@article{discovery10204538,
          volume = {693},
           title = {The persistent shadow of the supermassive black hole of M87:
II. Model comparisons and theoretical interpretations},
            note = {Copyright {\copyright} The Authors 2025.
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
This article is published in open access under the Subscribe to Open model. Subscribe to A\&A to support open access publication.},
           month = {January},
            year = {2025},
         journal = {Astronomy and Astrophysics (A\&A)},
       publisher = {EDP Sciences},
        keywords = {Accretion, accretion disks / black hole physics / gravitation / galaxies: active / galaxies: individual: M87 / galaxies: jets},
        abstract = {The Event Horizon Telescope (EHT) observation of M87? in 2018 has revealed a ring with a diameter that is consistent with the 2017 observation. The brightest part of the ring is shifted to the southwest from the southeast. In this paper, we provide theoretical interpretations for the multi-epoch EHT observations for M87? by comparing a new general relativistic magnetohydrodynamics model image library with the EHT observations for M87? in both 2017 and 2018. The model images include aligned and tilted accretion with parameterized thermal and nonthermal synchrotron emission properties. The 2018 observation again shows that the spin vector of the M87? supermassive black hole is pointed away from Earth. A shift of the brightest part of the ring during the multi-epoch observations can naturally be explained by the turbulent nature of black hole accretion, which is supported by the fact that the more turbulent retrograde models can explain the multi-epoch observations better than the prograde models. The EHT data are inconsistent with the tilted models in our model image library. Assuming that the black hole spin axis and its large-scale jet direction are roughly aligned, we expect the brightest part of the ring to be most commonly observed 90 deg clockwise from the forward jet. This prediction can be statistically tested through future observations.},
             url = {https://doi.org/10.1051/0004-6361/202451296},
            issn = {0004-6361},
          author = {Akiyama, K and Albentosa-Ru{\'i}z, E and Alberdi, A and Alef, W and Algaba, JC and Anantua, R and Asada, K and Azulay, R and Bach, U and Baczko, AK and Ball, D and Balokovi{\'c}, M and Bandyopadhyay, B and Barrett, J and Baub{\"o}ck, M and Benson, BA and Bintley, D and Blackburn, L and Blundell, R and Bouman, KL and Bower, GC and Bremer, M and Brissenden, R and Britzen, S and Broderick, AE and Broguiere, D and Bronzwaer, T and Bustamante, S and Carlstrom, JE and Chael, A and Chan, CK and Chang, DO and Chatterjee, K and Chatterjee, S and Chen, MT and Chen, Y and Cheng, X and Cho, I and Christian, P and Conroy, NS and Conway, JE and Crawford, TM and Crew, GB and Cruz-Osorio, A and Cui, Y and Curd, B and Dahale, R and Davelaar, J and De Laurentis, M and Deane, R and Dempsey, J and Desvignes, G and Dexter, J and Dhruv, V and Dihingia, IK and Doeleman, SS and Dzib, SA and Eatough, RP and Emami, R and Falcke, H and Farah, J and Fish, VL and Fomalont, E and Ford, HA and Foschi, M and Fraga-Encinas, R and Freeman, WT and Friberg, P and Fromm, CM and Fuentes, A and Galison, P and Gammie, CF and Garc{\'i}a, R and Gentaz, O and Georgiev, B and Goddi, C and Gold, R and G{\'o}mez-Ruiz, AI and G{\'o}mez, JL and Gu, M and Gurwell, M and Hada, K and Haggard, D and Hesper, R and Heumann, D and Ho, LC and Ho, P and Honma, M and Huang, CWL and Huang, L and Hughes, DH and Ikeda, S and Impellizzeri, CMV and Inoue, M and Issaoun, S and James, DJ and Jannuzi, BT and Janssen, M and Jeter, B and Jiang, W}
}