TY - JOUR A2 - Zheng, WeiKang AU - Tanaka, Masaomi PY - 2016 DA - 2016/07/14 TI - Kilonova/Macronova Emission from Compact Binary Mergers SP - 6341974 VL - 2016 AB - We review current understanding of kilonova/macronova emission from compact binary mergers (mergers of two neutron stars or a neutron star and a black hole). Kilonova/macronova is emission powered by radioactive decays of r 动线核最promisin之一g electromagnetic counterparts of gravitational wave sources. Emission from the dynamical ejecta of ~0.01 M ⊙ is likely to have a luminosity of ~10⁴⁰–10⁴¹ erg s⁻¹with a characteristic timescale of about 1 week. The spectral peak is located in red optical or near-infrared wavelengths. A subsequent accretion disk wind may provide an additional luminosity or an earlier/bluer emission if it is not absorbed by the precedent dynamical ejecta. The detection of near-infrared excess in short GRB 130603B and possible optical excess in GRB 060614 supports the concept of the kilonova/macronova scenario. At 200 Mpc distance, a typical peak brightness of kilonova/macronova with 0.01 M ⊙ ejecta is about 22 mag and the emission rapidly fades to >24 mag within ~10 days. Kilonova/macronova candidates can be distinguished from supernovae by (1) the faster time evolution, (2) fainter absolute magnitudes, and (3) redder colors. Since the high expansion velocity ( v ~ 0.1 – 0.2 c ) is a robust outcome of compact binary mergers, the detection of smooth spectra will be the smoking gun to conclusively identify the gravitational wave source. SN - 1687-7969 UR - https://doi.org/10.1155/2016/6341974 DO - 10.1155/2016/6341974 JF - Advances in Astronomy PB - Hindawi Publishing Corporation KW - ER -