Headlines > News > Neutron stars may be too weak to power some gamma-ray bursts

Neutron stars may be too weak to power some gamma-ray bursts

Published by Klaus Schmidt on Thu Nov 4, 2010 8:14 am via: Eurekalert
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Black holes could produce the enormous energies of a burst, but not neutron stars.

A gamma-ray burst is an immensely powerful blast of high-energy light thought to be generated by a collapsing star in a distant galaxy, but what this collapse leaves behind has been a matter of debate.

This is an illustration of the collapse of a massive star in which the large envelope forms a rotationally supported disk and may even lead to a relativistic jet. This "collapsar" picture may explain at least one class of gamma-ray bursts, cosmic explosions that are a million trillion times as bright as the sun! Gamma-ray bursts last for anywhere from a few milliseconds to several minutes, and for that time they are the brightest source of gamma-rays in the entire observable Universe. Credit: Tony Piro/Caltech

This is an illustration of the collapse of a massive star in which the large envelope forms a rotationally supported disk and may even lead to a relativistic jet. This "collapsar" picture may explain at least one class of gamma-ray bursts, cosmic explosions that are a million trillion times as bright as the sun! Gamma-ray bursts last for anywhere from a few milliseconds to several minutes, and for that time they are the brightest source of gamma-rays in the entire observable Universe. Credit: Tony Piro/Caltech

A new analysis of four extremely bright bursts observed by NASA’s Fermi satellite suggests that the remnant from a long-duration gamma-ray burst is most likely a black hole – not a rapidly spinning, highly magnetized neutron star, or magnetar since such a burst emits more energy than is theoretically possible from a magnetar.

“Some of the events we have been finding seem to be pushing right up against this total limit for a neutron star progenitor system,” said S. Bradley Cenko, a post-doctoral fellow from the University of California, Berkeley.

Cenko will present these findings on Wednesday, Nov. 3, at the Nov. 1-4 Gamma Ray Bursts 2010 conference in Annapolis, Md. Cenko is a member of an international team that includes astronomers from UC Berkeley and the National Radio Astronomy Observatory (NRAO) in New Mexico.

The group has submitted a paper detailing its analysis to The Astrophysical Journal.

Long-duration gamma-ray bursts (GRBs) are presumed to be created by the explosive collapse in distant galaxies of massive stars. The explosion is visible from Earth because the light is emitted in a narrow cone, like a beam from a lighthouse. First discovered in 1967 by satellites looking for nuclear blasts on Earth, gamma-ray bursts have been the focus of several satellite missions, most recently NASA’s Fermi gamma-ray space telescope, launched in 2008, and NASA’s Swift satellite, launched in 2004.

With accumulating observations, astronomers have been able to create models of how the collapse of a rapidly rotating, massive star can accelerate matter to nearly the speed of light and collimate it into two oppositely directed, tightly focused beams along the spin axis. They have also studied how these particles generate gamma rays and other emissions.

The two leading candidates for powering these long-duration bursts are a magnetar and a black hole, sometimes referred to as a collapsar. In both cases, material from the star falls inward and is catapulted out by the spinning neutron star or black hole. What distinguishes these models is that magnetar-powered bursts cannot be as powerful as black hole-powered bursts.

“The question we have been trying to answer is: What is the true energy release from these events?” Cenko said. “We can measure all the light emitted – very high energy gamma rays, and, at later times, X-ray, optical and radio afterglow emissions – but that doesn’t provide a very good estimate, because GRBs emit in relatively narrow jets. We have to get an idea of the geometry of this outflow, that is, how collimated the jets are.”

Previous studies have shown that light measured in the afterglow begins to drop steeply at a certain point, and the sooner this drop-off, called a jet break, the narrower the jet. Typically, the gamma-ray burst itself lasts from a few seconds to as long as 100 seconds, but the afterglow, produced when the jets interact with gas and dust surrounding the star, emits visible light for a couple of weeks and radio radiation for several months.

While Swift has observed hundreds of bursts in the past five years and notified astronomers within seconds of detection, the instruments aboard the satellite detect mostly medium-sized bursts that are not as highly collimated and that have a jet break many days or weeks after the burst.

Fermi’s Large Area Telescope, however, is sensitive to very bright bursts with jet breaks within several days of the burst, making follow-up observations easier with Swift’s X-ray and ultraviolet-optical telescopes and the ground-based Very Large Array, a radio telescope operated by NRAO.

Fermi detects few extremely bright bursts, however – only four in 2009, Cenko said – and does not notify astronomers for nearly a day afterward. Once alerted, however, Cenko’s team was able to observe the optical, X-ray and radio afterglow of these four events, find the jet break and use this information, along with the star’s distance calculated from its redshift, to estimate the total energy output.

If the energy from these bright bursts were emitted in all directions, it would be equivalent to the mass of the sun being converted instantaneously into pure energy. Because the gamma-ray burst was focused in a cone only a few degrees wide, however, the energies for all four bursts were about 100

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