XTE J1739-285
XTE J1739−285 is a neutron star,[2] in the constellation Ophiuchus, situated approximately 39,000 light-years from Earth. It was first observed on 19 October 1999 by NASA's Rossi X-ray Timing Explorer satellite.
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Ophiuchus |
| Right ascension | 17h 39m 53.95s |
| Declination | −28° 29′ 46.8″ |
| Characteristics | |
| Spectral type | Q |
| Variable type | None |
| Astrometry | |
| Distance | 39,000 Ly |
| Details | |
| Mass | 1.51[1] M☉ |
| Radius | 10.9 km |
| Other designations | |
SWIFT J1740.6−2821B | |
| Database references | |
| SIMBAD | data |
It had previously been claimed that XTE J1739−285 was the fastest-spinning celestial body yet known, with a frequency of 1122 Hz.[3] However, a re-analysis of these data by other astronomers has been unable to reproduce this result.[4]
XTE J1739−285 has been proposed as a possible quark star, as well as 3C 58.
References
- Zhang, C. M; Yin, H. X; Zhao, Y. H; Wei, Y. C; Li, X. D (2007). "Does Submillisecond Pulsar XTE J1739−285 Contain a Weak Magnetic Neutron Star or Quark Star?". Publications of the Astronomical Society of the Pacific. 119 (860): 1108. arXiv:0708.3566. Bibcode:2007PASP..119.1108Z. doi:10.1086/522796.
- Low mass X-ray binary
- Evidence of 1122 Hz X-Ray Burst Oscillations from the Neutron Star X-Ray Transient XTE J1739–285
- See footnote 1 of Chakrabarty, D; Wijnands, Rudy; Altamirano, Diego; Soleri, Paolo; Degenaar, Nathalie; Rea, Nanda; Casella, Piergiorgio; Patruno, Alessandro; Linares, Manuel (2008). "The spin distribution of millisecond X-ray pulsars". American Institute of Physics Conference Series. 1068: 67. arXiv:0809.4031. Bibcode:2008AIPC.1068...67C. doi:10.1063/1.3031208.
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