Radioactively-Powered Gamma-Ray Transient Associated with a Kilonova from Neutron Star Merger

Abstract

AAssociation of GW170817/GRB170817A/AT2017gfo provides the first direct evidence for neutron star mergers as significant sources of $r$-process nucleosynthesis. A gamma-ray transient (GRT) would be powered by the radioactive decay of the freshly-synthesized $r$-process elements. By analyzing the composition and gamma-ray opacity of the kilonova ejecta in details, we calculate the lightcurve and spectrum of the GRT for a range of spherically symmetric merger ejecta models with mass $M_{\mathrm{ej}}=0.001\sim 0.05M_{\odot }$ and expansion velocity $v_{\mathrm{ej}}=0.1\sim 0.4c$. It is found that the peak of the GRT lightcurve depends on $M_{\mathrm{ej}}$ and $v_{\mathrm{ej}}$ as $t_{\mathrm{pk}}\approx 0.5\mathrm{days}(M_{\mathrm{ej}}/0.01M_{\odot }{)}^{1/2}(v_{\mathrm{ej}}/0.1c{)}^{-1}$ and $L_{\mathrm{pk}}\approx 2.0\times 10^{41}{\mathrm{erg}\mathrm{s}}^{-1}(M_{\mathrm{ej}}/0.01M_{\odot }{)}^{1/2}(v_{\mathrm{ej}}/0.1c)$. Most radiating photons are in the $100-3000$ keV band and the spectrum peaks at about 800~keV for different nuclear physics inputs. The line features are blurred out by the Doppler broadening effect. Adopting the ejecta parameters reported in literature, we examine the detection probability of the possible GRT associated with AT2017gfo. We show that the GRT cannot be convincingly detected neither with current nor with the proposed missions in the MeV band, such as ETCC and AMEGO. The low gamma-ray flux, together with the extremely low event rate at local universe, makes a discovery of GRTs a great challenge.

arXiv comment16 pages, 7 figures. Accepted for publication in the ApJ Letters

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Cited by in corpus (3)

• Nucleosynthesis in outflows of compact objects and detection prospects of associated kilonovae
• The thermalization of $\gamma$-rays in radioactive expanding ejecta: A simple model and its application for Kilonovae and Ia SNe
• Impact of nuclear mass models on $r$-process nucleosynthesis and heavy element abundances in $r$-process enhanced metal-poor stars