Identifying the Remnants of Neutron Star Mergers. Wen-fai Fong University of Arizona
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1 Identifying the Remnants of Neutron Star Mergers Wen-fai Fong University of Arizona Einstein Fellows Symposium, Harvard-Smithsonian Center for Astrophysics,
2 What s left after two neutron stars merge?
3 What s left after two neutron stars merge? hypermassive neutron star magnetar
4 What s left after two neutron stars merge? hypermassive neutron star magnetar
5 What s left after two neutron stars merge? hypermassive neutron star short GRB magnetar
6 What s left after two neutron stars merge? hypermassive neutron star short GRB magnetar } How long is this stage?
7 Long-lived magnetars in short GRBs: Extended emission Perley et al. 2009
8 Long-lived magnetars in short GRBs: Extended emission Perley et al. 2009
9 Long-lived magnetars in short GRBs: X-ray plateaus Rowlinson et al. 2013
10 Long-lived magnetars in short GRBs: X-ray plateaus plateau Rowlinson et al. 2013
11 Long-lived magnetars in short GRBs: X-ray plateaus plateau Rowlinson et al. 2013
12 Long-lived magnetars in short GRBs: X-ray plateaus plateau plateau Rowlinson et al. 2013
13 Long-lived magnetars in short GRBs: X-ray plateaus no plateau plateau Rowlinson et al. 2013
14 Magnetar spin-down energy powers a radio transient? magnetar Nakar & Piran 2011; Metzger & Bower 2013
15 Magnetar spin-down energy powers a radio transient? Energy ~ erg magnetar Nakar & Piran 2011; Metzger & Bower 2013
16 Magnetar spin-down energy powers a radio transient? Energy ~ erg Deceleration time E, n, v Nakar & Piran 2011; Metzger & Bower 2013
17 Model light curves for varying densities E~10 52 v=0.8c L (erg s 1 ) Rest frame Time after Merger (yr)
18 Model light curves for varying densities E~10 52 v=0.8c L (erg s 1 ) cm cm cm 3 1 cm cm 3 Rest frame Time after Merger (yr)
19 Model light curves: Density is a key parameter E~10 52 v=0.8c tdec L (erg s 1 ) cm cm cm 3 1 cm cm 3 Rest frame Time after Merger (yr)
20 Model light curves: Density is a key parameter E~10 52 v=0.8c tdec~years L (erg s 1 ) cm cm cm 3 1 cm cm 3 Rest frame Time after Merger (yr)
21 Existing radio observations of short GRBs are too early 10 3 Detection 3 upper limit Radio Radio Flux Density (µjy) A A A B 10 1 Time after Burst t (days) Fong et al. 2015
22 Radio observations as a test of the magnetar model 9 events with previous signature of a magnetar
23 Radio observations as a test of the magnetar model 9 events with previous signature of a magnetar 5.8 GHz, VLA
24 What constraints can the upper limits place on the magnetar model? 10 3 GRB B 5.8 GHz Flux Density (µjy) Rest frame Time After Burst (yr) Fong et al., in prep
25 What constraints can the upper limits place on the magnetar model? 10 3 GRB B 5.8 GHz Flux Density (µjy) cm cm cm Rest frame Time After Burst (yr) 10 3 cm 3 Fong et al., in prep
26 What constraints can the upper limits place on the magnetar model? 10 3 GRB B 5.8 GHz Flux Density (µjy) cm cm cm Rest frame Time After Burst (yr) Afterglow density constraints from Fong et al cm 3 Fong et al., in prep
27 What constraints can the upper limits place on the magnetar model? 5.8 GHz Flux Density (µjy) cm cm cm 3 GRB B n<0.08 cm Rest frame Time After Burst (yr) Afterglow density constraints from Fong et al cm 3 Fong et al., in prep
28 What constraints can the upper limits place on the magnetar model? 5.8 GHz Flux Density (µjy) cm cm cm 3 GRB B n<0.08 cm Rest frame Time After Burst (yr) Afterglow density constraints from Fong et al cm 3 Fong et al., in prep
29 What constraints can the upper limits place on the magnetar model? 10 4 GRB A 5.8 GHz Flux Density (µjy) Rest frame Time After Burst (yr) Fong et al., in prep
30 What constraints can the upper limits place on the magnetar model? 10 4 GRB A 5.8 GHz Flux Density (µjy) cm cm cm Rest frame Time After Burst (yr) 10 3 cm cm 3 Fong et al., in prep
31 What constraints can the upper limits place on the magnetar model? 10 4 GRB A 5.8 GHz Flux Density (µjy) cm cm cm Rest frame Time After Burst (yr) Afterglow density constraints from Fong et al cm cm 3 Fong et al., in prep
32 What constraints can the upper limits place on the magnetar model? 5.8 GHz Flux Density (µjy) cm cm cm 3 GRB A n<0.002 cm Rest frame Time After Burst (yr) Afterglow density constraints from Fong et al cm cm 3 Fong et al., in prep
33 5.8 GHz Flux Density (µjy) GRB A n<0.50 cm GHz Flux Density (µjy) GRB A n<0.04 cm GHz Flux Density (µjy) GRB A n<0.01 cm Rest frame Time After Burst (yr) 10 0 Rest frame Time After Burst (yr) 10 0 Rest frame Time After Burst (yr) 5.8 GHz Flux Density (µjy) GRB A 10 4 n<0.002 cm 3 GRB GRB n<0.20 cm 3 n<0.015 cm cm cm cm Rest frame Time After Burst (yr) 10 3 cm cm GHz Flux Density (µjy) Rest frame Time After Burst (yr) 5.8 GHz Flux Density (µjy) Rest frame Time After Burst (yr) 5.8 GHz Flux Density (µjy) GRB A n<0.21 cm Rest frame Time After Burst (yr) 5.8 GHz Flux Density (µjy) GRB A n<0.06 cm Rest frame Time After Burst (yr) 5.8 GHz Flux Density (µjy) cm cm cm 3 GRB B n<0.08 cm Rest frame Time After Burst (yr) 10 3 cm 3
34 What constraints can the upper limits place on the magnetar model? L (erg s 1 ) Rest frame Time after Merger (yr) Fong et al., in prep
35 What constraints can the upper limits place on the magnetar model? L (erg s 1 ) cm cm cm 3 1 cm cm 3 Rest frame Time after Merger (yr) Fong et al., in prep
36 What constraints can the upper limits place on the magnetar model? L (erg s 1 ) cm cm cm 3 1 cm cm 3 Rest frame Time after Merger (yr) Fong et al., in prep
37 What constraints can the upper limits place on the magnetar model? L (erg s 1 ) cm cm cm 3 1 cm Mpc 10 4 cm 3 Rest frame Time after Merger (yr) aligo Fong et al., in prep
38 Summary & Future Directions + Ruled out long-lived magnetars for densities greater than cm -3 + Explore additional parameters (energy, velocity) + Consider future observations
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