Printed from: PhysLink.com; http://www.physlink.com/News/Index.cfm?ID=592
Original publication date: Tuesday July 8, 2008.
Einsteins Theory Passes Strict, New Test
Scientists at McGill University used the National Science Foundation's Robert C. Byrd Green Bank Telescope (GBT) to do a four-year study of a double-star system unlike any other known in the Universe. The system is a pair of neutron stars, both of which are seen as pulsars that emit lighthouse-like beams of radio waves.
'Of about 1700 known pulsars, this is the only case in which two pulsars orbit around each other,' said Rene Breton, a graduate student at McGill University in Montreal, Canada. In addition, the stars' orbital plane is aligned nearly perfectly with their line of sight to the Earth. This causes the signal of one to be blocked, or eclipsed, as it circles the other.
'Those eclipses are the key to making a measurement that could never be done before,' Breton said.
Einstein's 1915 theory predicted that in a close system of two very massive objects, such as neutron stars, one object's gravitational tug, along with an effect of its spinning around its axis, should cause the spin axis of the other to wobble, or precess.
Studies of other pulsars in binary systems had indicated that such wobbling occurred, but could not produce precise measurements of the amount of wobbling.
'Measuring the amount of wobbling is what tests the details of Einstein's theory and gives a benchmark that any alternative gravitational theories must meet,' said Scott Ransom of the National Radio Astronomy Observatory.
The eclipses allowed the astronomers to pin down the geometry of the double-pulsar system and track changes in the orientation of the spin axis of one of them. As one pulsar's spin axis slowly moved, the pattern of signal blockages as the other passed behind it also changed. The signal from the pulsar in back is absorbed by the ionized gas in the other's magnetosphere.
Pulsars, first discovered in 1967, are the 'corpses' of massive stars that have exploded as supernovae. What is left after the explosion is a superdense neutron star that packs more than the mass of our Sun into the size of an average city. Beams of radio waves stream outward from the poles of the star's intense magnetic field and sweep around as the star rotates, as often as hundreds of times a second.
The pair of pulsars studied with the GBT is about 1,700 light-years from Earth. The average distance between the two is only about twice the distance from the Earth to the Moon. The two orbit each other in just under two and a half hours.
'A system like this, with two very massive objects very close to each other, is precisely the kind of extreme 'cosmic laboratory' needed to test Einstein's prediction,' said Victoria Kaspi, leader of McGill University's Pulsar Group. Theories of gravity don't differ significantly in 'ordinary' regions of space such as our own Solar System. In regions of extremely strong gravity fields, such as near a pair of close, massive objects, however, differences are expected to show up.
In the binary-pulsar study, General Relativity 'passed the test' provided by such an extreme environment, the scientists said.
'It's not quite right to say that we have now 'proven' General Relativity,' Breton said. 'However, so far, Einstein's theory has passed all the tests that have been conducted, including ours.'
Breton, Kaspi and Ransom worked with Michael Kramer of the Jodrell Bank Observatory at the University of Manchester in Great Britain; Maura McLaughlin of West Virginia University and the NRAO; Maxim Lyutikov of Purdue University and other colleagues in Canada, the U.S., France and Italy. The researchers presented their work in an article in the July 4 issue of Science Magazine.
The National Radio Astronomy Observatory is a facility of the National Science Foundation, operated under cooperative agreement by Associated Universities, Inc.
News Story Origin and Copyright:
NSF : http://www.nsf.gov
Original news release:
For more physics & astronomy stories like this one, go to: http://www.PhysLink.com