A Universal Power-law Prescription for Variability from Synthetic Images of Black Hole Accretion Flows
Koch PM; Rygl KLJ; Heumann D; Lonsdale CJ; Trent T; Sanchez-Portal M; Kim DJ; Neri R; Ruszczyk C; Yuan F; Janssen M; Wagner J; Ward-Thompson D; Huang CWL; Cruz-Osorio A; Lisakov M; Ramakrishnan V; Yamaguchi P; Sasada M; Nadolski A; Mizuno Y; Gurwell M; Cui YZ; Ruiz I; Sanchez-Arguelles D; Nagar NM; SooHoo J; Natarajan I; Nakamura M; Preciado-Lopez JA; Keating GK; Kim J; Moran JM; Ball D; Small D; Gomez JL; Emami R; Matthews LD; Asada K; Jannuzi BT; Ho LC; Shao LJ; Traianou E; Lehner L; Broderick AE; Loinard L; Michalik D; Fomalont E; Brinkerink CD; Jiang W; Hughes DH; James DJ; Chatterjee S; Liu J; Deane R; Chan CK; Trippe S; Prather B; Savolainen T; Gomez-Ruiz AI; Kramer C; Bintley D; Eatough RP; Cordes JM; Titus M; Muller C; Dzib SA; Fromm CM; Kim JY; Qiu R; Sun H; Brissenden R; Wiik K; Bouman KL; Lauer TR; Rottmann H; Vos J; Schloerb FP; Dougal S; Okino H; Myserlis I; Alef W; Fuentes A; Pesce DW; Lindqvist M; Boyce H; Schuster KF; Ripperda B; Ni CC; Karami M; Ortiz-Leon GN; Zhao GY; Fraga-Encinas R; Witzel G; Yoon D; Gu MF; Britzen S; De Laurentis M; Ricarte A; Pu HY; Ros E; Ikeda S; Musoke G; Karuppusamy R; Matsushita S; Fish VL; Conway JE; Inoue M; Impellizzeri CMV; Anantua R; Cho I; Oyama T; Weintroub J; Leung PK; Torne P; Akiyama K; Oh J; Patel N; Johnson MD; Koyama S; Turk M; Falcke H; Christian P; Tiede P; Doeleman SS; Mus A; Barrett J; Wondrak MF; Kawashima T; Fuentes SN; Bach U; Rezzolla L; Lo WP; Lu RS; Kramer M; Nowak MA; Kino M; Narayanan G; Algaba JC; Crawford TM; Desvignes G; Koay JY; Zensus JA; Neilsen J; Park J; Dexter J; Markoff S; Wong GN; Souccar K; Young A; Conroy NS; Baczko AK; Dempsey J; Kuo CY; Zhao SS; Levis A; Freeman WT; Hada K; Potzl FM; Wardle J; van Rossum DR; Schonfeld J; Krichbaum TP; van Langevelde HJ; Narayan R; PopStefanija A; Palumbo DCM; Gentaz O; Carlstrom JE; Yuan YF; Pen UL; La Bella N; Rogers A; Roelofs F; van Bemmel I; Nathanail A; Huang L; Joshi AV; Jimenez-Rosales A; Marscher AP; Blackburn L; Shen ZQ; Galison P; Chatterjee K; Hesper R; Satapathy K; Chen YJ; Roshanineshat A; Sanchez S; Mizuno I; Davelaar J; Rao R; Parsons H; Farah J; Rawlings MG; Lee SS; Kofuji Y; Roy AL; Goddi C; Wielgus M; Raymond AW; Ford HA; Lee D; Tetarenko AJ; Marchili N; Jeter B; Sohn BW; Kocherlakota P; Friberg P; Gammie CF; Chen MT; Lindahl G; Marti-Vidal I; Lobanov AP; Marrone DP; Byun DY; Baubock M; Mao JR; Olivares H; Noutsos A; Haggard D; Tilanus RPJ; Azulay R; Moscibrodzka M; Crew GB; Zhang S; Cheng XP; Moriyama K; Younsi Z; Hecht MH; Ceccobello C; Ho P; Blundell R; Menten KM; Broguiere D; Gold R; Wu QW; Chael A; Benson BA; Lico R; Liuzzo E; Garcia R; Bronzwaer T; Balokovic M; Paraschos GF; Porth O; Tazaki F; Nagai H; Georgiev B; Haworth K; Plambeck R; Bustamante S; Bremer M; Dhruv V; Li ZY; Jorstad S; Kettenis M; Jung T; Romero-Canizales C; Wharton R; Alberdi A; Honma M; Bower GC; Young K; Wex N; Liu K; Pietu V; Issaoun S
https://urn.fi/URN:NBN:fi-fe2022081154631
Tiivistelmä
We present a framework for characterizing the spatiotemporal power spectrum of the variability expected from the horizon-scale emission structure around supermassive black holes, and we apply this framework to a library of general relativistic magnetohydrodynamic (GRMHD) simulations and associated general relativistic ray-traced images relevant for Event Horizon Telescope (EHT) observations of Sgr A*. We find that the variability power spectrum is generically a red-noise process in both the temporal and spatial dimensions, with the peak in power occurring on the longest timescales and largest spatial scales. When both the time-averaged source structure and the spatially integrated light-curve variability are removed, the residual power spectrum exhibits a universal broken power-law behavior. On small spatial frequencies, the residual power spectrum rises as the square of the spatial frequency and is proportional to the variance in the centroid of emission. Beyond some peak in variability power, the residual power spectrum falls as that of the time-averaged source structure, which is similar across simulations; this behavior can be naturally explained if the variability arises from a multiplicative random field that has a steeper high-frequency power-law index than that of the time-averaged source structure. We briefly explore the ability of power spectral variability studies to constrain physical parameters relevant for the GRMHD simulations, which can be scaled to provide predictions for black holes in a range of systems in the optically thin regime. We present specific expectations for the behavior of the M87* and Sgr A* accretion flows as observed by the EHT.
Kokoelmat
- Rinnakkaistallenteet [19207]