Astronomy:PSR J0437-4715
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Pictor |
| Right ascension | 04h 37m 15.81476s[1] |
| Declination | −47° 15′ 08.6242″[1] |
| Characteristics | |
| Spectral type | Pulsar |
| Astrometry | |
| Proper motion (μ) | RA: 121.453 mas/yr Dec.: 71.457 mas/yr |
| Distance | 509.8 ly (156.3[2] pc) |
| Details | |
| Mass | 1.8[1] M☉ |
| Other designations | |
PSR B0435-47, 1RXS J043714.5-471503 | |
| Database references | |
| SIMBAD | data |
PSR J0437-4715 is a pulsar. Discovered in the Parkes 70 cm survey,[3] it remains the closest and brightest millisecond pulsar (MSP) known. The pulsar rotates about its axis 173.7 times per second and therefore completes a rotation every 5.75 milliseconds. It emits a searchlight-like radio beam that sweeps past the Earth each time it rotates. Currently the most precisely located object outside of the Solar System, PSR J0437-4715 is 156.3 parsecs or 509.8 light years distant.[2]
This pulsar is distinguished by being the most stable natural clock known and is debatably more stable than man-made atomic clocks.[4][5] Its stability is about one part in 1015. Two other pulsars, PSR B1855+09 and PSR B1937+21 are known to be comparable in stability to atomic clocks, or about 3 parts in 1014.
PSR J0437-4715 is the first MSP to have its X-ray emission detected and studied in detail.[6] It is also the first of only two pulsars to have the full three-dimensional orientation of its orbit determined.[7]
Optical observations indicate that the binary companion of PSR J0437-4715 is most likely a low-mass helium white dwarf.[8] The pulsar is about 1.8 solar mass (M☉) and the companion is about 0.25 M☉.[1] The pair revolve around each other every 5.75 days in nearly perfect circular orbits.[9]
See also
References
- ↑ 1.0 1.1 1.2 1.3 Verbiest, J. P. W.; Bailes, M.; van Straten, W.; Hobbs, G. B. et al. (2008). "Precision Timing of PSR J0437-4715: An Accurate Pulsar Distance, a High Pulsar Mass, and a Limit on the Variation of Newton's Gravitational Constant". The Astrophysical Journal 679: 675. doi:10.1086/529576. Bibcode: 2008ApJ...679..675V.
- ↑ 2.0 2.1 Deller, A. T.; Verbiest, J. P. W.; Tingay, S. J.; Bailes, M. (2008). "Extremely High Precision VLBI Astrometry of PSR J0437-4715 and Implications for Theories of Gravity". The Astrophysical Journal 685: L67. doi:10.1086/592401. Bibcode: 2008ApJ...685L..67D.
- ↑ Johnston, Simon; Lorimer, D. R.; Harrison, P. A.; Bailes, M.; Lynet, A. G.; Bell, J. F.; Kaspi, V. M.; Manchester, R. N. et al. (1993). "Discovery of a very bright, nearby binary millisecond pulsar". Nature 361 (6413): 613–615. doi:10.1038/361613a0. Bibcode: 1993Natur.361..613J.
- ↑ "Timing stability". http://relativity.livingreviews.org/Articles/lrr-2005-7/articlesu18.html#x25-370004.3.
- ↑ Hartnett, J. G.; Luiten, A. N. (2011). "Colloquium: Comparison of astrophysical and terrestrial frequency standards". Reviews of Modern Physics 83: 1. doi:10.1103/RevModPhys.83.1. Bibcode: 2011RvMP...83....1H.
- ↑ Becker, Werner; Trümper, Joachim (1993). "Detection of pulsed X-rays from the binary millisecond pulsar J0437 - 4715". Nature 365 (6446): 528. doi:10.1038/365528a0. Bibcode: 1993Natur.365..528B.
- ↑ Van Straten, W.; Bailes, M.; Britton, M.; Kulkarni, S. R. et al. (2001). "A test of general relativity from the three-dimensional orbital geometry of a binary pulsar". Nature 412 (6843): 158–160. doi:10.1038/35084015. PMID 11449265. Bibcode: 2001Natur.412..158V.
- ↑ Bell, J. F.; Bailes, M.; Bessell, M. S. (1993). "Optical detection of the companion of the millisecond pulsar J0437–4715". Nature 364 (6438): 603. doi:10.1038/364603a0. Bibcode: 1993Natur.364..603B.
- ↑ "Tables of Binary and Millisecond Pulsars". http://relativity.livingreviews.org/Articles/lrr-2005-7/articlese7.html.
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