The Fractional Hydrogen Atom: A Paradigm for Astrophysical Phenomena

A. I. Arbab

Department of Physics, Faculty of Science, University of Khartoum, Khartoum, Sudan.

DOI: 10.4236/jmp.2012.311215                

Abstract

We have found that fractional principal quantum numbers are permitted in hydrogen atom which yield the conditions for neutron and white dwarf stars evolution. The number densities of neutron and white dwarf stars reveal that these systems have the maximal conductivity of 1.37×10¹⁰Ω^-1m^-1. They are giant perfect conductors at very high temperature and magnetic field.

Keywords

Hydrogen Atom; Fractional Quantum Number; Neutron Stars; White Dwarfs; Perfect Conductors

Conflicts of Interest

The authors declare no conflicts of interest.

References

[1]	S. Chandrasekhar, “The Density of White Dwarf Stars,” Philosophical Magazine, Vol. 11, No. 7, 1931, pp. 592- 596.
[2]	A. I. Arbab, “The Neutron Model,” The Hadronic Journal, Vol. 33, 2011, p. 695.
[3]	D. C. Tsui, H. L. Stormer and A. C. Gossard, “Two-Dimensional Magnetotransport in the Extreme Quantum Limit,” Physical Review Letters, Vol. 48, 1982, pp. 1559- 1562.
[4]	R. H. Fowler, “On Dense Matter,” Monthly Notices of the Royal Astronomical Society, Vol. 87, 1926, pp. 114-122.
[5]	G. Wunner, “Matter Under Extreme Conditions; Exotic QED Processes and Atoms in Strong External Fields,” Lecture Notes in Physics, Vol. 440, 1994, pp. 101-151.
[6]	C. C. Leiby, “The Fields of Pulsars and Magnetic White Dwarf Stars,” Astrophysics and Space Science, Vol. 122, No. 1, 1986, pp. 151.
[7]	J. D. Jackson, “Classical Electrodynamics,” 2nd Edition, John Wiley & Sons, New York, 1975.
[8]	A. C. Phillips, “The Physics of Stars,” 2nd Edition, Wiley, New York, 1999.
[9]	A. I. Arbab, “On the Electric and Magnetic Properties of Conductors,” Advanced Studies in Theoretical Physics, Vol. 5, No. 12, 2011, pp. 595-607.
[10]	D. Page, M. Prakash, J. M. Lattimer and A. W. Steiner, “Rapid Cooling of the Neutron Star in Cassiopeia A Triggered by Neutron Superfluidity in Dense Matter,” Physical Review Letters, Vol. 106, No. 8, 2011, pp. 081101-081104. doi:10.1103/PhysRevLett.106.081101
[11]	S. Jordan, “White Dwarfs,” Proceedings of the Royal Society A, Vol. 97, 1920, p. 374.
[12]	P. Fassbinder and W. Schweizer, “Stationary Hydrogen Lines in Magnetic and Electric Fields of White Dwarf Stars,” Astronomy & Astrophysics, Vol. 314, No. 2, 1996, pp. 700-706.
[13]	P. Drude, “Zur Elektronentheorie der metalle,” Annalen der Physik, Vol. 306, No. 3, 1900, pp. 566-613. doi:10.1002/andp.19003060312
[14]	S. T. Weir, A. C. Mitchell and W. J. Nellis, “Metallization of Fluid Molecular Hydrogen at 140 GPa,” Physical Review Letters, Vol. 76, No. 11, 1996, pp. 1860-1863.
[15]	N. G. Morawicz, K. W. J. Barnham and C. Zammit, “Observation of the Fractional Quantum Hall Effect under Hydrostatic Pressure,” Physical Review B, Vol. 41, No. 18, 1990, pp. 12687-12692. doi:10.1103/PhysRevB.41.12687
[16]	J. B. Holberg, M. A. Barstow, F. C. Bruhweiler, A. M. Cruise and A. J. Penny, “Sirius B: A New, More Accurate View,” The Astrophysical Journal, Vol. 497, No. 2, 1998, pp. 935-942. doi:10.1086/305489
[17]	J. Liebert, P. A. Young, D. Arnett, J. B. Holberg and K. A. Williams, “The Age and Progenitor Mass of Sirius B,” The Astrophysical Journal, Vol. 630, No. 1, 2005, pp. L69-L72. doi:10.1086/462419
[18]	W. Landsman, T. Simon and P. Bergeron, “The Hot White-Dwarf Companions of HR 1608, HR 8210, and HD 15638,” Astronomical Society of the Pacific, Vol. 105, No. 690, 1999, pp. 841-847. doi:10.1086/133242