Multimessenger Probes of Neutron Star Physics. David Tsang (U. Southampton)
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1 Resonant Shattering Flares: Multimessenger Probes of Neutron Star Physics David Tsang (U. Southampton)
2 GW/EM A Golden Binary Kasliwal Flux density (mjy) v 28º, j 15º 15 v 28º X-ray (on-axis) 6 GHz 19 GHz i band X-ray Time since gravitational-wave trigger (days) Apparent AB magnitude B + 7 V + 6 R + 5 I + 4 No wind Time since gravitational-wave trigger (days) avelength light curves for the counterpart of off-axis with viewing angle 28. For comparison wit Troja+, 2017 z + 3 J + 2 H + 1 K s Flux density (mjy) LVC + Fermi, 2017
3 GWs can provide tidal constraints But, kne & SGRBs don t tell us much about NS structure Only (messy) post merger physics r-process Metzger & Berger (2011) M ejecta
4 GWs can provide tidal constraints But, kne & SGRBs don t tell us much about NS structure Only (messy) post merger physics Mad Max: Fury Road (2015) r-process M ejecta
5 GWs can provide tidal constraints But, kne & SGRBs don t tell us much about NS structure Only (messy) post merger physics Mad Max: Fury Road (2015) r-process M ejecta RSFs are bright, isotropic EM counterparts that can provide detailed asteroseismic constraints on NS physics
6 Tidal Resonance can transfer huge amounts of energy from orbit to modes Need a mode that: strains the crust Tidal Resonance couples to the tidal field (l=2, spheroidal) hits a resonance well before merger (f < 1 khz)
7 Tidal Resonance Tidal Resonance can transfer huge amounts of energy from orbit to modes Need a mode that: strains the crust couples to the tidal field (l=2, spheroidal) hits a resonance well before merger (f < 1 khz) i2 l = 2 crust-core interface mode fractional radius r/r U(r) V(r) 10 Core Crust displacement km DT+, PRL, 108, (2012)
8
9 The i-mode exists because of the solid-fluid transition. The frequency depends on the core-crust transition radius and shear speed
10 Resonant Shattering Flares Orbit Ė tidal ' erg s 1 Resonance E b ' erg Mode E crack ' 2 bµ rcrust 3 ' erg Cracking Pair-Fireball ergs Seismic Magnetic Field L max erg s 1 (v/c) E elastic = I dv 2 bµ erg Seismic (shattered) (B surf /10 14 G) 2 (R/10 km) 2 DT+, PRL, 108, (2012) DT, ApJ, 777, 103 (2013)
11 Resonant Shattering Flares ERSF ~ erg, ΔtRSF ~ 0.1s RSF model can be easily tested with EM/GW coincident timing ~1-10 s Predicts weak GRB-like emission seconds before the chirp coalescence time from merger 0 The timing of the RSF provides precision asteroseismology of the NS i-mode i-mode frequency dependent on EOS, NS bulk properties and shear velocity at base of the crust ~ ms Constrains unknown nuclear physics (Symmetry energy, EOS )
12 Resonant Shattering Flares ERSF ~ erg, ΔtRSF ~ 0.1s RSF model can be easily tested with EM/GW coincident timing ~1-10 s Predicts weak GRB-like emission seconds before the chirp coalescence time from merger 0 The timing of the RSF provides precision asteroseismology of the NS i-mode i-mode frequency dependent on EOS, NS bulk properties and shear velocity at base of the crust ~ ms Constrains unknown nuclear physics (Symmetry energy, EOS )
13 DT+, PRL, 108, (2012)
14 DT+, PRL, 108, (2012)
15 t DT+, PRL, 108, (2012)
16 t DT+, PRL, 108, (2012)
17 Resonant Shattering Flares ERSF ~ erg, ΔtRSF ~ 0.1s RSF model can be easily tested with EM/GW coincident timing ~1-10 s Predicts weak GRB-like emission seconds before the chirp coalescence time from merger 0 The timing of the RSF provides precision asteroseismology of the NS i-mode i-mode frequency dependent on EOS, NS bulk properties and shear velocity at base of the crust ~ ms Constrains nuclear physics? (Symmetry energy, EOS )
18 Resonant Shattering Flares ERSF ~ erg, ΔtRSF ~ 0.1s RSF model can be easily tested with EM/GW coincident timing ~1-10 s Predicts weak GRB-like emission seconds before the chirp coalescence time from merger 0 The timing of the RSF provides precision asteroseismology of the NS i-mode i-mode frequency dependent on EOS, NS bulk properties and shear velocity at base of the crust ~ ms Constrains nuclear physics? (Symmetry energy, EOS )
19 Pair-Fireball ergs Magnetic Field L max erg s 1 (v/c) (B surf /10 14 G) 2 (R/10 km) 2
20 Gourgouliatos & Hollerbach (2018) Magnetic Field Pair-Fireball ergs L max erg s 1 (v/c) (B surf /10 14 G) 2 (R/10 km) 2 NS Surface B-field determines max luminosity Surface B-field depends on initial conditions, age, toroidal field, accretion history, core flux vs crust only (see e.g. Ho, Andersson, & Graber [2017]) Do not expect bright RSFs for all NS e.g. RSF not seen in GW170817
21 How detectable are EM counterparts? BH/NS Horizon ~930Mpc NS/NS Horizon ~440Mpc (kne detectability from Kalsiwal & Nissanke, 2014) kne (Red) kne (Blue) kne (Bright) (DT et al. in prep)
22 How detectable are EM counterparts? sgrb 1-2% of mergers (beaming) BH/NS Horizon ~930Mpc NS/NS Horizon ~440Mpc (kne detectability from Kalsiwal & Nissanke, 2014) kne (Red) kne (Blue) kne (Bright) (DT et al. in prep)
23 How detectable are EM counterparts? sgrb 1-2% of mergers (beaming) Detectable out to z~0.9 RSF (Pessimistic Fraction of Mergers ~1/10) RSF (Optimistic) Triggering (~1100 Mpc) BH/NS Horizon ~930Mpc NS/NS Horizon ~440Mpc (kne detectability from Kalsiwal & Nissanke, 2014) kne (Red) kne (Blue) kne (Bright) (DT et al. in prep)
24 SGRB Precursors Potential Orphan RSFs? ERSF ~ erg, trsf ~ 0.1s GRB T90(s) z BAT Fluence (10-7 erg cm -2 ) EBAT ISO (erg) Notes B x Fong+ High Ekin; (2016) B x10 48 Gehrels+ (2005) B x10 48 Bloom+ (2006) * x Tanvir Levan & (2008) Troja et al. ApJ, 723, 1711 (2010) *no afterglow; host galaxy within BAT error box Q: Is there a local orphan RSF component in SGRB population? (see e.g. Tanvir [2005])
25 Post-Merger Progenitor NS NS NS BH BH BH NS BH BH BH NS + Disk/Ejecta BH + Disk/Ejecta No Tidal Disruption No Matter kilo/macronovae kilo/macronovae EM Counterpart SGRB (prompt + afterglow) Cocoon emission SGRB (prompt + afterglow) Cocoon emission (DT et al. in prep)
26 Post-Merger Progenitor NS NS NS BH BH BH NS BH BH BH NS + Disk/Ejecta BH + Disk/Ejecta No Tidal Disruption No Matter kilo/macronovae kilo/macronovae EM Counterpart SGRB (prompt + afterglow) Cocoon emission RSF (prompt precursor + afterglow) SGRB (prompt + afterglow) Cocoon emission RSF (prompt precursor + afterglow) RSF (prompt precursor + afterglow) (DT et al. in prep)
27 Black Hole - Neutron Star Mergers DT et al. (in prep)
28 Summary sgrb 1-2% of mergers (beaming) Detectable out to z~0.9 RSFs caused by resonant tidal excitation of i-mode injecting energy into pair-fireball, seconds before merger RSFs are: Isotropic Bright: should be easily detectable within the LIGO horizon ERSF ~ ergs trsf ~ 0.1s Can appear as SGRB precursors or orphan RSFs (underluminous, very short GRBs) RSF (Optimistic) RSF (Pessimistic Fraction of Mergers ~1/10) Weak X-ray/Optical/Radio afterglow Triggering (~1100 Mpc) Coincident EM/GW timing will confirm RSF model and determine mode freq. Shear speed/nuclear physics constraints; Complementary to M, R, λ Does not need tidal disruption - larger fraction of NS-BH mergers kne (Red) kne (Blue) kne (Bright) NS/NS Horizon ~440Mpc BH/NS Horizon ~930Mpc
29 Questions Surface B-field - core vs crust evolution? Detectable out to z~0.9 sgrb 1-2% of mergers (beaming) N RSF/Nmerger? Excess of nearby orphan RSFs? Injection tests for burst pipelines? RSF (Pessimistic Fraction of Mergers ~1/10) How do the core-crust transition density and (effective) RSF shear modulus/speed depend on nuclear physics (Optimistic) parameters? (model dependence?) Pasta layer thickness? Triggering (~1100 Mpc) What constraints on NS EOS and dense matter can we obtain with i-mode frequency from coincident timing? BH/NS Horizon ~930Mpc kne (Red) NS/NS Horizon ~440Mpc kne (Blue) kne (Bright)
30 Questions Surface B-field - core vs crust evolution? Detectable out to z~0.9 sgrb 1-2% of mergers (beaming) N RSF/Nmerger? Excess of nearby orphan RSFs? Injection tests for burst pipelines? RSF (Pessimistic Fraction of Mergers ~1/10) How do the core-crust transition density and (effective) RSF shear modulus/speed depend on nuclear physics (Optimistic) parameters? (model dependence?) Pasta layer thickness? What constraints on NS EOS and dense matter can we Triggering (~1100 Mpc) obtain with i-mode frequency from coincident timing? Steiner & Watts, (2009), PRL, 103, BH/NS Horizon ~930Mpc kne (Red) NS/NS Horizon ~440Mpc kne (Blue) kne (Bright)
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