'Jekyll and Hyde' star morphs from radio to X-ray pulsar and back again

September 25, 2013
Neutron star and its companion during a period of accretion when the neutron star emits powerful X-rays. Credit: Bill Saxton; NRAO/AUI/NSF

Astronomers have uncovered the strange case of a neutron star with the peculiar ability to transform from a radio pulsar into an X-ray pulsar and back again. This star's capricious behavior appears to be fueled by a nearby companion star and may give new insights into the birth of millisecond pulsars.

"What we're seeing is a star that is the cosmic equivalent of 'Dr. Jekyll and Mr. Hyde,' with the ability to change from one form to its more intense counterpart with startling speed," said Scott Ransom, an astronomer at the National Radio Astronomy Observatory (NRAO) in Charlottesville, Va. "Though we have known that X-ray binaries—some of which are observed as X-ray pulsars—can evolve over millions of years to become rapidly spinning radio pulsars, we were surprised to find one that seemed to swing so quickly between the two."

Neutron stars are the superdense remains of massive stars that have exploded as supernovas. This particular neutron star, dubbed IGR J18245-2452, is located about 18,000 light-years from Earth in the constellation Sagittarius in a known as M28. It was first identified as a millisecond radio pulsar in 2005 with the National Science Foundation's Robert C. Byrd Green Bank Telescope (GBT) and then later rediscovered as an X-ray pulsar by another team of astronomers in 2013. The two teams eventually realized they were observing the same object, even though it was behaving very differently depending on when it was observed. Additional observations and archival data from other telescopes confirmed the on-again, off-again cycle of X-ray and radio pulsations.

"Various observations of one particular star over the years and with different telescopes have revealed vastly different things—at one time a pulsar and the other an X-ray binary," said Alessandro Papitto of the Institute of Space Sciences (Consejo Superior de Investigaciones Cientificas—Institut d'Estudis Espacials de Catalunya) in Barcelona, Spain, and lead author of a paper published in the journal Nature. "This was particularly intriguing because radio pulses don't come from an X-ray binary and the X-ray source has to be long gone before radio signals can emerge."

The answer to this puzzle was found in the complex interplay between the neutron star and its nearby companion.

Neutron star and its companion shown when the accretion has stopped and the neutron star is emitting radio pulses. Credit: Bill Saxton; NRAO/AUI/NSF

X-ray binaries, as their name implies, occur in a two-star system in which a neutron star is accompanied by a more normal, low-mass star. The smaller but considerably more massive neutron star can draw off material from its companion, forming a flattened disk of gas around the neutron star. Gradually, as this material swirls down to the surface of the neutron star, it becomes superheated and generates intense X-rays.

Astronomers believed that this process of accretion continued, mostly unabated, for millions of years. Eventually, the material would run out and the accretion would stop, along with the X-ray emission.

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A pulsar is a rapidly rotating neutron star that emits pulses of radiation (such as X-rays and radio waves) at regular intervals. A millisecond pulsar is one with a rotational period between one and 10 milliseconds, or from 60,000 to 6,000 revolutions per minute. Pulsars form in supernova explosions, but even newborn pulsars don't spin at millisecond speeds, and they gradually slow down with age. If, however, a pulsar is a member of a binary system with a normal star, gas transferred from the companion can spin up an old, slow pulsar to the millisecond range. This animation zooms into a neutron star and its accretion disk to show a millisecond pulsar in close-up. This animation zooms into a neutron star and its accretion disk to show a millisecond pulsar in close-up. Credit: NASA Scientific Visualization Studio

Without the influx of new material, the neutron star's powerful magnetic fields are able to generate beams of radio waves that sweep across space as the star rotates, giving the pulsar its characteristic lighthouse-like appearance.

Most radio pulsars rotate a few tens of times each second and—if left to their own devices—will slow down over many thousands of years. If the neutron star begins life as an X-ray binary, however, the matter accumulating on its surface causes the neutron star to "spin up," increasing its rate of rotation until it spins hundreds of times each second. When this accretion process stops, the result is a millisecond pulsar.

During their observations, the researchers detected outbursts of X-ray pulsations that went on for approximately one month and then abruptly stopped. Within a few days, the radio pulses once again emerged. These wild swings indicated that the material from the accretion disk was falling onto the neutron star in fits and starts, rather than in a long and constant stream as astronomers theorized.

An earlier study of another system with the GBT detected the first evidence of an accretion disk around a neutron star, which helped establish the link between low-mass X-ray binaries and pulsars.

The new data support this link but also show for the first time that the evolution process, which was thought to take perhaps millions of years, is actually more complex and can occur in episodic bursts that can last just a few days or weeks. "This not only demonstrates the evolutionary link between accretion and rotation-powered millisecond pulsars," said Ransom, "but also that some systems can swing between the two states on very short timescales."

The X-ray source was discovered by the International Gamma-Ray Astrophysics Laboratory (INTEGRAL) and follow-up X-ray observations were performed by the XMM-Newton, Swift, and Chandra satellites. Radio observations were made by the GBT, the Parkes radio telescope, the Australia Telescope Compact Array, and the Westerbork Synthesis Radio Telescope.

Explore further: Astronomers get new tools for gravitational-wave detection

More information: Paper: dx.doi.org/10.1038/nature12470

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1.5 / 5 (8) Sep 25, 2013
This would seem to be indicative of an oval shaped orbit of the secondary star around the primary one that is generating the radio and x-ray ways if it's going to keep switching back and forth. I guess those two would have to watched long term or on a regular basis to find out if that is the case.
5 / 5 (4) Sep 25, 2013
"This would seem to be indicative of an oval shaped orbit of the secondary star..."

Actually the eccentricity of the system derived from analysis of the x-ray lightcurve is nearly zero (i.e. circular).

As pointed out by the authors of the Nature paper, the radio output of the system is quenched when active accretion (and heightened x-ray emission) between the low-mass star and neutron star occurs. An early version of the paper in Nature is available here: http://arxiv.org/abs/1305.3884
1.5 / 5 (8) Sep 25, 2013
Thank you for the link. The article does a much better job of explaining what is going on.

1 / 5 (9) Sep 26, 2013
Perhaps the smaller neutron companion's normal response is to reject the dirty gas of the accretion ring by forcing it to the outer edges, allowing it to be a radio pulsar. Only when the dirty gas--metalized gas--is forced onto the neutron by the magnetic field of the larger companion does it become an an x-ray source.

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