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- W2108151777 abstract "We use 3D hydrodynamic simulations of the long-term evolution of neutron star merger ejecta to predict the light curves of electromagnetic transients that are powered by the decay of freshly produced r-process nuclei. For the dynamic ejecta that are launched by tidal and hydrodynamic interaction, we adopt grey opacities of 10 cm2 g−1, as suggested by recent studies. For our reference case of a 1.3–1.4 |$mathrm{{rm M}}_{odot }$| merger, we find a broad IR peak 2–4 d after the merger. The peak luminosity is ≈2 × 1040 erg s−1 for an average orientation, but increased by up to a factor of 4 for more favourable binary parameters and viewing angles. These signals are rather weak and hardly detectable within the large error box (∼100 deg2) of a gravitational wave trigger. A second electromagnetic transient results from neutrino-driven winds. These winds produce ‘weak’ r-process material with 50 < A < 130 and abundance patterns that vary substantially between different merger cases. For an adopted opacity of 1 cm2 g−1, the resulting transients peak in the UV/optical about 6 h after the merger with a luminosity of ≈1041 erg s−1 (for a wind of 0.01 |$mathrm{{rm M}}_{odot }$|) These signals are marginally detectable in deep follow-up searches (e.g. using Hypersuprime camera on Subaru). A subsequent detection of the weaker but longer lasting IR signal would allow an identification of the merger event. We briefly discuss the implications of our results to the recent detection of a near infrared (nIR) transient accompanying GRB 130603B." @default.
- W2108151777 created "2016-06-24" @default.
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- W2108151777 date "2014-01-31" @default.
- W2108151777 modified "2023-10-11" @default.
- W2108151777 title "The long-term evolution of neutron star merger remnants – II. Radioactively powered transients" @default.
- W2108151777 cites W1660004571 @default.
- W2108151777 cites W1851157365 @default.
- W2108151777 cites W1935672049 @default.
- W2108151777 cites W1963491799 @default.
- W2108151777 cites W1977998389 @default.
- W2108151777 cites W1978916504 @default.
- W2108151777 cites W1981109864 @default.
- W2108151777 cites W1982968317 @default.
- W2108151777 cites W1984290148 @default.
- W2108151777 cites W1984649626 @default.
- W2108151777 cites W1986183096 @default.
- W2108151777 cites W1986721897 @default.
- W2108151777 cites W1988605574 @default.
- W2108151777 cites W1993455451 @default.
- W2108151777 cites W1996162015 @default.
- W2108151777 cites W1999405654 @default.
- W2108151777 cites W2001646918 @default.
- W2108151777 cites W2009295842 @default.
- W2108151777 cites W2012291066 @default.
- W2108151777 cites W2012843373 @default.
- W2108151777 cites W2018829983 @default.
- W2108151777 cites W2019486664 @default.
- W2108151777 cites W2021807007 @default.
- W2108151777 cites W2024743329 @default.
- W2108151777 cites W2027299393 @default.
- W2108151777 cites W2032765055 @default.
- W2108151777 cites W2044602433 @default.
- W2108151777 cites W2049211861 @default.
- W2108151777 cites W2050838288 @default.
- W2108151777 cites W2058582347 @default.
- W2108151777 cites W2070722652 @default.
- W2108151777 cites W2076112541 @default.
- W2108151777 cites W2077007583 @default.
- W2108151777 cites W2079104852 @default.
- W2108151777 cites W2080461561 @default.
- W2108151777 cites W2083345410 @default.
- W2108151777 cites W2087010948 @default.
- W2108151777 cites W2094576070 @default.
- W2108151777 cites W2111641259 @default.
- W2108151777 cites W2123867568 @default.
- W2108151777 cites W2131335108 @default.
- W2108151777 cites W2133878192 @default.
- W2108151777 cites W2140058367 @default.
- W2108151777 cites W2141120919 @default.
- W2108151777 cites W2142775778 @default.
- W2108151777 cites W2143470469 @default.
- W2108151777 cites W2144898929 @default.
- W2108151777 cites W2155465642 @default.
- W2108151777 cites W2158571066 @default.
- W2108151777 cites W2159546027 @default.
- W2108151777 cites W2161549006 @default.
- W2108151777 cites W2567032824 @default.
- W2108151777 cites W3098036686 @default.
- W2108151777 cites W3098127390 @default.
- W2108151777 cites W3098553117 @default.
- W2108151777 cites W3098737165 @default.
- W2108151777 cites W3099134998 @default.
- W2108151777 cites W3099652661 @default.
- W2108151777 cites W3100108344 @default.
- W2108151777 cites W3100192584 @default.
- W2108151777 cites W3100421444 @default.
- W2108151777 cites W3100860095 @default.
- W2108151777 cites W3100952523 @default.
- W2108151777 cites W3101366092 @default.
- W2108151777 cites W3101955293 @default.
- W2108151777 cites W3102192395 @default.
- W2108151777 cites W3102644197 @default.
- W2108151777 cites W3102728091 @default.
- W2108151777 cites W3103989567 @default.
- W2108151777 cites W3104205580 @default.
- W2108151777 cites W3104259347 @default.
- W2108151777 cites W3104948335 @default.
- W2108151777 cites W3105884385 @default.
- W2108151777 cites W3122791830 @default.
- W2108151777 cites W3124479694 @default.
- W2108151777 cites W3124644644 @default.
- W2108151777 cites W3125372064 @default.
- W2108151777 cites W3125445448 @default.
- W2108151777 cites W3125817460 @default.
- W2108151777 doi "https://doi.org/10.1093/mnras/stt2503" @default.
- W2108151777 hasPublicationYear "2014" @default.
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