| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Scutum |
| Right ascension | 18h 30m 47.75s |
| Declination | −10° 59′ 10.8″ |
| Distance | 10,000
ly (3,200 [1] pc) |
| Spectral type | Pulsar |
| Other designations | |
| Database references | |
| SIMBAD | data |
PSR B1828-11 (also known as PSR B1828-10 [2]) is a pulsar approximately 10,000 light-years away in the constellation of Scutum. The star exhibits variations in the timing and shape of its pulses: this was at one stage interpreted as due to a possible planetary system in orbit around the pulsar, though the model required an anomalously large second period derivative of the pulse times. [3] The planetary model was later discarded in favour of precession effects as the planets could not cause the observed shape variations of the pulses. [4] [5] While the generally accepted model is that the pulsar is a neutron star undergoing free precession, [6] a model has been proposed that interprets the pulsar as a quark star undergoing forced precession due to an orbiting "quark planet". [7] The entry for the pulsar on SIMBAD lists this hypothesis as being controversial. [2]
References
- ^ Smith, D. A.; Guillemot, L.; Camilo, F.; Cognard, I.; et al. (2008). "Pulsar timing for the Fermi gamma-ray space telescope". Astronomy and Astrophysics. 492 (3): 923–931. arXiv: 0810.1637. Bibcode: 2008A&A...492..923S. doi: 10.1051/0004-6361:200810285. S2CID 119200759.
- ^ a b "PSR B1828-10 -- Pulsar". SIMBAD. Retrieved 2014-07-02.
- ^ Bailes, M.; Lyne, A. G.; Shemar, S. L. (1993). "Limits on pulsar planetary systems from the Jodrell Bank timing database". Planets around pulsars; Proceedings of the Conference. California Inst. of Technology, Pasadena. pp. 19–30. Bibcode: 1993ASPC...36...19B.
- ^ Stairs, I. H.; Lyne, A. G.; Shemar, S. L. (2000). "Evidence for free precession in a pulsar". Nature. 406 (6795): 484–486. Bibcode: 2000Natur.406..484S. doi: 10.1038/35020010. PMID 10952302. S2CID 4415709.
- ^ Link, Bennett; Epstein, Richard I. (2001). "Precession Interpretation of the Isolated Pulsar PSR B1828-11". The Astrophysical Journal. 556 (1): 392–398. arXiv: astro-ph/0101434. Bibcode: 2001ApJ...556..392L. doi: 10.1086/321581. S2CID 118948361.
- ^ Akgün, Taner; Link, Bennett; Wasserman, Ira (2006). "Precession of the isolated neutron star PSR B1828-11". Monthly Notices of the Royal Astronomical Society. 365 (2): 653–672. arXiv: astro-ph/0506606. Bibcode: 2006MNRAS.365..653A. doi: 10.1111/j.1365-2966.2005.09745.x. S2CID 14390165.
- ^ Liu; et al. (2007). "PSR B1828-11: a precession pulsar torqued by a quark planet?". Monthly Notices of the Royal Astronomical Society: Letters. 381 (1): L1–L5. arXiv: astro-ph/0411133. Bibcode: 2007MNRAS.381L...1L. doi: 10.1111/j.1745-3933.2007.00337.x. S2CID 119405995.
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 | This variable star–related article is a stub. You can help Wikipedia by expanding it. |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Scutum |
| Right ascension | 18h 30m 47.75s |
| Declination | −10° 59′ 10.8″ |
| Distance | 10,000
ly (3,200 [1] pc) |
| Spectral type | Pulsar |
| Other designations | |
| Database references | |
| SIMBAD | data |
PSR B1828-11 (also known as PSR B1828-10 [2]) is a pulsar approximately 10,000 light-years away in the constellation of Scutum. The star exhibits variations in the timing and shape of its pulses: this was at one stage interpreted as due to a possible planetary system in orbit around the pulsar, though the model required an anomalously large second period derivative of the pulse times. [3] The planetary model was later discarded in favour of precession effects as the planets could not cause the observed shape variations of the pulses. [4] [5] While the generally accepted model is that the pulsar is a neutron star undergoing free precession, [6] a model has been proposed that interprets the pulsar as a quark star undergoing forced precession due to an orbiting "quark planet". [7] The entry for the pulsar on SIMBAD lists this hypothesis as being controversial. [2]
References
- ^ Smith, D. A.; Guillemot, L.; Camilo, F.; Cognard, I.; et al. (2008). "Pulsar timing for the Fermi gamma-ray space telescope". Astronomy and Astrophysics. 492 (3): 923–931. arXiv: 0810.1637. Bibcode: 2008A&A...492..923S. doi: 10.1051/0004-6361:200810285. S2CID 119200759.
- ^ a b "PSR B1828-10 -- Pulsar". SIMBAD. Retrieved 2014-07-02.
- ^ Bailes, M.; Lyne, A. G.; Shemar, S. L. (1993). "Limits on pulsar planetary systems from the Jodrell Bank timing database". Planets around pulsars; Proceedings of the Conference. California Inst. of Technology, Pasadena. pp. 19–30. Bibcode: 1993ASPC...36...19B.
- ^ Stairs, I. H.; Lyne, A. G.; Shemar, S. L. (2000). "Evidence for free precession in a pulsar". Nature. 406 (6795): 484–486. Bibcode: 2000Natur.406..484S. doi: 10.1038/35020010. PMID 10952302. S2CID 4415709.
- ^ Link, Bennett; Epstein, Richard I. (2001). "Precession Interpretation of the Isolated Pulsar PSR B1828-11". The Astrophysical Journal. 556 (1): 392–398. arXiv: astro-ph/0101434. Bibcode: 2001ApJ...556..392L. doi: 10.1086/321581. S2CID 118948361.
- ^ Akgün, Taner; Link, Bennett; Wasserman, Ira (2006). "Precession of the isolated neutron star PSR B1828-11". Monthly Notices of the Royal Astronomical Society. 365 (2): 653–672. arXiv: astro-ph/0506606. Bibcode: 2006MNRAS.365..653A. doi: 10.1111/j.1365-2966.2005.09745.x. S2CID 14390165.
- ^ Liu; et al. (2007). "PSR B1828-11: a precession pulsar torqued by a quark planet?". Monthly Notices of the Royal Astronomical Society: Letters. 381 (1): L1–L5. arXiv: astro-ph/0411133. Bibcode: 2007MNRAS.381L...1L. doi: 10.1111/j.1745-3933.2007.00337.x. S2CID 119405995.
| Stars |
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|---|---|---|---|---|---|---|---|
| |||||||
|
Star clusters |
| ||||||
| |||||||
|
| This variable star–related article is a stub. You can help Wikipedia by expanding it. |