New information about the heart of one of the most famous objects in the sky — the Crab Pulsar in the Crab Nebula — has been revealed by an international team of scientists searching for gravitational waves. The team’s achievement also is the first direct look into the interior of a neutron star.
2 June 2008 –New information about the heart of one of the most famous objects in the sky — the Crab Pulsar in the Crab Nebula — has been revealed by an international team of scientists searching for gravitational waves. The team’s achievement also is the first direct look into the interior of a neutron star.
The research team detected signals from the pulsar — a rapidly spinning neutron star — with the Laser Interferometer Gravitational-Wave Observatory (LIGO). The analysis of the signals reveals that has shown that no more than 4 percent of the energy loss of the pulsar is caused by the emission of gravitational waves. This long-awaited analysis is one of LIGO’s first landmark results, bringing the search for gravitational waves into the outskirts of the realm of theoretical predictions made several years ago by Ben Owen, assistant professor of physics at Penn State. Owen is a co-author of the paper describing the discovery, which will be submitted to Astrophysical Journal Letters by the LIGO Scientific Collaboration, a 600-member group in which Penn State plays a key role.
The Crab Nebula, located 6,500 light years away in the constellation Taurus, was formed in a spectacular supernova explosion in 1054. It was visible in daylight for more than three weeks and may briefly have been brighter than the full moon. Ancient Chinese texts referred to the extraordinary event as a “guest star.” Today, at the heart of the Crab Nebula, remains an incredibly rapidly rotating neutron star that sweeps two narrow radio beams across the Earth each time it spins. The lighthouse-like radio pulses have given the star the name “pulsar.”
“The Crab Pulsar is spinning at a rate of 30 times per second. However, its rotation rate is decreasing rapidly relative to most pulsars, indicating that it is radiating energy at a prodigious rate,” says Graham Woan of the University of Glasgow, who co-led the science group that used LIGO data to analyze the Crab Pulsar, along with Michael Landry of the LIGO Hanford Observatory.
Pulsars, which are only 10 km in radius yet contain more mass than the Sun, are almost perfect spheres made up of neutrons. Gravitational waves are ripples in the fabric of space and time and are an important consequence of Einstein’s general theory of relativity. Gravitational-wave emission is one of the few physical mechanisms hypothesized for the pulsar’s energy loss and the accompanying slowing of its spin, but the scenario that gravitational waves significantly “brake” the Crab pulsar has been disproved by the new analysis. “These results strongly imply that no more than 4 percent of the pulsar’s energy loss is due to gravitational radiation,” Michael Landry said. “The remainder of the loss must be due to other mechanisms, such as a combination of electromagnetic radiation generated by the rapidly rotating magnetic field of the pulsar and the emission of high-velocity particles into the nebula.”
LIGO scientists monitored the neutron star from November 2005 to August 2006 using data from the three LIGO interferometers, which were combined to create a single, highly sensitive detector. They compared the LIGO data with published data about the pulsar’s rotation rate from the Jodrell Bank Observatory, looking for a synchronous gravitational-wave signal.
The analysis revealed no signs of gravitational waves — a result the scientists say is important because it provides information about the pulsar and its structure. They say a perfectly smooth neutron star will not generate gravitational waves as it spins, and that LIGO would have been able to detect gravitational waves from a star whose shape was deformed by only a few meters. Such distortion could occur in a young neutron star, like the Crab Pulsar, whose crust could still be semisolid, or in a star with an enormous magnetic field.
According to Ben Owen, “What LIGO really adds is that we can see more than skin deep. Astronomers see plenty of electromagnetic waves (radio waves, x-rays, and so on) from the Crab, but pulsars are so dense that even the x-rays can’t get through the interior and you can only see down to the surface. But gravitational waves can get through, so our result is the first direct look into a neutron star’s interior.” Joseph Taylor, a Nobel Prize-winning radio astronomer and professor of physics at Princeton University, says, “The physics world has been waiting eagerly for scientific results from LIGO. It is exciting that we now know something concrete about how nearly spherical a neutron star must be, and we have definite limits on the strength of its internal magnetic field.”
Looking to the future of research with LIGO, Ben Owen adds, “For a long time particle physicists have predicted a lot of strange possibilities for neutron star interiors, like neutrons dissolving into more fundamental particles called quarks. As LIGO’s sensitivity improves, we can explore more of those possibilities. If we see a strong signal in the next couple of years, it will be strong evidence that these strange states of matter exist.”
Research with LIGO is carried out by the LIGO Scientific Collaboration, which includes the Penn State group, led by Lee Samuel Finn, professor of physics and of astronomy and astrophysics, and Ben Owen. The Penn State group plays a key role in the analysis of LIGO data and its scientific interpretation.
CONTACTS:
Ben Owen: owen@gravity.psu.edu; via Skype: benjaminjowen; at a hotel on the evening of 2 and all say on 3 June: (740)593-5600; via staff assistant: (+1)814-865-5203; in office on and after 5 June: (+1)814-863-9597 Barbara Kennedy (PIO): 814-863-4682, science@psu.edu
MORE ABOUT LIGO:
The LIGO project, which is funded by the National Science Foundation, was designed and is operated by Caltech and the Massachusetts Institute of Technology for the purpose of detecting gravitational waves, and for the development of gravitational-wave observations as an astronomical tool. The LIGO Scientific Collaboration interferometer network includes the LIGO interferometers (including the 2 km and 4 km detectors in Hanford, Washington, and a 4 km instrument in Livingston, Louisiana) and the GEO600 interferometer, located in Hannover, Germany, and designed and operated by scientists from the Max Planck Institute for Gravitational Physics and partners in the United Kingdom.
The next major milestone for LIGO is the Advanced LIGO Project, slated for operation in 2014. Advanced LIGO, which will utilize the infrastructure of the LIGO observatories, will be 10 times more sensitive. The increased sensitivity will be important because it will allow scientists to detect cataclysmic events such as black-hole and neutron-star collisions at ten-times-greater distances and to search for much smaller “hills” on the Crab Pulsar. Advanced LIGO will incorporate advanced designs and technologies that have been developed by the LIGO Scientific Collaboration. It is supported by the U.S. National Science Foundation, with additional contributions from the U.K. Science and Technology Facilities Council and the German Max Planck Gessellschaft.
