Synchrotron and Inverse-Compton Signatures of Black to White Hole Explosions: Weibel-Mediated External Shocks in the Interstellar Medium
Hoang Van Quyet
arXiv:2608.12380v1 Announce Type: new
Abstract: We study the non-thermal electromagnetic counterpart expected when the relativistic, near-isotropic ejecta of a black-to-white hole transition sweep up the interstellar medium (ISM). Building on a photospheric model for the prompt $gamma$-ray emission~cite{Villani2026}, we parametrize the kinetic energy available for an external shock, $eiso=R_kegprompt$, and model the resulting collisionless forward shock with a Weibel-mediated field~cite{Weibel1959,MedvedevLoeb1999,SironiSpitkovsky2011}. We estimate the synchrotron and synchrotron self-Compton (SSC) emission from shock-accelerated electrons in a one-zone, Thomson-regime approximation, including inverse-Compton cooling, Klein-Nishina suppression, self-absorption, and $gamma$-$gamma$ opacity, all at order-of-magnitude or first-order accuracy. For illustrative parameters ($egpromptsim10^{44}$ erg, $R_k=0.1$, $Gamma_0=100$), the electrons are slow-cooling, so for $p=2.5arXiv:2608.12380v1 Announce Type: new
Abstract: We study the non-thermal electromagnetic counterpart expected when the relativistic, near-isotropic ejecta of a black-to-white hole transition sweep up the interstellar medium (ISM). Building on a photospheric model for the prompt $gamma$-ray emission~cite{Villani2026}, we parametrize the kinetic energy available for an external shock, $eiso=R_kegprompt$, and model the resulting collisionless forward shock with a Weibel-mediated field~cite{Weibel1959,MedvedevLoeb1999,SironiSpitkovsky2011}. We estimate the synchrotron and synchrotron self-Compton (SSC) emission from shock-accelerated electrons in a one-zone, Thomson-regime approximation, including inverse-Compton cooling, Klein-Nishina suppression, self-absorption, and $gamma$-$gamma$ opacity, all at order-of-magnitude or first-order accuracy. For illustrative parameters ($egpromptsim10^{44}$ erg, $R_k=0.1$, $Gamma_0=100$), the electrons are slow-cooling, so for $p=2.5

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