B03 progress report (2) Kilonova models for GW Masaomi Tanaka (Na$onal Astronomical Observatory of Japan)

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Horatio Harrell
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1 B03 progress report (2) Kilonova models for GW Masaomi Tanaka (Na$onal Astronomical Observatory of Japan)

2 B03 progress report (2) Kilonova models for GW Kilonova models Lessons learned from GW170817

3 L Kilonova/Macronova" IniGal works: Li & Paczynski 98, Kulkarni 05, Metzger+10, Goriely+11, High opacity: Kasen+13, Barnes & Kasen 13, MT & Hotokezaka 13, See Kenta s talk L peak t peak t Timescale t peak = 3 M ej 4 cv 1/2 bound-bound transigons of heavy elements 8.4 days M ej 0.01M 1/2 v 0.1c 1/2 10 cm 2 g 1 1/2 Luminosity L peak = L dep (t peak ) *assuming 50% thermalizagon erg s 1 M ej 0.01M 0.35 v 0.1c cm 2 g

4 open s shell (l=1) open p-shell (l=2) 5 4 open d-shell (l=3) E (ev) Fe II 3 E (ev) 2 1 Nd II 0 open f shell (l=4)

5 open s shell (l=1) Kasen+13: Sn II, Ce II-III, Nd I-IV, Os II Fontes+17: Ce I-IV, Nd I-IV, Sm I-IV, U I-IV Wollaeger+17: Se, Br, Zr, Pd, Te MT+17: Se I-III, Ru I-III, Te I-III, Nd I-III, Er I-III open p-shell (l=2) open d-shell (l=3) 1st peak 2nd peak 3rd peak open f shell (l=4)

6 Atomic structure calculagons HULLAC code (Bar-Shalom+99) GRASP2K code (Jonsson+13) H DC = N i=1 ( cαi p i +(β i 1)c 2 + V N i ) + N i>j 1 r ij, Ion Configurations Number of levels Number of lines Se I-III (Z=34, p) Ru I-III (Z=44, d) Te I-III (Z=52, p) Nd I-III (Z=60, f) Er I-III (Z=68, f) HULLAC Se i 4s 2 4p 4,4s 2 4p 3 (4d, 4f, 5 8l), 4s4p 5,4s4p 4 (4d, 4f), ,168 4s 2 4p 2 (4d 2, 4d4f, 4f 2 ), 4s4p 3 (4d 2, 4d4f, 4f 2 ) Se ii 4s 2 4p 3,4s 2 4p 2 (4d, 4f, 5 8l), 4s4p 4,4s4p 3 (4d, 4f), ,911 4s 2 4p(4d 2, 4d4f, 4f 2 ), 4s4p 2 (4d 2, 4d4f, 4f 2 ) Se iii 4s 2 4p 2,4s 2 4p(4d, 4f, 5 8l), 4s4p 3,4s4p 2 (4d, 4f), ,132 4s 2 (4d 2, 4d4f, 4f 2 ), 4s4p(4d 2, 4d4f, 4f 2 ) Ru i 4d 7 5s, 4d 6 5s 6, 4d 8,4d 7 (5p, 5d, 6s, 6p), 1, ,476 4d 6 5s(5p, 5d, 6s) Ru ii 4d 7,4d 6 (5s 5d, 6s, 6p) ,592 Ru iii 4d 6,4d 5 (5s 5d, 6s) ,066 Te i 5s 2 5p 4, 5s 2 5p 3 (4f, 5d, 5f, 6s 6f, 7s 7d, 8s), ,482 5s5p 5 Te ii 5s 2 5p 3, 5s 2 5p 2 (4f, 5d, 5f, 6s 6f, 7s 7d, 8s), 253 9,167 5s5p 4 Te iii 5s 2 5p 2, 5s 2 5p(5d, 6s 6d, 7s), 5s5p Nd i 4f 4 6s 2, 4f 4 6s(5d, 6p, 7s), 4f 4 5d 2, 4f 4 5d6p, 31,358 70,366, f 3 5d6s 2,4f 3 5d 2 (6s, 6p), 4f 3 5d6s6p Nd ii 4f 4 6s, 4f 4 5d, 4f 4 6p, 4f 3 6s(5d, 6p), 6,888 3,951,882 4f 3 5d 2,4f 3 5d6p Nd iii 4f 4,4f 3 (5d, 6s, 6p), 4f 2 5d 2,4f 2 5d(6s, 6p), ,161 4f 2 6s6p Er i 4f 12 6s 2, 4f 12 6s(5d, 6p, 6d, 7s, 8s), 10,535 9,247,777 4f 11 6s 2 (5d, 6p), 4f 11 5d 2 6s, 4f 11 5d6s(6p, 7s) Er ii 4f 12 6s, 4f 12 (5d, 6p), 4f 11 6s 2,4f 11 6s(5d, 6p), 5,333 2,432,665 4f 11 5d 2,4f 11 5d6p Er iii 4f 12,4f 11 (5d, 6s, 6p) ,671 GRASP

7 Bound-bound opaciges of lanthanide elements Fe (d shell) Nd (f shell) Er (f shell) Fe (Kurucz) Nd (HULLAC) Er (HULLAC) Opacity (cm 2 g -1 ) Wavelength (angstroms) MT+17 κ (p shell) << κ (d shell) << κ (f shell)

8 Expected light curves of kilonova L ~ erg s -1 t ~ weeks NIR > OpGcal Smooth spectra Absolute magnitude OpGcal NIR g r i z J H K (high velocity) -10 Kasen+13, Barnes & Kasen 13 MT & Hotokezaka 13, MT+14, Days after the merger

9 Y e = n e n p + n n = n p n p + n n - Low Ye => stronger r-process - Neutrino absorpgon increases Ye higher T higher Ye ν e + n -> p + e - n + e + -> ν e + p ν d p s f Se Ru Te Nd Er Ye = 0.30 Ye = 0.25 Ye = Mass fraction Atomic number

10 Nucleosynthesis are imprinted in the spectra Blue kilonova High Ye (Ye = 0.30) (Lanthanide-free) Medium Ye (Ye = 0.25) Low Ye (Ye = 0.1) Luminosity (erg s 1 Å 1 ) days days days days Red kilonova days MT Wavelength (Å)

11 B03 progress report (2) Kilonova models for GW Kilonova models Lessons learned from GW170817

12 GW170817: light curves NIR g ri Single component model - Mej = 0.03 Msun - <v> = 0.1c - Ye = 0.25 Model: MT+17b Observed magnitude z J H K Absolute magnitude Data: Utsumi, MT+17, Drout+17, Pian+17, Arcavi+17, Evans+17, Smarc+17, Diaz+17, Valen$+17, Cowperthwaite+17, Tanvir+17, Troja+17, Kasliwal OpGcal Days after GW Ejecta mass (La-rich) ~0.03 Msun => post-merger ejecta?

13 GW170817: Spectra Smooth spectra Smoking gun for v >~ 0.1c Spectra taken w/ VLT/X-shooter Data: Pian+ (MT), 2017 Model: MT+2017

14 Presence of blue kilonova Cowperthwaite et al. 2017; Drout et al. 2017; Nicholl et al. 2017; Villar et al Ye = 0.25 Ye = 0.1 MT+2017 Mej (blue) ~ 0.02 Msun too much for dynamical ejecta? => wind? But v ~ 0.2c (difficult with wind ejecta)

15 Origin of r-process elements GW Kilonova Rosswog+17 Hotokezaka+15, 18 SN rate Total amount seems to be OK but we do not now relagve fracgons of A > 80 or A > 130

16 Open quesgons Origin of high ejecta mass? Origin of high-velocity component in the early phase? Origin of blue and red component? Rela$ve frac$on? Similar to solar abundances?? 3rd peak?? (Au and Pt!) See Shinya s talk High Mej High v in early phase Blue Red Dynamical ejecta?? Disk wind?

17 X(Lan) ~ 0.01 or Ye ~ 0.25 MT+17b, Drout+17, Pian+17, Arcavi+17, Evans+17, Smarc+17, Cowperthwaite+17, Troja+17, Kasliwal X(La + Ac) at 1 day Y e

18 Summary RadiaGve transfer simulagons Construc$on of atomic data Predic$ons for kilonova GW Red and blue components => Ye ~ 0.25 or X(Lan) ~ if single component ~0.03 Msun ejec$on with Lanthanide => Enough to explain the origin of r-process elements Open quesgons/on-going works Abundance partners (frac$on of blue/red components) Mul$-D models and predic$on for future events

Opaci-es of and light curves of kilonovae. Masaomi Tanaka (Na-onal Astronomical Observatory of Japan)

Opaci-es of and light curves of kilonovae Masaomi Tanaka (Na-onal Astronomical Observatory of Japan) r-band magnitude @ 100 Mpc Mej = 0.01 Msun -16 19 r-band Absolute magnitude -15-14 -13-12 -11 NS-NS