MAGNETIZATION DEGREE AT THE JET BASE OF M87 DERIVED FROM THE EVENT HORIZON TELESCOPE DATA: TESTING THE MAGNETICALLY DRIVEN JET PARADIGM

We explore the degree of magnetization at the jet base of M87 by using the observational data of the event horizon telescope (EHT) at 230 GHz obtained by Doeleman et al. By utilizing the method in Kino et al., we derive the energy densities of magnetic fields (UB) and electrons and positrons (U±) in the compact region detected by EHT (EHT-region) with its full-width-half-maximum size 40 µas. First, we assume that an optically-thick region for synchrotron self absorption (SSA) exists in the EHT-region. Then, we find that the SSA-thick region should not be too large not to overproduce the Poynting power at the EHT-region. The allowed ranges of the angular size and the magnetic field strength of the SSA-thick region are 21 µas ≤ θthick ≤ 26.3 µas and 50 G ≤ Btot ≤ 124 G, respectively. Correspondingly UB ≫ U± is realized in this case. We further examine the composition of plasma and energy density of protons by utilizing the Faraday rotation measurement (RM) at 230 GHz obtained by Kuo et al. Then, we find that UB ≫ U± + Up still holds in the SSA-thick region. Second, we examine the case when EHT-region is fully SSA-thin. Then we find that UB ≫ U± still holds unless protons are relativistic. Thus, we conclude that magnetically driven jet scenario in M87 is viable in terms of energetics close to ISCO scale unless the EHT-region is fully SSA-thin and relativistic protons dominated. Subject headings: galaxies: active — galaxies: jets — radio continuum: galaxies —black hole physics —radiation mechanisms: non-thermal

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