NS+NS/BH mergers: GW and em counterparts Models and observations needed
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1 NS+NS/BH mergers: GW and em counterparts Models and observations needed Kandinksy Ccomposition Kandinksy Curves and sharp angles Frédéric Daigne (Institut d Astrophysique de Paris Sorbonne Université) TS2020_II / Transient Sky 2020 National Workshop - 2nd Edition 4-6 juin 2018 Montpellier
2 NS+NS/BH mergers: GW and em counterparts Models and observations needed? TS2020_II / Transient Sky 2020 National Workshop - 2nd Edition 4-6 juin 2018 Montpellier Kandinksy Curves and sharp angles Kandinksy Ccomposition Frédéric Daigne (Institut d Astrophysique de Paris Sorbonne Université)
3 GW and counterparts
4 Remnant of a NS+NS merger Radioactively powered emission (kilonova: visible-ir) + afterglow (radio)? R-process β decay Short GRB? Afterglow (Relativistic?) ejecta -acceleration? -composition? -geometry? BH/magnetar + accretion torus -mass, spin? -Disk mass? (EOS ) Quasi-spherical ejecta (several components?)
5 Remnant of a NS+NS merger Obs. GBM Radioactively powered emission (kilonova: visible-ir) + afterglow (radio)? Θ v <28? Short GRB? Afterglow? R-process β decay The case of BH/magnetar + accretion torus -mass, spin? -Disk mass? (EOS ) Quasi-spherical ejecta (several components?) Alexander et al. 2018
6 GW
7 NS+NS/BH: GW observations needed More events: merger rates NS+BH systems? More prompt small 3D error boxes: - more em counterparts, with different viewing angle - face-on systems? (θ v < a few degrees) Post-merger GW emission: nature/evolution of the central object after the merger (BH, NS, NS BH, ) Note for the search of em counterparts. After GW170817, we know that an afterglow can be found even without a GRB. KN detection sub arcsecond localization afterglow detection/severe upper limits Maximum distance for a KN detection? GW170817: M peak ~ -15 m peak ~ 100 Mpc
8 Kilonova
9 Kilonova: at least two components? Θ v <28? Obs. Dynamical ejecta? Neutrino wind from the disk?
10 Kilonova: observations needed Better estimates of the ejected mass/composition Better understanding of the geometry of the kilonova ejectas (more events with spectro-photometric follow-up+better models) Spectroscopic signature of heavy elements? KN associated to NS+BH? - Better constraints on (D, θv) - H0: many events needed indirect constraints on the nature of the post-merger central object, (if no post-merger GW signal) via the ejected mass Drout et al., Science, 2017 Notes: GW+KN
11 Are NS+NS mergers the main astrophysical site for the production of r-process heavy elements?
12 Merger rate: BNS Post-O1 upper limits on BNS rate Pop. models Based on short GRB rates Abbott et al. 2016, post-o1
13 Merger rate: BNS Post-O1 upper limits on BNS rate Abbott et al. 2016, post-o1
14 Merger rate: BNS Model: estimate the BNS rate assuming that most of the r-process elements are produced by NS+NS mergers Observations: Eu measured in metal-poor halo stars in the Milky Way = tracer of the time evolution of the r-process Merger rate Kilonova rate Cen Vangioni, Goriely, Daigne, François & Belczynski (2016)
15 Merger rate: BNS Post-O1 upper limits on BNS rate O2 detection Abbott et al. 2016, post-o1
16 To confirme that mergers are the main contributers of r-process elements: more evidence for heavy elements formation, estimate of the ejected mass, Merger rate: BNS Post-O1 upper limits on BNS rate O2 detection Abbott et al post-o1, Abott et al post-o2
17 Short GRB
18 Short GRB GRB170817A=puzzling (not very hard, very under-luminous) Standard GRB seen off-axis unlikely (Ep would be very high if seen on-axis)
19 Short GRB: relativistic jet, seen off-axis? Θ v <28? Obs.
20 Short GRB GRB170817A=puzzling (not very hard, very under-luminous) Standard GRB seen off-axis: very unlikely (Ep would be very high if seen on-axis)
21 Short GRB: dissipation in a (mildly?)relativistic ejecta pointing towards us? Θ v <28? Obs.
22 Short GRB: emission mechanism? Observations needed GRB170817A=puzzling (not very hard, very under-luminous) GRB at 40 Mpc (Daigne & Mochkovitch 2007) Dissipation in a mildly relativistic outflow pointing towards us? (jet with lateral structure, cocoon, ) Example: internal shocks can explain the peculiar properties of GRB170817A for a low Lorentz factor/moderate kinetic energy flux Needs more detections: intensity = f(θ v )?
23 Short GRB: GW-GRB delay? Observations needed GRB170817A=puzzling (not very hard, very under-luminous is less natural if the GRB is due to a shock breakout Frequency (Hz)) is natural 1) if the relativistic ejection occurs rapidly after the merger (i.e. << s) 2) if the emission occurs above the photosphere (shocks, recon.) Count rate (cts/s) GW-GRB delay: ~burst duration Time (s) Needs more detections, with some statistics on the measured delay
24 Afterglow
25 Afterglow Alexander et al GW170817: X, V and radio : same spectral regime n m <n obs <n c Rise to maximum as ~ t 1.5 / decline confirmed at 250 days
26 Afterglow: relativistic jet, seen off-axis? Θ v <28? Obs.
27 Afterglow: relativistic jet, seen off-axis? Θ v <28? Obs. Kilonova ejectas not shown
28 Afterglow: relativistic jet, seen off-axis? Θ v <28? Obs.
29 Afterglow Afterglow of a jet seen off-axis? No acceptable fit
30 Afterglow: quasi-spherical thin ejecta pointing towards us? without a core jet Θ v <28? Obs.
31 Afterglow Afterglow of a jet seen off-axis? No acceptable fit Expanding thin quasi-spherical ejecta seen on-axis? No acceptable fit
32 Afterglow: quasi-spherical ejecta with radial structure pointing towards us? without a core jet Θ v <28? Obs.
33 Afterglow Afterglow of a jet seen off-axis? No acceptable fit Expanding thin quasi-spherical ejecta seen on-axis? No acceptable fit Expanding quasi-spherical ejecta with radial structure: OK, large degeneracy in model parameters Radio Note : multi-lambda does not help (except for p) (Duque, Mochkovitch & Daigne) E 50 (bg) m (bg) M n e B red magenta cyan blue green
34 Afterglow: ejecta with lateral structure pointing towards us? Θ v <28? Obs.
35 Afterglow Lazzati et al Afterglow of a jet seen off-axis? No acceptable fit Expanding thin quasi-spherical ejecta seen on-axis? No acceptable fit Expanding quasi-spherical ejecta with radial structure: OK Lateral structure instead of radial structure: equally good fits Here: the central jet (E iso,on ~10 52 erg) contributes at 100 days
36 Afterglow Afterglow of a jet seen off-axis? No acceptable fit Expanding thin quasi-spherical ejecta seen on-axis? No acceptable fit Expanding quasi-spherical ejecta with radial structure: OK Lateral structure instead of radial structure: equally good fits These two classes of models can apply to two different post-merger behaviors: 1. relativistic ejection is delayed, jet has to go through the blue kilonova ejecta formation of a coocon (afterglow) ; jet breakout (GRB) ; jet emerges or not 2. the whole ejection is produced at the same time after the merger, with structure in the core: ultra-relativistic jet (bright GRB if on-axis), or not intermediate latitude: mildly rel. ejecta (afterglow) with radial/lateral structure larger latitudes: blue kilonova ejecta
37 Afterglow: quasi-spherical ejecta with radial structure with a core (hidden) jet? Θ v <28? Obs.
38 Afterglow: ejecta with lateral structure with a core (hidden) jet? Θ v <28? Obs.
39 Afterglow Expanding quasi-spherical ejecta with radial structure: OK Lateral structure instead of radial structure: equally good fits Hidden central ultra-relativistic jet? Example for q j =5, q v =25, e e =0.1 (note: if q v decreases, it is more difficult to hide the jet) Log n E j =10 51 erg Log e B E j =10 52 erg Log e B (Duque, Mochkovitch & Daigne)
40 Afterglow Expanding quasi-spherical ejecta with radial structure: OK Lateral structure instead of radial structure: equally good fits Hidden central ultra-relativistic jet? Example for q j =5, q v =25, e e =0.1 Radio (Duque, Mochkovitch & Daigne)
41 Afterglow Expanding quasi-spherical ejecta with radial structure: OK Lateral structure instead of radial structure: equally good fits Hidden central ultra-relativistic jet? Example for q j =5, q v =25, e e =0.1 Radio E=10 51 erg E=10 52 erg n=10-3 cm -3, e B =10-3 (Duque, Mochkovitch & Daigne)
42 Afterglow Expanding quasi-spherical ejecta with radial structure: OK Lateral structure instead of radial structure: equally good fits Hidden central ultra-relativistic jet? Example for q j =5, q v =25, e e =0.1 Radio E=10 51 erg E=10 52 erg Possible diagnostic: polarization (maximum polarization: ~28% at ~ one year) (Duque, Mochkovitch & Daigne)
43 Afterglow: observations needed More detection, at different viewing angles! Additional diagnostics to break the radial/lateral structure degeneracy: 3 GHz: GJ: Gaussian jet PLJ: Power-law jet QSph+E inj : quasi-spherical Sph+E inj : spherical Lateral structure vs radial structure Gill & Granot 2018
44 Afterglow: observations needed More detection, at different viewing angles! Additional diagnostics to break the radial/lateral structure degeneracy: Radio afterglow imaging (VLBI) GJ: Gaussian jet PLJ: Power-law jet Lateral structure Gill & Granot 2018
45 Afterglow: observations needed More detection, at different viewing angles! Additional diagnostics to break the radial/lateral structure degeneracy: Radio afterglow imaging (VLBI) QSph+E inj : quasi-spherical Sph+E inj : spherical Radial structure Gill & Granot 2018
46 Conclusion
47 Conclusions: observations needed More GW events, with different viewing angles NS+BH? Post merger GW signal Rates More KN events, with different viewing angles (change in color? Intensity?) Universal? NS+BH? Statistics: ejected mass? Composition? Spectroscopic signature of r-process elements? More GRBs, with different viewing angles (change in intensity? Hardness? No GRB?) Better description of lightcurve+spectrum Statistics: GW-GRB delay More afterglows, with different view angles (different components?) Polarization? Imaging (radio afterglow: VLBI?)
48 Conclusions: not discussed here Variability in the afterglow (flares?) Indirect constraints on the nature of the post-merger central object Information brought from the study of the host galaxy/source environment Cosmology/Fundamental physics Modelling tools at IAP: - Short GRB: detailed internal shock model - Afterglow: detailed model - fitting procedure - radial/lateral structure - polarization - soon: imaging - soon: reverse shock emission - Kilonova: very naive model
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