Are Ultralong Grbs Caused by Blue Supergiant Explosions, Newborn

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Are Ultralong GRBs Caused by Blue Supergiant Explosions, Newborn Magnetars, White Dwarf Tidal Disruption Events? Kunihito Ioka (Center for Gravitational Physics, YITP, Kyoto U.) with Kenta Hotokezaka (Hebrew) Tsvi Piran (Hebrew)

arXiv: 1608.02938 ApJ 833, 110 (2016) 2017/01/24 ultralong GRB & TDE by K. Ioka 2 Summary Supernova(-like Event)

Lbol (Greiner+15) ]

-1 L using unbroken afterglow Collapsar 44 bol 10 PS1-11af (TDE)

PTF11rks (SLSN)

1043 98bw (SN)

Explosion 52 4 9 -1 Ei=1.4×10 erg, ti=1×10 s, M=3 M , v=2×10 cm s , =0.2 ⊙ 2 Magnetar H=(E/te)/(1+t/te) 50 6 9 -1 E=1.4×10 erg, te=1.1×10 s, M=2.2 M , v=2×10 cm s , =0.04 42 ⊙ 5/3 Bolometric luminosity [erg s 10 Tidal Disruption Event H=(2E/3te)/(1+t/te) 50 5 9 -1 E=2.4×10 erg, te=2×10 s, M=1 M , v=2×10 cm s , =0.2 ⊙ 0 10 20 30 40 50 Rest-frame time after explosion [days] 2017/01/24 ultralong GRB & TDE by K. Ioka 3 Summary Supernova(-like Event)

Lbol (Greiner+15) ]

-1 L using unbroken afterglow Collapsar 44 bol 10 PS1-11af (TDE)

PTF11rks (SLSN)

1043 98bw (SN) Explosion Magnetar 52 4 9 -1 Ei=1.4×10 erg, ti=1×10 s, M=3 M , v=2×10 cm s , =0.2 ⊙ 2 Magnetar H=(E/te)/(1+t/te) 50 6 9 -1 E=1.4×10 erg, te=1.1×10 s, M=2.2 M , v=2×10 cm s , =0.04 42 ⊙ 5/3 Bolometric luminosity [erg s 10 Tidal Disruption Event H=(2E/3te)/(1+t/te) 50 5 9 -1 E=2.4×10 erg, te=2×10 s, M=1 M , v=2×10 cm s , =0.2 ⊙ 0 10 20 30 40 50 Rest-frame time after explosion [days] 2017/01/24 ultralong GRB & TDE by K. Ioka 4 Summary Supernova(-like Event)

Lbol (Greiner+15) ]

-1 L using unbroken afterglow Collapsar 44 bol 10 PS1-11af (TDE)

PTF11rks (SLSN)

1043 98bw (SN) Explosion Magnetar 52 4 9 -1 Ei=1.4×10 erg, ti=1×10 s, M=3 M , v=2×10 cm s , =0.2 ⊙ 2 Magnetar H=(E/te)/(1+t/te) 50 6 9 -1 E=1.4×10 erg, te=1.1×10 s, M=2.2 M , v=2×10 cm s , =0.04 42 ⊙ 5/3 Bolometric luminosity [erg s 10 Tidal Disruption Event H=(2E/3te)/(1+t/te) 50 5 9 -1 E=2.4×10 erg, te=2×10 s, M=1 M , v=2×10 cm s , =0.2 + Tidal ⊙ 0 10 20 30 40 50 Disruption Rest-frame time after explosion [days] Event 2017/01/24 ultralong GRB & TDE by K. Ioka 2 Diversity of GRB Ultra-long GRB

GRB 130925A

Low-Luminosity GRB

Magnetar Tidal Levan+ 14 Disruption Gendre+ 13 Lien+ 16 Event 2017/01/24 ultralong GRB & TDE by K. Ioka Nakauchi+2 13 Kashiyama+ 13 Suwa & KI 11 Collapsar? Nagakura+ 12 Ultra-long GRB

GRB 130925A

Low-Luminosity GRB

Magnetar Tidal Levan+ 14 Disruption Gendre+ 13 Lien+ 16 Event 2017/01/24 ultralong GRB & TDE by K. Ioka 7 Pop III GRB?

Present Day GRB

Komissarov & Barkov 10 ? Meszaros & Rees 10 Suwa & KI 11 Nagakura, Suwa & KI 12

Envelope accretion ⇒ Ultra-long 2017/01/24 ultralong GRB & TDE by K. Ioka 8 Cooling Envelope? z=0.677

Blue supergiant (BSG)

M=75M¤, Z=1e-4Z¤, R=8.6e12cm Ec=1e53 erg, Mc=5.8M¤ Cocoon thermal emission Nakauchi+ 13, 12; Kashiyama+ 13 ≈ Superluminous supernova 2017/01/24 ultralong GRB & TDE by K. Ioka 2 Levan+ 14 Gendre+ 13 TDE? MacLeod+ 14 Ultra-long GRB

GRB 130925A

Low-Luminosity GRB

Magnetar Tidal Levan+ 14 Disruption Gendre+ 13 Lien+ 16 Event 2017/01/24 ultralong GRB & TDE by K. Ioka 10 Swift J1644+57

~t-5/3

tvar~100sec ﬂare~103-4sec quiescent~5x104s Burrows+ 11 duration~107s 2017/01/24 ultralong GRB & TDE by K. Ioka 11 ULGRB = TDE?

Similar? Dissimilar?

Evans+ 14 2017/01/24 ultralong GRB & TDE by K. Ioka 12 White Dwarf TDE

⎛ ⎞2 3 ⎛ ⎞−1 3 M BH 12 M* amin ~ ⎜ ⎟ R* ~ 10 cm⎜ ⎟ ⎝ M* ⎠ ⎝ M8 ⎠ ⎛ ⎞2 3 ⎛ ⎞−1 3 M BH ρ* ×⎜ 5 ⎟ ⎜ 6 −3 ⎟ ⎝10 M8 ⎠ ⎝10 g cm ⎠ 1 2 3 ⎛ ⎞− amin 3 M* t0 ~ 2π ~ 4 ×10 sec⎜ ⎟ GM BH ⎝ M8 ⎠ 1 2 −1 2 ⎛ M ⎞ ⎛ ρ ⎞ × BH * a ⎜ 5 ⎟ ⎜ 6 −3 ⎟ min ⎝10 M8 ⎠ ⎝10 g cm ⎠ Ultra-long duration requires WD density Krolik & Piran 11 2017/01/24 ultralong GRB & TDE by K. Ioka 2

Magnetar? Greiner+ 15 Ultra-long GRB

GRB 130925A

Low-Luminosity GRB

Magnetar Toma+ 07 Tidal Levan+ 14 Disruption Gendre+ 13 Lien+ 16 Event 2017/01/24 ultralong GRB & TDE by K. Ioka 14 Supernova Component?

Even brighter than SN1998bw (hypernova)?

Against TDE model? Really supernova? Levan+ 14 2017/01/24 ultralong GRB & TDE by K. Ioka 15 Bright SN 2011kl

~10 days after GRB 111209 GROND multiband X-shooter on VLT Supernova ⇒ TDE × No H line ⇒ BSG × ⇒ Magnetar? Greiner+ 15 2017/01/24 ultralong GRB & TDE by K. Ioka 16 Spectrum X-shooter spectrum − GRB afterglow − host galaxy

Supernova ⇒ TDE × No H line ⇒ BSG × ⇒ Magnetar

No Ca II, C II lines ⇒ v>2e9 cm/s

Greiner+ 15 2017/01/24 ultralong GRB & TDE by K. Ioka 17 SN does not Exclude TDE

Half bound Half unbound

Super-Eddington ⇒ Disk outﬂow, γ ⇒ E into Ejecta ⇒ SN-like bump

KI, Hotokezaka & Piran 16 2017/01/24 ultralong GRB & TDE by K. Ioka 18 Light Curve Modeling One zone Arnett 79, 82 3 Kasen & Bildsten 10 V ∝ R Dexter & Kasen 13 ∂E ∂V E int p = int = −p + H (t) + L(t) 3V t t ∂ ∂ v = R! L t c ∂ E V c E V ( ) = ( int ) ≈ int 4π R2 3κρ ∂R 3κρ R ! d t $ t Diffusion time # + 2 &L(t) = 2 H (t) " dt td % td t2 3κM − 2 2 t( 2td t = e t 2 d L t = dt( t(e 2td H t( 4πcv ( ) 2 ∫ 0 ( ) td 2017/01/24 ultralong GRB & TDE by K. Ioka 19 SN-like Light Curve

Lbol (Greiner+15) ] GM BH (M* 2)

-1 L using unbroken afterglow 44 bol E ~ 10 PS1-11af (TDE) 2amin 51 PTF11rks (SLSN) ~ 4 ×10 erg 43 −1 L ~ LEdd ~ 10 erg s 43 ⎛ ⎞ 10 M BH 98bw (SN) ×⎜ 5 ⎟ ⎝10 M8 ⎠ Explosion 52 4 9 -1 Ei=1.4×10 erg, ti=1×10 s, M=3 M , v=2×10 cm s , =0.2 GM BH ⊙ 2 v ~ Magnetar H=(E/te)/(1+t/te) min 50 6 9 -1 E=1.4×10 erg, te=1.1×10 s, M=2.2 M , v=2×10 cm s , =0.04 2amin 42 ⊙ 5/3 Bolometric luminosity [erg s 10 Tidal Disruption Event H=(2E/3te)/(1+t/te) 50 5 9 -1 9 −1 E=2.4×10 erg, te=2×10 s, M=1 M , v=2×10 cm s , =0.2 ~ 2 10 cm s ⊙ × 0 10 20 30 40 50 Rest-frame time after explosion [days] KI, Hotokezaka & Piran 16 2017/01/24 ultralong GRB & TDE by K. Ioka 20 Multi-band Lightcurve 1

18 u 19 g r 20 i z 21

22 Magnetar 2

AB magnitude 23 H=(E/te)/(1+t/te) 50 E=1.4×10 erg 6 24 te=1.1×10 s M=2.2 M 9 ⊙ -1 Caveat 25 v=2×10 cm s =0.04 Ekin >> Einj 26 4 5 6 7 ~0.04 10 10 10 10 κ Observer time after burst trigger [s] 2017/01/24 ultralong GRB & TDE by K. Ioka 21 Multi-band Lightcurve 2

18 u 19 g r 20 i z 21

22 Blue Supergiant

AB magnitude 23 52 Ei=1.4×10 erg 4 24 ti=1×10 s M=3 M ⊙9 -1 25 v=2×10 cm s =0.2 Caveat 26 4 5 6 7 10 10 10 10 Ekin >> Einj Observer time after burst trigger [s] 2017/01/24 ultralong GRB & TDE by K. Ioka 22 Multi-band Lightcurve 3

18 u 19 g r Power-law AG 20 i z (Not broken PL) 21 ⇒ Different Lbol 22 Tidal Disruption Event 5/3

AB magnitude 23 H=(2E/3te)/(1+t/te) 50 E=2.4×10 erg 5 24 te=2×10 s M=1 M ⊙9 -1 25 v=2×10 cm s =0.2 26 104 105 106 107 Observer time after burst trigger [s] 2017/01/24 ultralong GRB & TDE by K. Ioka 23 Peculiar Magnetar l Spindown time should be tuned to tpeak 3 −2 2 6Ic 6 $ B ' $ P ' te = ≈ 1.1×10 s& ) & ) B2 R6Ω2 % 7.5×1014 G ( %12.2ms( >> tGRB See also Cano, Johansson & Maeda 16 l Radiation energy Bersten+ 16 1 E = IΩ2 ≈ 1.3×1050 erg rot 2 << Kinetic energy Mv2/2 l How to explain GRB? Not simple 2017/01/24 ultralong GRB & TDE by K. Ioka 24 Tidal Disruption Event?

• Supernova: might be • GRB timescales ⇒ WD TDE • Energy ⇒ WD has enough mass • Super-Eddington ⇒ Jet • Event rate ~3e-6/yr ⇒ consistent • Light curve L~t-5/3 • Host galaxies 2017/01/24 ultralong GRB & TDE by K. Ioka 25 Host Galaxies

• faint, compact, and highly star forming dwarf galaxies, typical of "blue compact galaxies”

For WD TDE 6 MBH<10 M¤

M-σ relation 2017/01/24 ultralong GRB & TDE by K. Ioka 26 Host Galaxies

• Position in the host

2 2 2 !150pc $ ! 250pc $ ! 600pc $ # & ⋅# & ⋅# & ~ 0.0005 " 600pc% " 700pc% " 2400pc% 2017/01/24 ultralong GRB & TDE by K. Ioka 27

⇔ KI+ 1608.02938 2017/01/24 ultralong GRB & TDE by K. Ioka 28 Summary Supernova(-like Event)

Lbol (Greiner+15) ]

-1 L using unbroken afterglow Collapsar 44 bol 10 PS1-11af (TDE)

PTF11rks (SLSN)

1043 98bw (SN) Explosion Magnetar 52 4 9 -1 Ei=1.4×10 erg, ti=1×10 s, M=3 M , v=2×10 cm s , =0.2 ⊙ 2 Magnetar H=(E/te)/(1+t/te) 50 6 9 -1 E=1.4×10 erg, te=1.1×10 s, M=2.2 M , v=2×10 cm s , =0.04 42 ⊙ 5/3 Bolometric luminosity [erg s 10 Tidal Disruption Event H=(2E/3te)/(1+t/te) 50 5 9 -1 E=2.4×10 erg, te=2×10 s, M=1 M , v=2×10 cm s , =0.2 + Tidal ⊙ 0 10 20 30 40 50 Disruption Rest-frame time after explosion [days] Event 2017/01/24 ultralong GRB & TDE by K. Ioka 29 宿題

-3 3 • Event rate ~ 10 RSN ~ 1/(200Mpc) /yr • ~17.5 mag @200Mpc • ~19 mag @400Mpc • ~10000 deg2/40000 deg2 ~ 1/4 • ~17.5 mag までで ~¼ event/yr • ~19 mag までで ~1 event/yr • 多分 off-axis ul-GRB • 母銀河は小さい、核付近で起こる • λ/Δλ 3.8m > λ/Δλ GROND multiband

2017/01/24Direct Collapseultralong GRB & TDE by K. Ioka BHs can 30 Launch GRBs? 9 10 M¤ BH @z>6 Super-Edd. accretion? or DCBH?

GRB jets break out the star?

Matsumoto+ 15

2017/01/24 Ultra-Luminousultralong GRB & TDE by K. Ioka 31 Supernova

Jet ⇒ Cocoon ~1045-46 erg/s for ~300 days

Matsumoto+ 16 2017/01/24 ultralong GRB & TDE by K. Ioka 32 H, Carbon-Oxygen Lines

• X-ray is observed at t~10 day • We can show that H,CO is highly ionized • Absence of H,CO line is not a problem 2017/01/24 ultralong GRB & TDE by K. Ioka 33 Waxman’s talk Wang’s talk HE ν? Meszaros’s talk TeV-PeV ν from Low-power GRB Jets inside Stars Ultra-long GRB, Low-luminosity GRB Murase & KI PRL13 l Γβ dec Stellar envelope Jet head Collimated jet Collimation Radiation shock x Internal shocks Coccon Pre-collimated jet 2017/01/24 ultralong GRB & TDE by K. Ioka 34

2017/01/24GRB Jetsultralong can GRB & TDE by K.Break Ioka Out 35 Supermassive Stars Radiation pressure- dominated ⇒ Breakout

Total energy ~1055-56 erg

~Mhalo vesc vc ⇒ Expel the host galaxy?

Matsumoto+ 15