PSR B0943+10 is a pulsar 2,000 light years from Earth[2] in the direction of the constellation of Leo.[4] It was discovered at Pushchino in December 1968, becoming the first pulsar discovered by Soviet astronomers.[5][6] The original designation of this pulsar was PP 0943.[1]
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Leo |
| Right ascension | 09h 46m 7.31s[1] |
| Declination | +09° 51′ 57.3″[1] |
| Astrometry | |
| Distance | 2,000 ly (630 ± 100[2] pc) |
| Characteristics | |
| Spectral type | Neutron star |
| Variable type | Pulsar |
| Details | |
| Mass | 1.5[3] M☉ |
| Luminosity | 1.31×10−5[2] L☉ |
| Temperature | 3.1×106[a][2] K |
| Rotation | 1.1 s[2] |
| Age | 5[b][2] Myr |
| Database references | |
| SIMBAD | data |
Characteristics
editThe pulsar is estimated to be 5 million years old, which is relatively old for a pulsar.[7] It has a rotational period of 1.1 seconds and emits both radio waves and X-rays.[8] Ongoing research at the University of Vermont discovered that the pulsar was found to flip roughly every few hours between a radio bright mode with highly organized pulsations and a quieter mode with rather chaotic temporal structure.[9][10]
Moreover, the observations of the pulsar performed simultaneously with the European Space Agency's XMM-Newton X-ray observatory and ground-based radio telescopes revealed that it exhibits variations in its X-ray emission that mimic in reverse the changes seen in radio waves – the pulsar has a weaker non-pulsing X-ray luminosity during the radio bright mode and is actually brighter during the radio quiet mode emitting distinct X-ray pulses.[10] Such changes can only be explained if the pulsar's magnetosphere (which may extend up to 52,000 km from the surface) quickly switches between two extreme states.[7] The change happens on a few seconds timescale, far faster than most pulsars. Despite being one of the first pulsars discovered, the mechanism for its unusual behavior is unknown.[9]
In 2006, a research group from Peking University published a paper suggesting that the pulsar may actually be a low-mass quark star with mass around 0.02 M☉.[11]
Planetary system
editIn May 2014, two gas giants were found orbiting PSR B0943+10.[12][3][13]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| b | 2.8 MJ | 1.8 | 730 | — | — | — |
| c | 2.6 MJ | 2.9 | 1,460 | — | — | — |
Notes
edit- ^ Blackbody temperature of a small emitting area at the poles
- ^ Characteristic age
References
edit- ^ a b c PSR B0943+10 -- Pulsar in SIMBAD
- ^ a b c d e f Zang, Bing; Sanwal, Divas & Pavlov, George G. (2005). "An XMM-Newton Observation of the Drifting Pulsar B0943+10". Astrophysical Journal. 624 (2): L109–L112. arXiv:astro-ph/0503423. Bibcode:2005ApJ...624L.109Z. doi:10.1086/430522. S2CID 119418646.
- ^ a b "The Extrasolar Planets Encyclopaedia Planet PSR B0943+10 c"
- ^ G.S. Mudur (25 January 2013). "Pune telescope spots Jekyll & Hyde puzzle in sky". The Telegraph, India. Archived from the original on February 16, 2013. Retrieved 31 January 2013.
- ^ Shklovsky, Iosif (1970). "Rozhdyonnye katastrofoi". In N. Lazarev; F. Naumov (eds.). Evrika-70 (in Russian). Moscow: Molodaya Gvardiya. p. 16.
- ^ Braude, S. Y.; et al., eds. (2012). A Brief History of Radio Astronomy in the USSR. A Collection of Scientific Essays. Astrophysics and Space Science Library. 382. Vol. 382. Springer. p. 45. doi:10.1007/978-94-007-2834-9. ISBN 978-94-007-2833-2.
- ^ a b ESA (25 January 2013). "Baffling pulsar leaves astronomers in the dark". Astronomy.com. Retrieved 31 January 2013.
- ^ Elizabeth Howell (24 January 2013). "Weird Spinning Star Defies Explanation". Space.com. Retrieved 31 January 2013.
- ^ a b Staff (24 January 2013). "Chameleon Pulsar Dramatically Changes the Way It Shines". Sciencedaily.com. Retrieved 31 January 2013.
- ^ a b Hermsen, W.; Hessels, J. W. T.; Kuiper, L.; Van Leeuwen, J.; Mitra, D.; De Plaa, J.; Rankin, J. M.; Stappers, B. W.; Wright, G. A. E.; Basu, R.; Alexov, A.; Coenen, T.; Grießmeier, J. - M.; Hassall, T. E.; Karastergiou, A.; Keane, E.; Kondratiev, V. I.; Kramer, M.; Kuniyoshi, M.; Noutsos, A.; Serylak, M.; Pilia, M.; Sobey, C.; Weltevrede, P.; Zagkouris, K.; Asgekar, A.; Avruch, I. M.; Batejat, F.; Bell, M. E.; Bell, M. R. (2013). "Synchronous X-ray and Radio Mode Switches: A Rapid Global Transformation of the Pulsar Magnetosphere". Science. 339 (6118): 436–439. arXiv:1302.0203. Bibcode:2013Sci...339..436H. doi:10.1126/science.1230960. PMID 23349288. S2CID 2460047.
- ^ Yue, Y. L.; Cui, X. H.; Xu, R. X. (2006). "Is PSR B0943+10 a low-mass quark star?". Astrophysical Journal. 649 (2): L95. arXiv:astro-ph/0603468v2. Bibcode:2006ApJ...649L..95Y. doi:10.1086/508421. S2CID 18183996.
- ^ Suleymanova, S. A.; Rodin, A. E. (2014). "Detection of regular variations in the intensity and pulse time of arrival of the anomalous pulsar PSR B0943+10". Astronomy Reports. 58 (11): 796–807. Bibcode:2014ARep...58..796S. doi:10.1134/S1063772914110067. S2CID 255196382.
- ^ "The Extrasolar Planets Encyclopaedia Planet PSR B0943+10 b"