A possible influence on standard model of quasars and active galactic nuclei in strong magnetic field
arXiv:1509.07726 · doi:10.1007/s10509-016-2977-8
Abstract
Recent observational evidence indicates that the center of our Milky Way harbours a super-massive object with ultra-strong radial magnetic field (Eatough et al., 2013). Here we demonstrate that the radiations observed in the vicinity of the Galactic Center (GC) (Falcke and Marko 2013) cannot be emitted by the gas of the accretion disk since the accreting plasma is prevented from approaching to the GC by the abnormally strong radial magnetic field. These fields obstruct the infalling accretion flow from the inner region of the disk and the central massive black hole in the standard model. It is expected that the observed radiations near the Galactic Center cannot be generated by the central black hole. We also demonstrate that the observed ultra-strong radial magnetic field near the Galactic Center ( Eatough et al., 2013) cannot be generated by the - turbulence dynamo mechanism of Parker since preliminary qualitative estimate in terms of this mechanism gives a magnetic field strength six orders of magnitude smaller than the observed field strength at . However, both these difficulties or the dilemma of the standard model can be overcome if the central black hole in the standard model is replaced by a supper-massive stellar object containing magnetic monopoles ( SMSOMM, Peng and Chou, 2001). The observed power peaking of the thermal radiation is essentially the same as our theoretical prediction. In addition, the discovery of the ultra-strong radial magnetic field near the Galactic Center can be naturally explained and is consistent with the prediction of our model( Peng and Chou 2001). Furthermore, the observed ultra-strong radial magnetic field in the vicinity of the Galactic Center may be considered as the astronomical evidence for the existence of magnetic monopoles as predicted by the Grand Unified Theory of particle physics.
11 pages, Accepted for publication in Astrophysics and Space Science. arXiv admin note: text overlap with arXiv:1404.0677 by other authors
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