High energy neutrino signals from NS-NS mergers

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1 High energy neutrino signals from NS-NS mergers He Gao 高鹤 University of Nevada Las Vegas Collaborators: Bing Zhang, Xue-Feng Wu & Zi-Gao Dai Multi-Messenger KIAA

2 EM signals for a magnetar post-merger product Jet- shock (Afterglow) SGRB MNS Poynting flux X-ray X-ray Zhang 2013; Gao et al. 2013a Radio Optical X-ray SGRB? Late central engine activity ~Plateau & X-ray flare Magnetic Dissipation X-ray Afterglow ~ 10 erg s cm ~10000 s Zhang, shock with Energy Injection (EI) Multi-band transient ~hours, days, weeks, or even years Gao et al, 2013a

3 EM signals for a magnetar post-merger product Jet- shock (Afterglow) SGRB MNS Poynting flux X-ray X-ray Zhang 2013; Gao et al. 2013a Radio Optical X-ray SGRB? Late central engine activity ~Plateau & X-ray flare Magnetic Dissipation X-ray Afterglow ~ 10 erg s cm ~10000 s Zhang, shock with Energy Injection (EI) Multi-band transient ~hours, days, weeks, or even years Gao et al, 2013a

4 General picture for neutrino signal releasing Dissipated photons e p e p EM HECR Gao et al, 2013 Kotera & Olinto 2011

5 General picture for neutrino signal releasing γ γ γ γ γ γγγγ γ p

6 General picture for neutrino signal releasing γ γ γ γ γ γγγγ γ p

7 Neutrino signals for a magnetar post-merger product p γ p γ γz γ γ γ γ

8 Neutrino signals for a magnetar post-merger product p γ γ z γ γ γ γ γ γ!!!

9 Neutrino signals for a magnetar post-merger product p γ γ z γ γ γ γ γ γ

10 General picture for neutrino signal releasing p γ p γ γz γ γ γ γ

11 General picture for neutrino signal releasing p γ p γ γz γ γ γ γ Typical energy of neutrino: E ν,t E ~0.05E ~ Γ GeV /E 2 2 ν,t p,t γ,t Typical value of neutrino fluence: f E f f tot,t ν 2 4πd

12 General picture for neutrino signal releasing p γ p γ γz γ γ γ γ Typical energy of neutrino: E ν,t E ~0.05E ~ Γ GeV /E 2 2 ν,t p,t γ,t Typical value of neutrino fluence:? E peak f E f f tot,t ν 2 4πd

13 General picture for neutrino signal releasing p γ p γ γz γ γ γ γ Typical energy of neutrino: E ν,t E ~0.05E ~ Γ GeV /E 2 2 ν,t p,t γ,t Typical value of neutrino fluence: f E f f tot,t ν 2 4πd? E peak Proton Distribution

14 General picture for neutrino signal releasing p γ p γ γz γ γ γ γ Typical energy of neutrino: E ν,t E ~0.05E ~ Γ GeV /E 2 2 ν,t p,t γ,t Typical value of neutrino fluence: f? E f f tot,t ν 2 4πd? Dynamics

15 Typical photon energy M Dissipation process happened before the collision Optically thin Zhang, /2 4/3 2/3 1.8 kev L0,47η-1 σ0,7r 0,7 15 R IC ~10 cm Zhang & Yan, 2011

16 Typical photon energy M Collision between magnetized wind and ejecta induced dissipation Optically thin Dissipation process happened before the collision Optically thin 3/2 4/3 2/3-5/3 1.8 kev L0,47η-1 σ0,7r0,7r15 Zhang, /2 4/3 2/3 1.8 kev L0,47η-1 σ0,7r 0,7 15 R IC ~10 cm Zhang & Yan, 2011

17 Typical photon energy M Collision between magnetized wind and ejecta induced dissipation Optically thick Collision between magnetized wind and ejecta induced dissipation Optically thin Dissipation process happened before the collision Optically thin 3/2 4/3 2/3-5/3 0.5 kev L η R 1.8 kev L η σ R R 1/4 1/4-0, L0 kt~k 4 R 2 R ph 1/4 ~ cm M 14 ej,-3 0,47-1 0,7 0,7 15 Zhang, /2 4/3 2/3-5/3 1.8 kev L0,47η-1 σ0,7r0,7ri,15 None R ~10 R cm 15 IC i,15 Zhang & Yan, R sd ~2ΓsdcTsd

18 Proton distribution properties PL distribution f E f f tot,t ν 2 4πd dn( ) / d p p ΓGeV /(E m c ) 2 2 γ,t p E =4πR nγ(γ-1)m c /3 tot 3 2 p 2 ΓγMmc p γm 1 E γ p,t p,t Eγ γp,t Etot γm p,t f γ ~ p,t 2-p γm,t γ M p-2 Assuming p>2, one can easily estimate: γ m ~(Γ-1) +1 p-1 By balancing acceleration time scale and the ΓteB' dynamical timescale, we could estimate: γm mc p p 1 τ f pγ ~ (1-(1-<χ pπ >) ) 0.1τ pγ 2 (χ p π 0.2, τ pγ 3) Dynamics?

19 - shock dynamics For given B p different leads to different Dynamics cases. M ej M ~ 610 M I P 3 2 ej, cr,2 45 0, 3 If M ej M ej, cr,2 Non-relativistic Gao et al, 2013

20 Examples: B p =10 15 G, M ej =10-4 M sun M 300Mpc R R RIC ph N =12.0 =55.9 1/4-5/12 2/3-1/6 =0.01η -1 L0,49 Mej,-4n 0 R15 3/2-1/6 2/3 4/3 2/3-4/3 3/2-1/6 2/3 4/3 2/3 1/3 η-1 L0,49Mej,-4n 0 0,7 R0,7R15 η-1 L0,49Mej,-4 n0 0,7 R0,7R17 Rsd needs to be accelerated to relativistic for significant neutrino releasing E f ν,t ν,t =0.02 PeV η L M R R 3/ 2 1/6-2/3 4/3 2/3 7/3-1 0,49 ej,-4 0,7 0,7 15 =6.310 GeV cm 11 2 η L n R R ,49 0 0,7 0,7 17 E f ν,t ν,t =0.5 PeV η L M R R 3/ 2 1/6-2/3 4/3 2/3 2/3-1 0,49 ej,-4 0,7 0,7 15 =6.310 GeV cm 7 2 η L n R R ,49 0 0,7 0,7 17

21 Detection prospect Single event detection probability Optimistic cases happened in 300Mpc E ν ~ PeV : IceCube f 5 2 ~10 GeV cm ν N ice 5 ~10 /event Event Rate in 300 Mpc: 0.1~10 3 yr -1 Diffuse background Talk in Zhang GRB: (300Mpc) Gao et al, 2013b, To be submitted 10 GeV cm 4 2 Event Rate: ~10 yr -1 He et al, 2012

22 Accompanied high energy photons p γ p γ γz γ γ γ γ E ~2E ν ~0.2 PeV f ~ f ~10 GeV cm ν 5 2

23 Accompanied high energy photons p γ p γ γz γ γ γ γ f E ~2E ν ~ PeV ~ f ~10 GeV cm ν e EM Gao et al, 2013

24 Accompanied high energy photons p γ p γ γz γ γ γ γ e EM f E ~2E ν ~PeV 1 ~ f ~10 GeV cm ν 5 2 Cascade Gao et al, Single event: N ice ~10 /event Contribute to diffuse background 100GeV LAT A eff ~10 cm 4 2 Atwood et al, 2009

25 Only if the NS-NS merger leave behind a magnetar rather than a BH, besides GW, the non-relativistic ejecta launched during the merger process would be pushed by a magnetar wind, a bright broadband EM afterglow emission would be developed; NS-NS merger event could act as accelerators of galactic high energy cosmic rays; ~PeV level neutrinos could be emitted from the shock front region as long as the ejecta could be accelerated to be relativistic. NS-NS merger event could also be a strong candidate for diffuse background of sub-tev gamma-ray photons. Besides GRBs, NS-NS merger scenario has the potential to become another Multi-Messenger, which will help us better understand our universe.

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