outline n n l GRBs s GRBs ls

outline n n l. GRBs & s. GRBs & ls. GRBs Macronova (kilonova) & GW GRB 170817 A/GW 170817 Summary

L & offset (Zhang et al. 2017)

GRB 130603 B (Tanvir et al. 2013) • (Berger et al. 2013)

08/09/2016 8 GRB 050709 新的macronova信号 (Jin et al. 2016 Nat. Commun. ) 图左: GRB 050709的光学余辉图，注意I/F 814 W波段和R波段衰减的显著不同. 图右: GRB 050709的I/F 814 W波段的辐射很难用单一幂率衰减拟合，而和GRB 060614中 macronova成分高度相似.

Energy conversion efficiencies of s. GRBs (Shen et al. 2017)

GRB 060614：Long GRB without SN • 100秒 • Gehrels et al. 2006 Nature • Fynbo et al. 2006 Nature • 11

Macronova signature in GRB 060614 • SN 2008 ha (Yang et al. 2015, Nature Communications, Jin et al. 2015, Ap. JL)

Macronova与超新星光变曲线的比较 (Jin et al. 2016) (Smartt et al. 2017, Nature)

长短暴 n n n 长短暴-不伴有超新星的长暴 GRB 060614, GRB 060505 GRB 111005 A, T 90 = 26 s, z = 0. 0133

GRB 111005 A &GRB 170817 A 17

ls. GRBs &GRB 170817 A

GRB 111005 A类事件的发生率 事件探测率 (Wang et al. 2017)

s. GRB/GW association: suggested in 1980 s • 22

基本信息 n n n GW 170817/GRB 170817 A 引力波与伽玛暴时间间隔 1. 7秒 距离 40 Mpc T 90 ~2 s Epeak ~ 185 Ke. V

Macronova的光变曲线 跟GRB 060614、 GRB 050709的比较 (Kasliwal et al. 2017, Science)

s. GRBs with jet breaks (Jin et al. 2017)

The neutron star merger rate in the local Universe The rate density of neutron star merger can be calculated as For off-axis events, the rate may be enhanced by a factor (Jin et al. 2017)

s. GRB/GW association: time-lag The time-lag consists of two parts, including: 1. The time of launching the ultrarelativistic ejecta (Depending on the collapse timescale of the merger remnant into black hole? ) 2. The time of the energy dissipation (Depending on the energy dissipation mechanism)

s. GRB/GW association: time-lag Usually the time-lag is expected to be ~1 ms-1 s. (Li et al. 2016)

GRB/GW association: measuring GW velocity u. In GR the GW velocity is the speed of the light (c) u. In other theories the GW velocity could be either lower or higher than c. No direct measurement before u. The detection of GRB/GW (or other kinds of transient and GW) association can be used to directly and accurately measure the GW velocity!

GRB 170817 A: off-axis s. GRB? In the off-beam case, we have the following relations For typical bright s. GRBs we have an isotropic equivalent gamma-ray radiation energy (Wang et al. 2017)

Possible constraint on the subluminal movement the optical emission of macronova/kilonova is known to present within 1 day after the merger. The successful detection of macronova/kilonova emission at ∼ 0. 5 days suggest that the time delay of the arrival of the GW signal due to its subluminal movement can not be longer than ∼ 0. 5 days, then we have (Wang et al. 2017)

Testing the Einstein equivalence principle The Shapiro delay is generally calculated as (Wang et al. 2017)

The r-process element production To account for the measured total mass of galactic heavy r-process Elements , the binary neutron star merger rate averaged over the galaxy age should be The merger rate is actually not a constant and the inferred merger rate at present time (R 0) may be lower than the averaged one by a factor of a few (i. e. , Ro < �R�) (Wang et al. 2017)

Diverse macronova emission? (Yue et al. 2017)

Masses of neutron-rich ejecta (Wang. et al. 2017)

Diverse macronova emission? . The redshift is not secure: GRB 061201. . No redshift measurement: GRB 080503. . Limits of afterglow/macronova is not secure: GRB 050509 B. 41

whether some bright GRBs could be similar to GRB 170817 A if viewed off-beam (Yue et al. 2017)

whethere are some weak SN-less GRBs similar to GRB 170817 A (Yue et al. 2017)

(Huang et al. 2018)