Millisecond pulsar

A millisecond pulsar (MSP) is a pulsar with a rotational period smaller than about 10 milliseconds. Millisecond pulsars have been detected in radio, X-ray, and gamma ray parts of the electromagnetic spectrum. The leading theory for the origin of millisecond pulsars is that they are old, rapidly rotating neutron stars that have been spun up or "recycled" through accretion of matter from a companion star in a close binary system.[1][2] For this reason, millisecond pulsars are sometimes called recycled pulsars.

Millisecond pulsars are thought to be related to low-mass X-ray binary systems. It is thought that the X-rays in these systems are emitted by the accretion disk of a neutron star produced by the outer layers of a companion star that has overflowed its Roche lobe. The transfer of angular momentum from this accretion event can theoretically increase the rotation rate of the pulsar to hundreds of times per second, as is observed in millisecond pulsars.

However, there has been recent evidence that the standard evolutionary model fails to explain the evolution of all millisecond pulsars, especially young millisecond pulsars with relatively high magnetic fields, e.g. PSR B1937+21. Bülent Kiziltan and S. E. Thorsett showed that different millisecond pulsars must form by at least two distinct processes.[3] But the nature of the other process remains a mystery.[4]
The stellar grouping Terzan 5

Many millisecond pulsars are found in globular clusters. This is consistent with the spin-up theory of their formation, as the extremely high stellar density of these clusters implies a much higher likelihood of a pulsar having (or capturing) a giant companion star. Currently there are approximately 130 millisecond pulsars known in globular clusters.[5] The globular cluster Terzan 5 alone contains 37 of these, followed by 47 Tucanae with 22 and M28 and M15 with 8 pulsars each.

Millisecond pulsars, which can be timed with high precision, have a stability comparable to atomic-clock-based time standards when averaged over decades.[6][7] This also makes them very sensitive probes of their environments. For example, anything placed in orbit around them causes periodic Doppler shifts in their pulses' arrival times on Earth, which can then be analyzed to reveal the presence of the companion and, with enough data, provide precise measurements of the orbit and the object's mass. The technique is so sensitive that even objects as small as asteroids can be detected if they happen to orbit a millisecond pulsar. The first confirmed exoplanets, discovered several years before the first detections of exoplanets around "normal" solar-like stars, were found in orbit around a millisecond pulsar, PSR B1257+12. These planets remained for many years the only Earth-mass objects known outside the Solar System. One of them, PSR B1257+12 D, has an even smaller mass, comparable to that of our Moon, and is still today the smallest-mass object known beyond the Solar System.[8]
Pulsar rotational speed limits

The first millisecond pulsar, PSR B1937+21, was discovered in 1982 by Backer et al.[9] Spinning roughly 641 times per second, it remains the second fastest-spinning millisecond pulsar of the approximately 200 that have been discovered.[10] Pulsar PSR J1748-2446ad, discovered in 2005, is, as of 2012, the fastest-spinning pulsar currently known, spinning 716 times per second.[11][12]

Current theories of neutron star structure and evolution predict that pulsars would break apart if they spun at a rate of c. 1500 rotations per second or more,[13][14] and that at a rate of above about 1000 rotations per second they would lose energy by gravitational radiation faster than the accretion process would speed them up.[15]

However, in early 2007 data from the Rossi X-ray Timing Explorer and INTEGRAL spacecraft discovered a neutron star XTE J1739-285 rotating at 1122 Hz.[16] The result is not statistically significant, with a significance level of only 3 sigma. Therefore, while it is an interesting candidate for further observations, current results are inconclusive. Still, it is believed that gravitational radiation plays a role in slowing the rate of rotation. Furthermore, one X-ray pulsar that spins at 599 revolutions per second, IGR J00291+5934, is a prime candidate for helping detect such waves in the future (most such X-ray pulsars only spin at around 300 rotations per second).
References

Bhattacharya & van den Heuvel (1991), "Formation and evolution of binary and millisecond radio pulsars", Physics Reports 203, 1
Tauris & van den Heuvel (2006), "Formation and evolution of compact stellar X-ray sources", In: Compact stellar X-ray sources. Edited by Walter Lewin & Michiel van der Klis. Cambridge Astrophysics Series, p.623-665, DOI: 10.2277/0521826594
Kızıltan, Bülent; Thorsett, S. E. (2009). "Constraints on Pulsar Evolution: The Joint Period-Spin-down Distribution of Millisecond Pulsars". The Astrophysical Journal Letters. 693 (2): L109–L112.arXiv:0902.0604. Bibcode:2009ApJ...693L.109K. doi:10.1088/0004-637X/693/2/L109. S2CID 2156395.
Naeye, Robert (2009). "Surprising Trove of Gamma-Ray Pulsars". Sky & Telescope.
Freire, Paulo. "Pulsars in globular clusters". Arecibo Observatory. Retrieved 2007-01-18.
Matsakis, D. N.; Taylor, J. H.; Eubanks, T. M. (1997). "A Statistic for Describing Pulsar and Clock Stabilities" (PDF). Astronomy and Astrophysics. 326: 924–928. Bibcode:1997A&A...326..924M. Retrieved 2010-04-03.
Hartnett, John G.; Luiten, Andre N. (2011-01-07). "Colloquium: Comparison of astrophysical and terrestrial frequency standards". Reviews of Modern Physics. 83 (1): 1–9.arXiv:1004.0115. doi:10.1103/revmodphys.83.1. ISSN 0034-6861. S2CID 118396798.
Rasio, Frederic (2011). "Planet Discovery near Pulsars". Science.
Backer, D. C.; Kulkarni, S. R.; Heiles, C.; Davis, M. M.; Goss, W. M. (1982), "A millisecond pulsar", Nature, 300 (5893): 615–618, Bibcode:1982Natur.300..615B, doi:10.1038/300615a0, S2CID 4247734
"The ATNF Pulsar Database". Retrieved 2009-05-17.
Hessels, Jason; Ransom, Scott M.; Stairs, Ingrid H.; Freire, Paulo C. C.; Kaspi, Victoria M.; Camilo, Fernando (2006). "A Radio Pulsar Spinning at 716 Hz". Science. 311 (5769): 1901–1904.arXiv:astro-ph/0601337. Bibcode:2006Sci...311.1901H. doi:10.1126/science.1123430. PMID 16410486. S2CID 14945340.
Naeye, Robert (2006-01-13). "Spinning Pulsar Smashes Record". Sky & Telescope. Archived from the original on 2007-12-29. Retrieved 2008-01-18.
Cook, G. B.; Shapiro, S. L.; Teukolsky, S. A. (1994). "Recycling Pulsars to Millisecond Periods in General Relativity". Astrophysical Journal Letters. 423: 117–120. Bibcode:1994ApJ...423L.117C. doi:10.1086/187250.
Haensel, P.; Lasota, J. P.; Zdunik, J. L. (1999). "On the minimum period of uniformly rotating neutron stars". Astronomy and Astrophysics. 344: 151–153. Bibcode:1999A&A...344..151H.
Chakrabarty, D.; Morgan, E. H.; Muno, M. P.; Galloway, D. K.; Wijnands, R.; van der Klis, M.; Markwardt, C. B. (2003). "Nuclear-powered millisecond pulsars and the maximum spin frequency of neutron stars". Nature. 424 (6944): 42–44.arXiv:astro-ph/0307029. Bibcode:2003Natur.424...42C. doi:10.1038/nature01732. PMID 12840751. S2CID 1938122.

Kiziltan, Bulent; Thorsett, Stephen E. (2007-02-19). "Integral points to the fastest spinning neutron star". Spaceflight Now. European Space Agency.arXiv:0902.0604. Bibcode:2009ApJ...693L.109K. doi:10.1088/0004-637X/693/2/L109. S2CID 2156395. Retrieved 2007-02-20.

External links

"Pinning Down a Pulsar's Age[permanent dead link]". Science News.
"How Millisecond Pulsars Spin So Fast". Universe Today.
"Fast-Spinning Star Could Test Gravitational Waves". New Scientist.
"Astronomical whirling dervishes hide their age well". Astronomy Now.
Audio: Cain/Gay - Pulsars Astronomy Cast - Nov 2009.

vte

Neutron star
Types

Radio-quiet Pulsar

Single pulsars

Magnetar
Soft gamma repeater Anomalous X-ray Rotating radio transient

Binary pulsars

Binary X-ray pulsar
X-ray binary X-ray burster List Millisecond Be/X-ray Spin-up

Properties

Blitzar
Fast radio burst Bondi accretion Chandrasekhar limit Gamma-ray burst Glitch Neutronium Neutron-star oscillation Optical Pulsar kick Quasi-periodic oscillation Relativistic Rp-process Starquake Timing noise Tolman–Oppenheimer–Volkoff limit Urca process