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Parabolic Jets from the Spinning Black Hole in M87

Masanori NakamuraInstitute of Astronomy & Astrophysics, Academia Sinica, 11F of Astronomy-Mathematics Building, AS/NTU No. 1, Taipei 10617, Taiwan; [email protected]Keiichi AsadaInstitute of Astronomy & Astrophysics, Academia Sinica, 11F of Astronomy-Mathematics Building, AS/NTU No. 1, Taipei 10617, Taiwan; [email protected]Kazuhiro HadaMizusawa VLBI Observatory, National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, JapanHung-Yi PuInstitute of Astronomy & Astrophysics, Academia Sinica, 11F of Astronomy-Mathematics Building, AS/NTU No. 1, Taipei 10617, Taiwan; [email protected]Scott C. NobleDepartment of Physics and Engineering Physics, University of Tulsa, Tulsa, OK 74104, USAC.-Y. TsengDepartment of Physics, National Taiwan University, Taipei 10617, TaiwanKenji TomaAstronomical Institute, Tohoku University, Sendai 980-8578, JapanMotoki KinoKogakuin University of Technology & Engineering, Academic Support Center, 2665-1 Nakano, Hachioji, Tokyo 192-0015, JapanHiroshi NagaiNational Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, JapanKazuya TakahashiCenter for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, JapanJuan Carlos AlgabaDepartment of Physics and Astronomy, Seoul National University, 1 Gwanak-ro, Gwanak-gu, Seoul 08826, Republic of KoreaM. OrientiINAF-Istituto di Radio Astronomia, via P. Gobetti 101, I-40129 Bologna, ItalyKazunori AkiyamaMassachusetts Institute of Technology, Haystack Observatory, 99 Millstone Road, Westford, MA 01886, USAAkihiro DoiInstitute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuou-ku, Sagamihara, 252-5210, Kanagawa, JapanG. GiovanniniDipartimento di Fisica e Astronomia, Universita di Bologna, via Gobetti 93/2, I-40129 Bologna, ItalyM. GirolettiINAF-Istituto di Radio Astronomia, via P. Gobetti 101, I-40129 Bologna, ItalyMareki HonmaMizusawa VLBI Observatory, National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, JapanShoko KoyamaInstitute of Astronomy & Astrophysics, Academia Sinica, 11F of Astronomy-Mathematics Building, AS/NTU No. 1, Taipei 10617, Taiwan; [email protected]Rocco LicoDipartimento di Fisica e Astronomia, Universita di Bologna, via Gobetti 93/2, I-40129 Bologna, ItalyKotaro NiinumaGraduate School of Science and Engineering, Yamaguchi University, 753-8511, Yamaguchi, JapanFumie TazakiMizusawa VLBI Observatory, National Astronomical Observatory of Japan, Osawa, Mitaka, Tokyo 181-8588, Japan

2018en

ABI

Annotatsiya

Abstract The M87 jet is extensively examined by utilizing general relativistic magnetohydrodynamic (GRMHD) simulations, as well as the steady axisymmetric force-free electrodynamic (FFE) solution. Quasi-steady funnel jets are obtained in GRMHD simulations up to the scale of ∼100 gravitational radii ( r g ) for various black hole (BH) spins. As is known, the funnel edge is approximately determined by the following equipartitions: (i) the magnetic and rest-mass energy densities and (ii) the gas and magnetic pressures. Our numerical results give an additional factor that they follow the outermost parabolic streamline of the FFE solution, which is anchored to the event horizon on the equatorial plane. We also show that the matter-dominated, nonrelativistic corona/wind plays a dynamical role in shaping the funnel jet into the parabolic geometry. We confirm a quantitative overlap between the outermost parabolic streamline of the FFE jet and the edge of the jet sheath in very long baseline interferometry (VLBI) observations at ∼(10 1 –10 5 ) r g , suggesting that the M87 jet is likely powered by the spinning BH. Our GRMHD simulations also indicate a lateral stratification of the bulk acceleration (i.e., the spine-sheath structure), as well as an emergence of knotty superluminal features. The spin characterizes the location of the jet stagnation surface inside the funnel. We suggest that the limb-brightened feature could be associated with the nature of the BH-driven jet, if the Doppler beaming is a dominant factor. Our findings can be examined with (sub)millimeter VLBI observations, giving a clue for the origin of the M87 jet.

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DOI: 10.3847/1538-4357/aaeb2d

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