General relativistic MHD simulations of non-thermal flaring in Sagittarius A*

This research was enabled by support provided by grant no. NSF PHY-1125915 along with a INCITE program award PHY129, using resources from the Oak Ridge Leadership Computing Facility, Summit, which is a DOE office of Science User Facility supported under contract DE-AC05- 00OR22725, and Calcul Quebec (http://www.calculquebec.ca) and Compute Canada (http://www.computecanada.ca). The authors acknowledge the Texas Advanced Computing Center (TACC) at The University of Texas at Austin for providing HPC and visualisation resources (allocation AST20011) that have contributed to the research results reported within this paper (http://www.tacc.utexas.edu). KC, SM and DY are supported by the Netherlands Organisation for Scientific Research (NWO) VICI grant (no. 639.043.513). K.C. is also supported by a Black Hole Initiative Fellowship at Harvard University, which is funded by grants from the Gordon and Betty Moore Foundation, John Templeton Foundation and the Black Hole PIRE program (NSF grant OISE1743747). The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the Moore or Templeton Foundations. ZY is supported by a UKRI Stephen Hawking Fellowship and acknowledges support from a Leverhulme Trust Early Career Fellowship, MvdK is supported by the NWO Spinoza Prize, AT by Northwestern University and by National Science Foundation grants AST-1815304, AST-1911080, and AI by a Royal Society University Research Fellowship. DH acknowledges support from the Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant, the Canada Research Chairs program, and the Canadian Institute for Advanced Research (CIFAR). This research has made use of NASA's Astrophysics Data System