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Revisiting the Parameter Space of Binary Neutron Star Merger Event GW170817
High Energy Astrophysical Phenomena · Submitted 22 Feb 2023
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that our model prefers a gamma-ray burst with jet energy $E_j\sim10^{50}$ ergs and with an observer angle of $\theta_{obs}=0.65^{+0.13}_{-0.14}$ radians and ratio to jet opening angle of ($\theta_{obs}/\theta_j$) = 5.4$^{+0.53}_{-0.38}$.
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The abstract, sentence by sentence
Since the gravitational wave event GW170817 and gamma-ray burst GW170817A there have been numerous studies constraining the burst properties through analysis of the afterglow light curves. Most agree that the burst was viewed off-axis with a ratio of the observer angle to the jet angle ($\theta_{obs}/\theta_j$) between 4 - 6. We use a parameterized model and broadband synchrotron data up to $\sim 800$ days post-merger to constrain parameters of the burst. To reproduce the hydrodynamics of a gamma-ray burst outflow we use a two-parameter "boosted fireball" model. The structure of a boosted fireball is determined by the specific internal energy, $\eta_0$, and the bulk Lorentz factor, $\gamma_B(\sim 1/\theta_j)$ with shapes varying smoothly from a quasi-spherical outflow for low values of $\gamma_B$ to a highly collimated jet for high values. We run simulations with $\gamma_B$ in the range $1-20$ and $\eta_0$ in the range $2-15$. To calculate light curves we use a synchrotron radiation model characterized by $F_{peak}$, $\nu_m$, and $\nu_c$ and calculate millions of spectra at different times and $\theta_{obs}$ values using the \texttt{boxfit} radiation code. We can tabulate the spectral parameter values from our spectra and rapidly generate arbitrary light curves for comparison to data in MCMC analysis. We find that our model prefers a gamma-ray burst with jet energy $E_j\sim10^{50}$ ergs and with an observer angle of $\theta_{obs}=0.65^{+0.13}_{-0.14}$ radians and ratio to jet opening angle of ($\theta_{obs}/\theta_j$) = 5.4$^{+0.53}_{-0.38}$.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Since the gravitational wave event GW170817 and gamma-ray burst GW170817A there have been numerous studies constraining the burst properties through analysis of the afterglow light curves. | background 1.00 | 0.04 | 0.01 | asserted 1.00 |
| s1 | Most agree that the burst was viewed off-axis with a ratio of the observer angle to the jet angle ($\theta_{obs}/\theta_j$) between 4 - 6. | background 1.00 | 0.04 | 0.05 | asserted 0.89 |
| s2 | We use a parameterized model and broadband synchrotron data up to $\sim 800$ days post-merger to constrain parameters of the burst. | method 0.68 | 0.95 | 0.03 | asserted 0.98 |
| s3 | To reproduce the hydrodynamics of a gamma-ray burst outflow we use a two-parameter "boosted fireball" model. | method 0.99 | 0.79 | 0.02 | asserted 0.99 |
| s4 | The structure of a boosted fireball is determined by the specific internal energy, $\eta_0$, and the bulk Lorentz factor, $\gamma_B(\sim 1/\theta_j)$ with shapes varying smoothly from a quasi-spherical outflow for low values of $\gamma_B$ to a highly collimated jet for high values. | method 0.93 | 0.12 | 0.03 | asserted 1.00 |
| s5 | We run simulations with $\gamma_B$ in the range $1-20$ and $\eta_0$ in the range $2-15$. | method 0.99 | 0.95 | 0.02 | asserted 0.97 |
| s6 | To calculate light curves we use a synchrotron radiation model characterized by $F_{peak}$, $\nu_m$, and $\nu_c$ and calculate millions of spectra at different times and $\theta_{obs}$ values using the \texttt{boxfit} radiation code. | method 1.00 | 0.94 | 0.02 | asserted 0.99 |
| s7 | We can tabulate the spectral parameter values from our spectra and rapidly generate arbitrary light curves for comparison to data in MCMC analysis. | method 0.98 | 0.93 | 0.03 | asserted 0.77 |
| s8 | We find that our model prefers a gamma-ray burst with jet energy $E_j\sim10^{50}$ ergs and with an observer angle of $\theta_{obs}=0.65^{+0.13}_{-0.14}$ radians and ratio to jet opening angle of ($\theta_{obs}/\theta_j$) = 5.4$^{+0.53}_{-0.38}$. | result 1.00 | 0.97 | 0.93 | asserted 1.00 |
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The paper
Original abstract
Since the gravitational wave event GW170817 and gamma-ray burst GW170817A there have been numerous studies constraining the burst properties through analysis of the afterglow light curves. Most agree that the burst was viewed off-axis with a ratio of the observer angle to the jet angle ($\theta_{obs}/\theta_j$) between 4 - 6. We use a parameterized model and broadband synchrotron data up to $\sim 800$ days post-merger to constrain parameters of the burst. To reproduce the hydrodynamics of a gamma-ray burst outflow we use a two-parameter "boosted fireball" model. The structure of a boosted fireball is determined by the specific internal energy, $\eta_0$, and the bulk Lorentz factor, $\gamma_B(\sim 1/\theta_j)$ with shapes varying smoothly from a quasi-spherical outflow for low values of $\gamma_B$ to a highly collimated jet for high values. We run simulations with $\gamma_B$ in the range $1-20$ and $\eta_0$ in the range $2-15$. To calculate light curves we use a synchrotron radiation model characterized by $F_{peak}$, $\nu_m$, and $\nu_c$ and calculate millions of spectra at different times and $\theta_{obs}$ values using the \texttt{boxfit} radiation code. We can tabulate the spectral parameter values from our spectra and rapidly generate arbitrary light curves for comparison to data in MCMC analysis. We find that our model prefers a gamma-ray burst with jet energy $E_j\sim10^{50}$ ergs and with an observer angle of $\theta_{obs}=0.65^{+0.13}_{-0.14}$ radians and ratio to jet opening angle of ($\theta_{obs}/\theta_j$) = 5.4$^{+0.53}_{-0.38}$.
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How the literature uses it
2 arXiv papers cite this in 5 sentences
Papers citing it · 4 sentences without a confident label
Uses its method or tool 1 paper
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In this paper, we derive an improved measurement of $H_0$ by deriving updated viewing angle constraints from the EM counterpart using data out to over 3 years from the GW merger, in place of the data up to $∼1$ year, state-of-the-art hydrodynamic simulations from [ref] , as well as including a proper treatment of the impact of peculiar velocity of the host galaxy [ref] .
A standard siren measurement of the Hubble constant using GW170817 and the latest observations of the electromagnetic counterpart afterglow · Introduction · 0.98
What it cites
Cites as background 1 paper
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Semi-analytic models for the deceleration and spreading of the jetted outflow have been presented which attempt to explain the evolution of the jet in both 1D and 2D and compute afterglow radiation estimates from the hydrodynamics ( [ref] , [ref] ).
Deceleration of relativistic jets with lateral expansion · Boosted Fireball · 0.89
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