Radio Flares from Neutron Star merges + More Tsvi Piran

Transcription

1 Radio Flares from Neutron Star merges + More Tsvi Piran Kenta Hotokezaka, Ehud Nakar, Ben Margalit Paz Beniamini, Stephan Rosswog

2 Outline A 2nd Macronova (Yang + 15, Nature comm in press.) Remarks about nucleosynthesis (Hotokezaka + Piran 15 in prep) Radio Flares (Nakar Piran, 11 Nature, )

3 The Macronova in Bin Yang Zhi-Ping Jin, Xiang Li, Stefano Covino, Xian-Zhong Zheng, Kenta Hotokezaka, Yi-Zhong Fan Tsvi Piran, Da-Ming; Wei Nature Phys a nearby long-short burst 102 sec No SNe z=0.125

4 Kilonova The Macronova in Bin Yang Zhi-Ping Jin, Xiang Li, Stefano Covino, Xian-Zhong Zheng, Kenta Hotokezaka, Yi-Zhong Fan Tsvi Piran, Da-Ming; Wei Nature Phys a nearby long-short burst 102 sec No SNe z=0.125

5 Kilonova -> Hectonova The Macronova in Bin Yang Zhi-Ping Jin, Xiang Li, Stefano Covino, Xian-Zhong Zheng, Kenta Hotokezaka, Yi-Zhong Fan Tsvi Piran, Da-Ming; Wei Nature Phys a nearby long-short burst 102 sec No SNe z=0.125

6 Kilonova -> Hectonova->Decanova? The Macronova in Bin Yang Zhi-Ping Jin, Xiang Li, Stefano Covino, Xian-Zhong Zheng, Kenta Hotokezaka, Yi-Zhong Fan Tsvi Piran, Da-Ming; Wei Nature Phys a nearby long-short burst 102 sec No SNe z=0.125

7 Kilonova -> Hectonova->Decanova? The Macronova in Bin Yang Zhi-Ping Jin, Xiang Li, Stefano Covino, Xian-Zhong Zheng, Kenta Hotokezaka, Yi-Zhong Fan Tsvi Piran, Da-Ming; Wei Nature Phys a nearby long-short burst 102 sec No SNe z=0.125

8 The Macronova

9 The Macronova

10 The Macronova B

11 Independent Analysis GRB i α =2.17 ± 0.13 k = ± flux (mjy) t t 0 (days) flux (mjy) d d d d d β 1 = 0.49 ± 0.11 β 2 = 1.21 ± 0.26 β 3 = 1.67 ± 0.32 β 4 = 1.03 ± 1.13 β 5 = 3.92 ± ν obs (Å) Zach Cano 2015 in prep.

12 Peak time and peak luminosity Diffusion time = expansion time <=> Mass of the emitting region Luminosity Radioactive heating rate The peak time The peak luminosity

13 Not so easy Peak at days -> ~ 0.1 M sun ->? Black Hole - NS merger?

14 Macronova

15 Macronova Nucleosynthesis Lattimer Schramm 76

16 Macronova Nucleosynthesis GRBs Lattimer Schramm 76 Eichler, Livio Piran, Schramm 89

17 R(z=0) [Myr -1 ] LIGO/Virgo limit R-element mass (A>90) Advanced (5yr) M ej [M sun ] Macronova candidate Galactic NS 2 Short GRBs

18 R(z=0) [Myr -1 ] LIGO/Virgo limit R-element mass (A>90) Advanced (5yr) M ej [M sun ] Macronova candidate Galactic NS 2 Short GRBs Wanderman Piran 15

19 R(z=0) [Myr -1 ] LIGO/Virgo limit R-element mass (A>90) Advanced (5yr) M ej [M sun ] Macronova candidate Galactic NS 2 Short GRBs Wanderman Piran 15

20 R(z=0) [Myr -1 ] LIGO/Virgo limit R-element mass (A>90) Advanced (5yr) M ej [M sun ] Macronova candidate Galactic NS 2 Short GRBs

21 R(z=0) [Myr -1 ] LIGO/Virgo limit R-element mass (A>90) Advanced (5yr) M ej [M sun ] Macronova candidate Galactic NS 2 Short GRBs

22 A comment on Galactic NS binary population Biniamin and Piran 15 in prep MS pulsars No kick Almost No mass ejection Regular pulsars Large kick Significant mass ejection

23 R-Process Nucleosynthesis - limits from the solar system Kenta Hotokezaka and Tsvi Piran

24 Abundance of live 244Pu in deep-sea reservoirs on Earth points to rarity of actinide nucleosynthesis A. Wallner, T. Faestermann, J. Feige, C. Feldstein, K. Knie, G. Korschinek, W. Kutschera, A. Ofan, M. Paul, F. Quinto, G. Rugel & P. Steier Nature Comm. 2014

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26 Mixing time D(t mix ) = A 1/2 / (R t mix ) D(t mix ) - mixing distance A - Area of the Galaxy R - Rate of events in the Galaxy We should compare t mix with the age of the Galaxy.

27 Mixing time D(t mix ) = A 1/2 / (R t mix ) D(t mix ) - mixing distance A - Area of the Galaxy R - Rate of events in the Galaxy We should compare t mix with the age of the Galaxy.

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30 The early solar system

31 Rare Events t Frequent events t

32 High 244 Pu at the early solar system => 244 Pu Radioactive decay time ~ 100 Myear A nearby event near solar system Mixing time < 150 Myr Large fluctuations possible => Event rate is low Lack of Cu => 10 Myr < Mixing length

33 Why EM signal? (Kochaneck & Piran 1993) Improves detectability Essential for localization Much more physics

34 GRBs are beamed -> dificult to catch the GRB Orpha afterglow will be too weak

35 Macronova Li & Paczynski 1997 Numerical simulations => NS merger eject >0.1 M o Davies, Benz, Piran & Thielemann 1994; Rosswog et al., 1999 Freiburghaus, Rosswog, & Thielemann, 1999

36 Radio Flares Nakar & Piran 2011 Interaction of the sub or mildly relativistic outflow with the ISM produces a long lived radio flare Supernova -> SNR macronova -> Radio Flare

37 Dynamics days log R Sedov-Taylor log t

38 Radio Supernova e.g. 1998bw (Chevalier 98) Tycho's supernova remnant seen at radio wavelengths e e =ε e e e B =B 2 /8π=ε B e N(γ) γ- p for γ> γ m p=2.5-3 γ m = (m p /m e )e e (Γ-1) ν=(3/4π)eb γ 2 F ν =(σ T c/e)n e B

39 Frequency and Intensity (Nakar & TP Nature, 2011)

40 Rosswog, TP, Nakar 13, TP, Nakar, Rosswog 13

41 Rosswog, TP, Nakar 13, TP, Nakar, Rosswog 13

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43 Radio Flares

44 The light curve ν m ν a ν obs ν m ν a ν eq ν m ν obs ν a t dec t dec t dec Text

45 The light curve F ν ν ν obs ν eq ν m ν a ν ν m ν obs ν a t dec t t dec t t dec t Text

46 The light curve F ν ν ν m ν a ν eq ν ν ν m obs ν a ν obs t dec t t dec t t dec t Text

47 The light curve F ν ν ν obs ν m ν a ν eq t dec t t dec t Text

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49 Effect of sphericity Margalit & Piran 15

50 Dale Frail

51 Dale Frail

52 Dale Frail

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56 Summary A detection of a macronova like signal in But need 0.1 M sun? Macronova ==> R process nucleosynthesis + sgrbs from Mergers 244 Pu gives strong support for R process nucleosynthesis consistent with Mergers Early solar system 244 Pu also set limits on mixing Radio flares are a second type of EM counterparts that can follow Mergers (long term - advantage) Detectablity prospects of radio flares (Hotokezaka talk)

57 Summary A detection of a macronova like signal in But need 0.1 M sun? Macronova ==> R process nucleosynthesis + sgrbs from Mergers 244 Pu gives strong support for R process nucleosynthesis consistent with Mergers Early solar system 244 Pu also set limits on mixing Radio flares are a second type of EM counterparts that can follow Mergers (long term - advantage) Detectablity prospects of radio flares (Hotokezaka talk)