PSR J1748−2446ad is the fastest-spinning pulsar known, at 716 Hz (times per second),[2] or 42,960 revolutions per minute. This pulsar was discovered by Jason W. T. Hessels of McGill University on November 10, 2004, and confirmed on January 8, 2005.
 The location of PSR J1748-2446ad in the night sky. The pulsar is located in the center of the yellow square. It is too faint in this image to be visible against the background. Credit: GALEX GR6/7 Data Release | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Sagittarius |
| Right ascension | 17h 48m 04.9s |
| Declination | −24° 46′ 04″ |
| Characteristics | |
| Spectral type | Pulsar |
| U−B color index | ? |
| B−V color index | ? |
| Variable type | None |
| Astrometry | |
| Distance | 18,000 Ly[1] |
| Details[2] | |
| Mass | <2 M☉ |
| Radius | <16 km |
| Rotation | 0.00139595482(6) s 716.35556(3) Hz |
| Age | ≥2.5×107 years |
| Database references | |
| SIMBAD | data |
If the neutron star is assumed to contain less than two times the mass of the Sun, within the typical range of neutron stars, its radius is constrained to be less than 16 km. At its equator it is spinning at approximately 24% of the speed of light, or over 70,000 km per second.
The pulsar is located in a globular cluster of stars called Terzan 5, located approximately 18,000 light-years from Earth in the constellation Sagittarius. It is part of a binary system and undergoes regular eclipses with an eclipse magnitude of about 40%. Its orbit is highly circular, with a 26-hour period. The other object in the system is at least 0.14 solar masses, with a radius of 5–6 solar radii. Hessels and collaborators state that the companion may be a "bloated main-sequence star, possibly still filling its Roche Lobe". Hessels and collaborators go on to speculate that gravitational radiation from the pulsar might be detectable by LIGO.[2]
See also
edit- PSR J0901–4046 longest period pulsar known
- PSR J0952–0607 second-fastest-spinning pulsar known
- NGC 6624, a globular cluster containing a neutron star spinning at possible the same velocity.
References
edit- ^ Ortolani, S.; Barbuy, B.; Bica, E.; Zoccali, M.; Renzini, A. (2007). "Distances of the bulge globular clusters Terzan 5, Liller 1, UKS 1, and Terzan 4 based on HST NICMOS photometry". Astronomy and Astrophysics. 470 (3): 1043–1049. arXiv:0705.4030. Bibcode:2007A&A...470.1043O. doi:10.1051/0004-6361:20066628. S2CID 18360940.
- ^ a b c Hessels, J. W. T.; Ransom, S. M.; Stairs, I. H.; Freire, P. C.; Kaspi, V. M.; Camilo, F. (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.