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Synchrotron and Inverse-Compton Signatures of Black to White Hole Explosions: Weibel-Mediated External Shocks in the Interstellar Medium
High Energy Astrophysical Phenomena · Submitted 28 Jul 2026
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We identify parameter regions where a 1 keV photon-count estimate, below the intrinsic peak, exceeds a nominal detection threshold, and discuss features -- a fast, faint, roughly isotropic transient after a hard-spectrum prompt flash, without an achromatic jet break -- that may distinguish this scenario from short GRBs, magnetar giant flares, and other fast transients, while flagging the assumptions (forward-shock-only dynamics, one-zone Thomson-regime radiation, an illustrative detectability criterion) limiting its quantitative reach.
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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, $\eiso=R_k\egprompt$, 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 ($\egprompt\sim10^{44}$ erg, $R_k=0.1$, $\Gamma_0=100$), the electrons are slow-cooling, so for $p=2.5<3$ the synchrotron spectrum peaks at the cooling frequency $\nu_c$, in the MeV-to-GeV range and softening with time; the afterglow evolves in a fraction of a second to tens of seconds -- orders of magnitude faster than a classical long-duration GRB afterglow at comparable energy, density, and Lorentz factor -- with duration, peak energy, and flux depending sensitively on $R_k$, $\nism$, and $\epse,\epsB,\xie$. We identify parameter regions where a 1 keV photon-count estimate, below the intrinsic peak, exceeds a nominal detection threshold, and discuss features -- a fast, faint, roughly isotropic transient after a hard-spectrum prompt flash, without an achromatic jet break -- that may distinguish this scenario from short GRBs, magnetar giant flares, and other fast transients, while flagging the assumptions (forward-shock-only dynamics, one-zone Thomson-regime radiation, an illustrative detectability criterion) limiting its quantitative reach.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | 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). | contribution 0.98 | 0.59 | 0.06 | asserted 0.73 |
| s1 | Building on a photospheric model for the prompt $\gamma$-ray emission~\cite{Villani2026}, we parametrize the kinetic energy available for an external shock, $\eiso=R_k\egprompt$, and model the resulting collisionless forward shock with a Weibel-mediated field~\cite{Weibel1959,MedvedevLoeb1999,SironiSpitkovsky2011}. | method 0.99 | 0.84 | 0.04 | asserted 0.96 |
| s2 | 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. | method 0.99 | 0.90 | 0.06 | asserted 0.98 |
| s3 | For illustrative parameters ($\egprompt\sim10^{44}$ erg, $R_k=0.1$, $\Gamma_0=100$), the electrons are slow-cooling, so for $p=2.5<3$ the synchrotron spectrum peaks at the cooling frequency $\nu_c$, in the MeV-to-GeV range and softening with time; the afterglow evolves in a fraction of a second to tens of seconds -- orders of magnitude faster than a classical long-duration GRB afterglow at comparable energy, density, and Lorentz factor -- with duration, peak energy, and flux depending sensitively on $R_k$, $\nism$, and $\epse,\epsB,\xie$. | result 1.00 | 0.89 | 0.36 | asserted 0.99 |
| s4 | We identify parameter regions where a 1 keV photon-count estimate, below the intrinsic peak, exceeds a nominal detection threshold, and discuss features -- a fast, faint, roughly isotropic transient after a hard-spectrum prompt flash, without an achromatic jet break -- that may distinguish this scenario from short GRBs, magnetar giant flares, and other fast transients, while flagging the assumptions (forward-shock-only dynamics, one-zone Thomson-regime radiation, an illustrative detectability criterion) limiting its quantitative reach. | interpretation 0.52 | 0.92 | 0.61 | hedged possibility 0.98 |
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The paper
Original 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, $\eiso=R_k\egprompt$, 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 ($\egprompt\sim10^{44}$ erg, $R_k=0.1$, $\Gamma_0=100$), the electrons are slow-cooling, so for $p=2.5<3$ the synchrotron spectrum peaks at the cooling frequency $\nu_c$, in the MeV-to-GeV range and softening with time; the afterglow evolves in a fraction of a second to tens of seconds -- orders of magnitude faster than a classical long-duration GRB afterglow at comparable energy, density, and Lorentz factor -- with duration, peak energy, and flux depending sensitively on $R_k$, $\nism$, and $\epse,\epsB,\xie$. We identify parameter regions where a 1 keV photon-count estimate, below the intrinsic peak, exceeds a nominal detection threshold, and discuss features -- a fast, faint, roughly isotropic transient after a hard-spectrum prompt flash, without an achromatic jet break -- that may distinguish this scenario from short GRBs, magnetar giant flares, and other fast transients, while flagging the assumptions (forward-shock-only dynamics, one-zone Thomson-regime radiation, an illustrative detectability criterion) limiting its quantitative reach.
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What it cites · 15 sentences without a confident label
Builds on 1 paper
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We have extended the photospheric model of Villani [ref] with a first, explicitly approximate, estimate of the non-thermal emission produced when the relativistic, near-isotropic kinetic energy left over from a black-to-white hole transition collides with the interstellar medium.
Electromagnetic emission from a black-to-white hole transition -- Photospheric emission · Conclusions · 1.00
Uses data or values from 1 paper
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Villani [ref] self-consistently solves for the energy radiated in the prompt photospheric flash, $$, finding $∼5×10^43$–$3×10^44$ erg depending on the assumed pion fraction and ejecta temperature.
Electromagnetic emission from a black-to-white hole transition -- Photospheric emission · Prompt radiated energy versus blast-wave kinetic energy · 0.99
Compares with 1 paper
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Figure [ref] compares the prompt photospheric emission of Villani [ref] with the afterglow synchrotron and SSC emission computed here, using the absolute energy fluence (erg cm$^-2$) in both cases – the prompt fluence from the actual radiated energy $$ distributed over the spectral shape of Ref. [ref] , and the afterglow fluence from the synchrotron and SSC flux integrated over the ultra-relativistic window $t_dec≤t≤t_valid$, with $t_valid$ defined by $Γ(t_valid)=2.5$ (Sec. [ref]A) – rather than an arbitrarily normalized snapshot.
Electromagnetic emission from a black-to-white hole transition -- Photospheric emission · Detectability: an illustrative count-based criterion · 0.98
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