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Physical constraints on the Maldacena-Shenker-Stanford chaos bound in black hole spacetimes

Terkaa Victor Targema1,2,*, Kazuharu Bamba1,†, Riasat Ali3,‡, and Usman Zafar1,§

  • *Contact author: s2571502@ipc.fukushima-u.ac.jp
  • †Contact author: bamba@sss.fukushima-u.ac.jp
  • ‡Contact author: riasatyasin@gmail.com
  • §Contact author: s2471001@ipc.fukushima-u.ac.jp
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Phys. Rev. D 113, 104056 – Published 26 May, 2026

DOI: https://doi.org/10.1103/s39h-mlcs

Abstract

Chaotic motion near black holes has recently been examined through the lens of the Maldacena-Shenker-Stanford (MSS) chaos bound, but reported violations remain contradictory. A significant source of ambiguity stems from treating the particle angular momentum as an independently adjustable parameter instead of as a quantity fixed by the circular-orbit conditions. We develop a constrained framework in which the angular momentum is determined self-consistently from the geometry. Applied to the charged Kiselev black hole, this framework shows that certain previously reported violations of the chaos bound can be attributed to inconsistent parameter choices rather than to intrinsic curvature effects. By extending the analysis to geometries containing higher-order curvature terms, we find genuine chaos-bound violations at large charge-to-mass ratios, originating from curvature corrections rather than orbital parameters. Our approach, therefore, provides a systematic means to distinguish between parameter-induced (apparent) and curvature-induced (physical) violations in Einstein gravity and its extensions.

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Phys. Rev. D 113, 104056– Published 26 May, 2026
  • Received 1 January 2026
  • Accepted 8 April 2026
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Published by the American Physical Society under the terms of the Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article’s title, journal citation, and DOI. Funded by SCOAP3.

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