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Magnetars by condensed matter physics

5th International Conference on Theoretical, Materials and Condensed Matter Physics

November 26-28, 2018 | Los Angeles, USA

Qiu-he Peng

Nanjing University, China

Keynote: Res. Rev. J Mat. Sci

DOI: 10.4172/2321-6212-C10-040


1. We present the microscopic origin of the super-strong magnetic fields in magnetars. The ultra-strong magnetic field of the magnetars originates really from the induced paramagnetic moment of the 3P2 superfluid with a significant mass more than 0.1m⊙ in a condition when their interior temperature here is the energy gap of the neutron 3P2 Cooper pairs. In the case, a phase transition from paramagnetism to ferromagnetism due to the induced paramagnetic moment of 3P2 Cooper pairs in the presence of background magnetic field. The upper limit of the magnetic field for the magnetars is 2. We find that the electron Fermi energy, Ef(e), increases with the magnetic field strength and it is proportional to B1/4 under the super strong magnetic field. We note that this result is exactly the opposite of the popular idea that the electron Fermi energy decreases with the magnetic field. The key reason for the dilemma is that an incorrect formulae of the microscopic number of states for the electrons in the intense magnetic field from some internationally well known popular textbooks on statistical physics has been repeatedly quoted by many authors. An important inference from our idea is the direct Urca process is permitted in the magnetars. 3. We propose a new mechanism for the production of the high soft X-ray luminosities of magnetars. In particular, the Fermi energy of the electrons is higher than 60MeV in ultra-strong magnetic fields, B>>Bcr (=4.414×1013 gauss), which is much higher than the Fermi energy of the neutrons. In this case, the process of electron capture (EC) by protons around the proton Femi surface would dominate in magnetars. The outgoing high-energy neutrons due to EC process can easily destroy the 3P2 Cooper pairs through the nuclear strong interaction. When one Cooper pair is destroyed, the orderly magnetic energy 2μn B would be released and transformed into disorder thermal energy, then it may be radiated as soft X-rays. The Energy is in the X-ray range. The total magnetic energy of 3P2 Cooper pairs can be estimated as 1.0×1047B15(m(3P2)/0.1m⊙)ergs. This energy can maintain over 104−6 yrs for LX ≈ 1034-1036 ergs/s. We have also calculated the theoretical luminosities of magnetars, and our results compared very well with observations of magnetars.


Qiu-he Peng graduated from Department of Astronomy, Nanjing University at 1960 firstly taught at Peking University for 18 years and then is teaching at Nanjing University. He is mainly engaged in nuclear astrophysics, particle astrophysics, and galactic astronomy research. In the field of nuclear astrophysics, his researches involve neutron stars (pulsars), the supernova explosion mechanism and the thermonuclear reaction inside the star, the synthesis of heavy elements and an interstellar radioactive element such as the origin of celestial 26Al. 225 papers of him have been published.

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