American Journal of Astronomy and Astrophysics
Volume 6, Issue 3, September 2018, Pages: 91-96
Received: Oct. 11, 2018;
Accepted: Nov. 2, 2018;
Published: Nov. 29, 2018
Views 290 Downloads 127
Cuixiang Zhong, Department of Physics, Jiangxi Normal University, Nanchang, China
The discovery of pulsar is an exciting discovery in 1960s, it has a profound influence on the development of modern physics. Although after the discovery of the first pulsar, it is quickly confirmed that pulsars are rapidly rotating neutron stars, yet people knew little about the essential mechanism leading neutron stars to pulse electromagnetic radiation. Thus, the author has analyzed the morphology and atmospheric environment of neutron stars, and found that a neutron star usually has two vortex structures located at its South pole and North pole, consisting of two groups of parallel spiral cloud paths, therefore producing two groups of corresponding dipole magnetic fields located at the South pole and the North pole respectively. It is the superposition of these two groups of dipole magnetic fields with the same polarity that form the neutron star’s magnetic field continuously giving off radio and X-ray pulsations in lighthouse-like beams. Since the atmospheric vortexes on the planets of the Solar System are tiny accretion disks, and the accretion disks on neutron stars, black holes or active galactic nuclei are essentially large-scale atmospheric vortexes, neutron star’s vortex-formation mechanism and electromagnetic radiation mechanism can be extended to the accretion and jets of black holes.
Formation and Evolution of Pulsars & Accretion and Jets of Black Holes, American Journal of Astronomy and Astrophysics.
Vol. 6, No. 3,
2018, pp. 91-96.
Copyright © 2018 Authors retain the copyright of this article.
This article is an open access article distributed under the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/
) which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
Bell Burnell, S. Jocelyn. Little Green Men, White Dwarfs, or Pulsars? Annals of the New York Academy of Science, vol. 302, pages 685–689, Dec., 1977.
Bell Burnell, S. Jocelyn (23 April 2004). So Few Pulsars, So Few Females . Science. 304 (5670): 489.
Gold, T. (1968). "Rotating Neutron Stars as the Origin of the Pulsating Radio Sources". Nature. 218 (5143): 731.
Deneva, J. S.; Cordes, J. M.; Lazio, T. J. W. (2009). Discovery of Three Pulsars from a Galactic Center Pulsar Population. The Astrophysical Journal Letters. 702 (2): L177–182.
D. Backer; Kulkarni, Shrinivas R.; Heiles, Carl; Davis, M. M.; Goss, W. M. (1982). A millisecond pulsar. Nature. 300 (5893): 315–318.
Matsakis, D. N.; Taylor, J. H.; Eubanks, T. M. (1997). A Statistic for Describing Pulsar and Clock Stabilities. Astronomy and Astrophysics. 326: 924–928.
Pacini, F. (1967). Energy Emission from a Neutron Star. Nature. 216 (5115): 567.
Young, M. D.; Manchester, R. N.; Johnston, S. (1999). A Radio Pulsar with an 8.5-Second Period that Challenges Emission Models. Nature. 400 (6747): 848–849.
Lyne, Andrew G.; Graham-Smith, Francis. Pulsar Astronomy. Cambridge University Press, 1998.
Arcavi, Iair; et al. (2017). Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star. Nature. 551 (7679): 210
Cho, A. (16 February 2018). A weight limit emerges for neutron stars. Science. 359 (6377): 724–725.
Margalit, B.; Metzger, B. D. (2017-12-01). Constraining the Maximum Mass of Neutron Stars from Multi-messenger Observations of GW170817. The Astrophysical Journal. 850 (2): L19.
Ruiz, M.; Shapiro, S. L.; Tsokaros, A. (2018-01-11). GW170817, general relativistic magnetohydrodynamic simulations, and the neutron star maximum mass. Physical Review D. 97 (2): 021501.
Gurzadyan, V. G.; Ozernoy, L. M. (1979). Accretion on massive black holes in galactic nuclei. Nature. 280.
Floyd, David J. E.; Bate, N. F.; Webster, R. L. (2009). The accretion disc in the quasar SDSS J0924+0219. Monthly Notices of the Royal Astronomical Society. 398 (1): 233–239.
Beckwith, K.; Hawley, J. F.; Krolik, J. H. (2009). Transport of large-scale poloidal flux in black hole accretion. Astrophysical Journal. 707 (1): 428–445.
Poindexter, Shawn; Morgan, Nicholas; Kochanek, Christopher S. (2008). The Spatial Structure of An Accretion Disk. The Astrophysical Journal. 673 (1): 34–38.
Beckwith, K.; Hawley, J. F.; Krolik, J. H. (2009). TRANSPORT OF LARGE-SCALE POLOIDAL FLUX IN BLACK HOLE ACCRETION (PDF). Astrophysical Journal. 707 (1): 428–445.
Daniel Clery. (2014). What powers a black hole's mighty jets? . Science | AAAS. Nov. 19, 2014.
Johnson, M. D.; Fish, V. L.; Doeleman, S. S.; Marrone, D. P.; Plambeck, R. L.; Wardle, J. F. C.; Akiyama, K.; Asada, K.; Beaudoin, C. (4 December 2015). Resolved magnetic-field structure and variability near the event horizon of Sagittarius A*. Science. 350 (6265): 1242–1245.