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binary-pulsar

Binary pulsar

A binary pulsar is a pulsar with a binary companion, often another pulsar, white dwarf or neutron star. They are one of the few objects which allow physicists to test general relativity in the case of a strong gravitational field. Although the binary companion to the pulsar is usually difficult or impossible to observe, the timing of the pulses from the pulsar can be measured with extraordinary accuracy by radio telescopes. A relatively simple 10-parameter model incorporating information about the pulsar timing, the Keplerian orbits and three post-Keplerian corrections (the rate of periastron advance, a factor for gravitational redshift and a rate of change of the orbital period from gravitational radiation) is sufficient to completely model the pulsar timing. Binary pulsar timing has thus indirectly confirmed the existence of gravitational radiation and verified Einstein's general theory of relativity in a previously unknown regime.

The first binary pulsar, PSR 1913+16 or the "Hulse-Taylor binary pulsar" was discovered in 1974 at Arecibo by Joseph Hooton Taylor, Jr. and Russell Hulse, for which they won the 1993 Nobel Prize in Physics. Pulses from this system have been tracked, without glitches, to within 15 μs since its discovery.

Binary pulsars are one of the few tools scientists have to detect evidence of gravitational waves; Einstein’s theory of general relativity predicts that two neutron stars would emit gravitational waves as they orbit a common center of mass, which would carry away orbital energy and cause the two stars to draw closer together. As the two stellar bodies draw closer to one another, often a pulsar will absorb matter from the other causing a violent accretion process. This interaction can heat the gas being exchanged between the bodies and produce X-ray light which can appear to pulsate, causing binary pulsars to occasionally be referred to as X-ray binaries. This flow of matter from one stellar body to another is known as an accretion disk. Millisecond pulsars (or MSP's) create a sort of "wind", which in the case of binary pulsars can blow away the magnetosphere of the neutron stars and have a dramatic effect on the pulse emission. The 1993 Noble Prize was awarded to Joseph Taylor and Russell Hulse after they discovered two such stars. While Hulse was observing a new pulsar, named PSR 1913+16, he noticed that the frequency with which it pulsed fluctuated. It was concluded that the simplest explanation was that the pulsar was orbiting another star very closely at a high velocity. Hulse and Taylor determined that the stars were equally heavy by observing these pulse fluctuations, which led them to believe the other spacial object was also a neutron star.

The observations made of the orbital decay of this star system was a near perfect match to Einstein’s equations. Relativity predicts that over time a binary system’s orbital energy will be converted to gravitational radiation. Data collected by Taylor and his colleagues of the orbital period of PRS 1913+16 supported this relativistic prediction; they reported in 1983 that there was a difference in the observed minimum separation of the two pulsars compared to that expected if the orbital separation had remained constant. In the decade following its discovery the system’s orbital period had decreased by about 76 millionths of a second per year-this means that the pulsar was approaching its maximum separation more than a second earlier than it would have if the orbit had remained the same (Haynes 2007). Subsequent observations continue to show this decrease.

The study of binary pulsars also led to the first accurate determination of neutron star masses, using relativistic timing effects. Scientists can find the radial velocity of a pulsar as it moves through its orbit by observing the number of pulses received each second. As a pulsar is moving towards us, the pulses will be more frequent and the pulse repetition rate will be its highest. Conversely, as it moves away from us the pulses will be more spread out, and fewer will be detected in a given time period. One can think of the pulses like the ticks of a clock; changes in the ticking are indications of changes in time due to these relativistic changes. When the two bodies are in close proximity, the gravitational field is stronger, the passage of time is slowed–and the time between pluses (or ticks) is lengthened. As the pulsar clock travels more slowly through the weakest part of the field it regains time. This relativistic time delay is the difference between what one would expect to see if the pulsar were moving at a constant distance and speed around it companion in a circular orbit, and what is actually observed (Haynes 2007).

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