Population III���Gamma-Ray Burst

Kunihito Ioka (KEK) Suwa & KI arXiv:1009.6001 Nagakura+ arXiv:1104.5691 de Souza, Yoshida & KI arXiv:1105.2395 KI & Meszaros astro-ph/0408487 KI astro-ph/0309200

Population III���Gamma-Ray Burst

Kunihito Ioka (KEK) Suwa & KI arXiv:1009.6001 Nagakura+ arXiv:1104.5691 de Souza, Yoshida & KI arXiv:1105.2395 KI & Meszaros astro-ph/0408487 KI astro-ph/0309200

You can find these guys

z=6.3: GRB050904 z=6.41: Quasar z=6.7: GRB080913 z=7.085: Quasar z=8.26: GRB090423 z=8.6: Galaxy z=9.4: GRB090429B

1st Star Era!!

3

Pop III (Zero Metal) ~1000M¤(!?)

Present Day Massive Star

~20M¤

Omukai & Nishi 98; Abel+ 02; Bromm+ 02; Omukai+ 03; Yoshida+ 08; Omukai’s talk; Whalen’s talk

First stars are very MASSIVE?

Super-Massive Pop III Star?

Mini halo (first object): ~1000M¤ If all the mass is accreted to a proto-star,

4

Pop III GRB?

Present Day GRB

Komissarov & Barkov 10 Meszaros & Rees 10 Suwa & KI 11 Nagakura+ 11

Gigantic (x100) GRB @ z~10-30???

? 5

Massive Envelope

Ohkubo+ 09 Heger+ 03 Suwa & KI 10

l  No mass loss l  Accretion may ���

prevent CHE l  SN-II w/o GRB

R/c~103s > TGRB~10s ⇒ No GRB?

Core Envelope

6

Duration ~10 s ? l  Loophole: TPop III GRB~10 sec? l  Accretion ⇒ Jet l  Massive envelope���⇒ Long duration?

l  Stellar envelope���determines 1.  Jet luminosity 2.  Jet head velocity

€

˙ M

€

L j

Stellar envelope

€

vh

7

MacFadyen & Woosley 99

Penetration Problem 1.  Give the envelope profile 2.  Calculate accretion���

3.  ⇒ Lj(t)

4.  ⇒ Jet head dynamics

€

˙ M

€

L j

Stellar envelope

€

vhM t( ) = dM

dt ff, t ff ≈

r3

GMr

(calibrated by low-z GRB)

8

Penetration Problem 1.  Give the envelope profile 2.  Calculate accretion���

3.  ⇒ Lj(t)

4.  ⇒ Jet head dynamics

€

˙ M

€

L j

Stellar envelope

€

vhM t( ) = dM

dt ff, t ff ≈

r3

GMr

(calibrated by low-z GRB) Jet Lj

Envelope

Shoc

ked

Enve

lope

Shoc

ked

Jet

Con

tact

dis

cont

inui

ty

9

Bromberg’s talk

Penetration Problem 1.  Give the envelope profile 2.  Calculate accretion���

3.  ⇒ Lj(t)

4.  ⇒ Jet head dynamics

€

˙ M

€

L j

Stellar envelope

€

vhM t( ) = dM

dt ff, t ff ≈

r3

GMr

(calibrated by low-z GRB) Jet Lj

Envelope

Shoc

ked

Enve

lope

Shoc

ked

Jet

Con

tact

dis

cont

inui

ty

€

L j

πθ 2r2c~ ρ*c

2βh2

⇒ Jet head velocity

€

cβh ~cθ

L j

πc 3ρ*r2

&

' (

)

* +

1 2

Ram pressure

€

βhΓh2 ~ 0.1 Liso

1052erg/s$

% &

'

( )

1 2

×

r1012cm$

% &

'

( ) −1

ρ*

10−3g/cm3

$

% &

'

( )

−1 2

10

Suwa & KI 10

Pop III

Wolf-Reyet

Red Giant

€

L∝ ˙ M ⇒ vJet head inside the star

Core Acc. ~ a few sec

Envelope Accretion

Pop III GRB

is Possible

Envelope Accretion

11

Suwa & KI 10

Pop III

Wolf-Reyet

Red Giant

€

L∝ ˙ M ⇒ vJet head inside the star

Very long duration ~3000(1+z) sec

Long Duration

12

Suwa & KI 10

Pop III

Wolf-Reyet

Red Giant

€

L∝ ˙ M ⇒ vJet head inside the star

Very long duration ~1000(1+z) sec

Long Duration

? Long Short

Pop III

13

Suwa & KI 10

Pop III

Wolf-Reyet

Red Giant

€

L∝ ˙ M ⇒ vJet head inside the star

Energetic Eγ,iso~1055erg Modest Lγ,iso~1052erg/s

Bright phase ⇒ Cocoon

Not so Bright

14

Detectability l  Pop III GRB at z~20

l  Swift BAT sensitivity ~10-8 erg cm-2 s-1 l  Future (LOFT, HiZ-GUNDAM, …)

~10-9 erg cm-2 s-1

15

Analytic Expressions

Suwa & KI 10 16

Nagakura+ 11 2D, rela-hydro, Mass accretion from inner boundary ⇒ Jet 17

GRB jet can breakout the first star!

18

Stop Accretion?

Hosokawa+ 11; McKee & Tan 08; Omukai’s talk

HII region breakout & Photoevaporation of

the accretion disk ⇒ ~40M¤ 19

Light Pop III Star

Heger+ 03 Nagakura+ 11

Light Pop III ~40M¤

Light Pop III star also via l  Disk fragmentaion l  Pop III.2 (Z=0, from���

once-ionized gas)

Massive Pop III

20

Light Pop III GRB

1010

1011

1012

1013

1014

10 100 1000

R * [c

m]

M* [M!]

1010

1011

1012

1013

1014

10 100 1000

R * [c

m]

M* [M!]

tb"tff

vh"vcRSG

WR

lpop3

mpop3

Breakout is possible also for Light Pop III

Nagakura+ 11 Suwa & KI 10

Breakout time~Free fall time

Jet head velocity~Cocoon velocity

Analytic + Numerial 21

Schematical

Pop III.1+III.2���Star Formation Rate

: f*~0.01

f*~0.001

Trenti & Stiavelli 09

Bromm & Loeb 06

Tornatore+ 07

de Souza, Yoshida & KI 11

Our optimistic case is still conservative 22

See also Virgili, Zhang+ 11

Pop III.1. & III.2 ���GRB Rate

# (

on+

off-a

xis

GR

B) /

yr o

n th

e sk

y

f*=0.01

f*=0.1

vwind=50km/s fGRB=0.1

Pop III.2 GRB rate >> Pop III.1 GRB rate

de Souza, Yoshida & KI 11 23

Pop III.2 (Z=0, from���once-ionized gas)

Pop III.1. & III.2 ���GRB Rate

# (

on+

off-a

xis

GR

B) /

yr o

n th

e sk

y

f*=0.01

vwind=50km/s fGRB=0.1

Huge Rate!

de Souza, Yoshida & KI 11 24

f*=0.1

Radio Afterglow

KI & Meszaros 05 Inoue+ 07, Toma+ 10

K-correction ⇒ Not dim @high-z

Flux

ν

Spherical after jet break

25

Radio Transient

Bower & Saul 11 Bower+ 07 (VLA) Gal-Yam+ 06 (FIRST, NVSS)

Optimistic ~105/yr/z x (z~10) x 100day ~3x105 on the sky

Surf

ace

dens

ity

(deg

-2)

Flux (µJy) Δt ~ 1yr

We can limit Pop III GRB rate by radio transient survey

26

Radio Transient Optimistic ~105/yr/z x (z~10) x 100day ~3x105 on the sky

Surf

ace

dens

ity

(deg

-2)

Flux (µJy) Δt ~ 1yr

Bower & Saul 11 Bower+ 07 (VLA) Gal-Yam+ 06 (FIRST, NVSS)

We can limit Pop III GRB rate by radio transient survey

27

Future Radio Transient

1112.2579

Surf

ace

dens

ity

(deg

-2)

Flux (Jy)

Optimistic Case

Future: EVLA, LOFAR, SKA can survey Pop III era

28

arXiv:1112.5940

29

l  ~20GeV-100TeV l  x10 Sensitivity l  Δθ~1-2 min l  FOV~5-10 deg l  ~20 s slew (LST) l  ~2015 (?) l  ~150€

CTA

Summary l  Can GRB jets break out the first stars? –  Yes! –  Massive & Light Pop III stars –  Envelope accretion: Long, Energetic, Modest L –  Sensitive to the envelope mass

l  Pop III GRB Rate –  Pop III.2 GRB (~40M¤) > III.1 GRB –  Radio afterglow is observable up to high-z –  Radio & X-ray transient survey

30

Suwa & KI 10 Nagakura+ 11

de Souza+11 KI & Meszaros 05 KI 03