PSR B0329+54: Difference between revisions
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==Planetary system== |
==Planetary system== |
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In 1979, two [[extrasolar planet]]s were announced to be orbiting the pulsar (being classified as [[pulsar planet]]s). Later observations ruled out this idea.<ref name=mnras402_2_1027/><ref name=apj519_L81/><ref name=apj775_1/> However |
In 1979, two [[extrasolar planet]]s were announced to be orbiting the pulsar (being classified as [[pulsar planet]]s). Later observations ruled out this idea.<ref name=mnras402_2_1027/><ref name=apj519_L81/><ref name=apj775_1/> However, on October 3, 2017 the longest period exoplanet been confirmed.<ref name="arxiv.org">[https://arxiv.org/pdf/1710.01153.pdf "On The Existence of Planets Around the Pulsar PSR B0329+54".] E. D. Starovoit , and A. E. Rodin, (October 3, 2017).</ref> |
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| <ref>[https://arxiv.org/pdf/1710.01153.pdf "On The Existence of Planets Around the Pulsar PSR B0329+54".] E. D. Starovoit , and A. E. Rodin, (October 3rd of 2017).</ref> |
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==References== |
==References== |
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{{Stars of Camelopardalis}} |
{{Stars of Camelopardalis}} |
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Revision as of 10:49, 31 March 2019
| Observation data Epoch Equinox | |
|---|---|
| Constellation | Camelopardalis |
| Right ascension | 03h 32m 59.368s[1] |
| Declination | +54° 34′ 43.57″[1] |
| Distance | 3,460 ly (1,060 pc) |
| Spectral type | Pulsar |
| Other designations | |
| Database references | |
| SIMBAD | data |
PSR B0329+54 is a pulsar approximately 3,460 light-years away in the constellation of Camelopardalis. It completes one rotation every 0.71452[2] seconds and is approximately 5 million years old.[3]
The emissions of this pulsar and the Vela Pulsar were converted into audible sound by the French composer Gérard Grisey, and used as such in the piece Le noir de l'étoile (1989–90).[4][5][6]
Planetary system
In 1979, two extrasolar planets were announced to be orbiting the pulsar (being classified as pulsar planets). Later observations ruled out this idea.[7][3][8] However, on October 3, 2017 the longest period exoplanet been confirmed.[9]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (years) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 1.97 ± 0.19 M🜨 | 10.26 ± 0.07 | 27.76 ± 0.03 | 0.236 ± 0.011 | — | — |
See also
References
- ^ a b Cutri, R. M.; et al. (June 2003), 2MASS All Sky Catalog of point sources, NASA/IPAC, Bibcode:2003tmc..book.....C.
- ^ Konacki, Maciej; et al. (July 1999), "Are There Planets around the Pulsar PSR B0329+54?", The Astrophysical Journal, 519 (1): L81 – L84, Bibcode:1999ApJ...519L..81K, CiteSeerX 10.1.1.20.6608, doi:10.1086/312089.
- ^ a b Konacki, Maciej; et al. (July 1999), "Are There Planets around the Pulsar PSR B0329+54?", The Astrophysical Journal, 519 (1): L81 – L84, Bibcode:1999ApJ...519L..81K, doi:10.1086/312089.
- ^ Re, Giuseppe del. 2000. Cosmic Dance, pp. 24–25. Templeton Foundation Press, ISBN 9781890151256
- ^ Luminet, Jean-Pierre. 2011. Illuminations: Cosmos et esthétique, pp. 419–420. Odile Jacob, ISBN 9782738185938
- ^ "Le Noir de l'Étoile, Gérard Grisey". IRCAM. Retrieved 12 January 2016.
- ^ Hobbs, G.; Lyne, A. G.; Kramer, M. (February 2010), "An analysis of the timing irregularities for 366 pulsars", Monthly Notices of the Royal Astronomical Society, 402 (2): 1027–1048, arXiv:0912.4537, Bibcode:2010MNRAS.402.1027H, doi:10.1111/j.1365-2966.2009.15938.x.
- ^ Shabanova, T. V.; et al. (September 2013), "Timing Observations of 27 Pulsars at the Pushchino Observatory from 1978 to 2012", The Astrophysical Journal, 775 (1): 24, arXiv:1307.0297, Bibcode:2013ApJ...775....2S, doi:10.1088/0004-637X/775/1/2, 2.
- ^ "On The Existence of Planets Around the Pulsar PSR B0329+54". E. D. Starovoit , and A. E. Rodin, (October 3, 2017).
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