energy-momentum tensor allowed on the brane [@Shi-Mae-Sas:1999:]. The Randall-Sundrum model gives 4D Einstein gravity in low energies and the Newtonian limit appears on the 3-brane with high accuracy. Significant deviations from the Einstein gravity occur at very high energies, in the early universe and in vicinity of compact objects as black holes and neutron stars [@Maar:2004:].

Recently, no exact solution of the full 5D Einstein equations is know, but there is a variety of astrophysically plausible special solutions of the 4D effective Einstein equations constrained to the brane. Such solutions describe black holes with spherical symmetry [@Dad-Maar-Pap-Rez:2000:PHYSR4:] or with axial symmetry [@Ali-Gum:2005:] and compact objects that could represent neutron (quark) stars [@Ger-Maar:2001:]. The black hole spacetimes are determined by geometry of the spherical Reissner-Nordström (R-N) and axial Kerr-Newman (K-N) type where the electric charge squared is substituted by the braneworld “tidal charge” parameter representing the tidal (Weyl tensor) effects of the bulk space onto the 4D black hole structure. Astrophysically relevant properties of the braneworld black holes were studied in a series of papers devoted to both motion of matter in their vicinity [@Stu-Kot:2009:; @Ali-Tal:2009:; @Abdu-Ahme:2010:PHYSR4; @Mam-Hak-Toj:2010:MPLA:; @Mor-Ahme-Abdu-Mam:2010:ASS:] and optical phenomena [@Sche-Stu:2009:a; @Sche-Stu:2009:b; @Bin-Nun:2010:PHYSR4:a; @Bin-Nun:2010:PHYSR4:b].

In the simple model of 