What causes a star to catastrophically explode? Answering these and other questions about stellar evolutions requires knowing the rates of the reactions involved...

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Possible Extragalactic Source of High-Energy Neutrinos

Fermi LAT images showing the gamma-ray sky around the blazar PKS B1424-418. Brighter colors indicate greater numbers of gamma rays. The dashed arc marks part of the source region established by IceCube for the Big Bird neutrino (50-percent confidence level). Left: An average of LAT data centered on July 8, 2011 covering 300 days when the blazar was inactive. Right: An average of 300 active days centered on Feb. 27, 2013, when PKS B1424-418 was the brightest blazar in this part of the sky. Credit: NASA/DOE/LAT Collaboration

Fermi LAT images showing the gamma-ray sky around the blazar PKS B1424-418. Brighter colors indicate greater numbers of gamma rays. The dashed arc marks part of the source region established by IceCube for the Big Bird neutrino (50-percent confidence level). Left: An average of LAT data centered on July 8, 2011 covering 300 days when the blazar was inactive. Right: An average of 300 active days centered on Feb. 27, 2013, when PKS B1424-418 was the brightest blazar in this part of the sky. Credit: NASA/DOE/LAT Collaboration

Nearly 10 billion years ago in galaxy PKS B1424-418, a dramatic explosion occurred. Light from this blast began arriving at Earth in 2012. Now, an international team have shown that a record-breaking neutrino seen around the same time likely was born in the same event...

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Rare Transit of Mercury to take place on 9 May

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The smallest planet in our Solar System will pass directly between the Earth and the Sun May 9. The last time this happened was in 2006, and the next 2 occasions will be in 2019 and 2032. During the transit, which takes place in the afternoon and early evening in the UK, Mercury will appear as a dark silhouetted disk against the bright surface of the Sun.

From the UK the transit begins at 1112 GMT (1212 BST), when the limb of Mercury appears to touch the limb of the Sun, and ends at 1842 GMT (1942 BST) when the limb of the silhouetted planet appears to leave the Sun. Observers in different locations will see the transit taking place at a slightly different time, as the planet will appear to take a slightly different path across the Sun.

Rare transit of Mercury to take place on 9 May

The transit of Mercury of November 2006...

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