The Cocoon emission in the early macronova in …Beyond r-process: The Cocoon emission in the early...

Beyond r-process: The Cocoon emission in the

early macronova in GW170817

Hamid Hamidani, Kunihito Ioka, & Kenta Kiuchi

2019年5月22日 ̶24日原子核物理でつむぐrプロセス

ReviewFernandez Metzger 2016

This study Late ObservationsNumerical Relativity

Jet propagation in an expanding ejecta

• 1

HH+19 in prep

Motivation• Engine powered “Cocoon”:

What EM counterparts/signature to be expected?

Credit: Kasliwal+17

Tool I. Numerical Simulations

Velocity Density

β = β2r + β2

θ log10(ρ)

Tool II. Analytic Modeling

MNRAS 000, 1–3 (2018) Preprint 13 August 2018 Compiled using MNRAS LATEX style file v3.0

The propagation of relativistic jets in an expanding ejecta

Hamid Hamidani?, Kunihito Ioka, and Kenta Kiuchi

Yukawa Institute for Theoretical Physics, Kyoto University, Kyoto 606-8502, Japan

Last updated 2018 August 30

ABSTRACT...

Key words: gamma-ray: burst – hydrodynamics – relativistic processes – shockwaves – ISM: jets and outflows – supernovae: general

1 INTRODUCTION

Gamma-Ray Bursts (GRBs) are ... ...The numerical simulations were carried-out using

CFCA X30. In total, this study consumed about ??? 000core-hours of computing time.

This paper is organized as follows: In § 2, we. In § 3, we. In § ??, we . Results are presented and discussed in § 4. Aconclusion is given at the end of this paper (§ 5).

2 NUMERICAL METHOD

We...

3 SETUP OF THE SIMULATIONS

3.1 Stellar model

...

3.2 Grid

4 RESULTS

4.1 ???

5 CONCLUSION

Using a 2D hydrodynamical relativistic code...

(i) aaaa(ii) bbbb

Considering the above results ...

? E-mail: [email protected]

ACKNOWLEDGEMENTS

We gratefully thank. This research was supported by theMEXT of Japan, for which we are gratefully thankful. Nu-merical computations were carried out on Cray XC30 atCenter for Computational Astrophysics, National Astro-nomical Observatory of Japan. This work has been partlysupported by Grants-in-Aid for Scientific Research (??????)from Japan Society for the Promotion of Science and Grant-in-Aid for Scientific Research on Innovative Areas (??????)from the MEXT in Japan.

APPENDIX A: THE ANALYTICAL MODEL

Here we prsent the analytical model for a relativistic jet,powered by the central engine, and expanding in a givenmedium (or ejecta). The shock jump conditions can be writ-ten as (refer to Bromberg et al. 2011; and, Ioka & Nakamura2017):

hj⇢jc2�2

j�2j + Pj = he⇢ec

2�e�2e + Pe (A1)

Both Pe and Pj can be neglected. Hence, we can writethe jet head velocity as it follows:

�h =�j � �e

1 + L̃�1/2+ �e ' L̃1/2 + �e (A2)

Where L̃ is the ratio of energy density between the jetand the ejecta.

L̃ =hj⇢j�

2j

he⇢e�2e' Lj

⌃j⇢ec3(A3)

⌃j is the jet cross section. Assuming ✓j as the jet open-ing angle, ⌃j = 4⇡✓2j r

2j . We assume that the jet opening

angle is roughly constant: ✓j ' ✓0.

A1 Case 1: Static ejecta

For a static medium (or ejecta) case, �e ' 0 and �j ' 1.Equation A2 can be simplified to the following:

c� 2018 The Authors

Gives: Jet head motion

Cocoon (E, M, <v>)






ABSTRACT...


1 INTRODUCTION




2 NUMERICAL METHOD

We...


3.1 Stellar model

...

3.2 Grid

4 RESULTS

4.1 ???

5 CONCLUSION


(i) aaaa(ii) bbbb



ACKNOWLEDGEMENTS




hj⇢jc2�2


2�e�2e + Pe (A1)


�h =�j � �e

1 + L̃�1/2+ �e ' L̃1/2 + �e (A2)


L̃ =hj⇢j�

2j

he⇢e�2e' Lj

⌃j⇢ec3(A3)







Ram Pressure Balance

Engine Ejecta

Tool II. Analytic Modeling






ABSTRACT...


1 INTRODUCTION




2 NUMERICAL METHOD

We...


3.1 Stellar model

...

3.2 Grid

4 RESULTS

4.1 ???

5 CONCLUSION


(i) aaaa(ii) bbbb



ACKNOWLEDGEMENTS




hj⇢jc2�2


2�e�2e + Pe (A1)


�h =�j � �e

1 + L̃�1/2+ �e ' L̃1/2 + �e (A2)


L̃ =hj⇢j�

2j

he⇢e�2e' Lj

⌃j⇢ec3(A3)







drh(t)dt

+ (−vej

rm(t) ) rh(t) = Arm(t)3 − n2 rh(t)

n − 22

drh(t)dt

= Arh(t)n − 2

2 Static medium

Expanding medium

A = (r3−nm,0 − r3−n

0

(3 − n)r3−nm,0 ) (

4Lj

θ2j Mejc )

0.0E+00

5.0E+08

1.0E+09

1.5E+09

2.0E+09

0 0.05 0.1 0.15 0.2 0.25

r h(t)

[cm

]

t – t0 [s]

n=0 (A) n=0 (S)

n=1 (A) n=1 (S)

n=2 (A) n=2 (S)

rm(t)

vej = 0.1c

0.0E+00

5.0E+08

1.0E+09

1.5E+09

2.0E+09

2.5E+09

3.0E+09

0 0.05 0.1 0.15 0.2 0.25 0.3r h

(t) [c

m]

t – t0 [s]

n=0 (A) n=0 (S)

n=1 (A) n=1 (S)

n=2 (A) n=2 (S)

rm(t)

vej = 0.2c

I. Analytic Vs. Numerical Breakouts

HH+19 in prep

Results I: Engine parameters and jet dynamics

vb = A rb + vej

tb − t0 =r

4 − n2

m,0 − r4 − n

20

r4 − n

2m,0

vej

(4 − n)A+

rm,0

vej

2

−rm,0

vej

A = (r3−nm,0 − r3−n

0

(3 − n)r3−nm,0 ) (

4Liso,0

Mejc )

1.E+48

1.E+49

1.E+50

1.E+51

1.E+52

1.E+53

1.E+54

0.001 0.010 0.100 1.000

L iso

,0 [e

rg s-1

]

t0 – tm [s]

tb – t0 = 1s

vb /vej = 2 (Ioka Nakamura 2017)

vb ~ c Relativistic Breakout

vb /vej = 1.6

tb – t0 = 0.1s

tb – t0 = 0.01s

Results I: Engine parameters and jet dynamics

Engine collapse/activation time

Engine Power

II. Application for GW170817’s Cocoon

Modeling The Cocoon

Ein = 3PcVc

Ec = Ein + Ek,e

Ein = Lj(tb − t0)(1 − 1/c × Rb/(tb − t0))

Approximations/Assumptions:

β⊥ =Pc

ρa (rh) c2

Ec, Mc, & ⟨βc⟩Gives:

Results I: GW170817’s Cocoon (preliminary)

1.E+48

1.E+49

1.E+50

1.E+51

1.E+52

1.E+53

1.E+54

0.001 0.010 0.100 1.000

L iso

,0 [e

rg s-1

]

t0 – tm [s]

Mc = 1.1×10 -4M

⨀ <"c>

energy = 0.27

Narrow Jet (#0=6.8º)

Delay ⩽ 1.7s

Delay > 1.7s

tb – t0 = 1s

GW170817 (VLBI)

~50% of sGRBstb – t0 ≲ Median(T90)

GW170817:Delay = 1.7s

(Numerical relativity)for Mej ≳ 0.01M⨀

vb ~ c


Relativistic Breakout

vb /vej = 1.6

tb – t0 = 0.1s

tb – t0 = 0.01s

Mc = 1.2×10 -4 M

⨀ <"c>energy = 0.27

Mc = 1.2×10 -4 M

⨀ <"c>energy = 0.29

Mc = 1.1×10 -4 M⨀ <"

c>energy = 0.30

Results I: GW170817’s Cocoon (preliminary)

1.E+48

1.E+49

1.E+50

1.E+51

1.E+52

1.E+53

1.E+54

0.001 0.010 0.100 1.000

L iso

,0 [e

rg s-1

]

t0 – tm [s]

Mc = 4 ×10 -4 M⨀ <"

c>energy = 0.29

Wide Jet (#0=18.0º)

Delay ⩽ 1.7s

Delay > 1.7s

tb – t0 = 1s

GW170817 (VLBI)

~50% of sGRBstb – t0 ≲ Median(T90)

GW170817:Delay = 1.7s

(Numerical relativity)for Mej ≳ 0.01M⨀

vb ~ c


Relativistic Breakout

vb /vej = 1.6

tb – t0 = 0.1s

tb – t0 = 0.01s

Mc = 4.2 ×10 -4 M⨀ <"

c>energy = 0.29

Mc = 4.2 ×10 -4 M⨀ <"

c>energy = 0.34

Mc = 4 ×10 -4 M

⨀ <"c>energy = 0.34

The EM Counterparts & The Cocoon

Photospheric Velocity (preliminary)

0.2

0.3

0.4

0 0.5 1

v/c

Time since GW170817 [day]

Delay ≥ 1.7s(VLBI)

GW170817's

<!c>

"0 = 1º

"0 = 3.4º

"0 = 9º

"0 = 20º

# = 1 cm2 g -1

0.1

0.2

0.3

0.4

0 1 2 3 4 5

v/c


GW170817's Cocoon

! = 1 cm2 g -1

! = 0.3 –3 cm2 g -1

EE, and Plateau Emission

Kisaka+17

The Different Cocoons (preliminary)

HH+19 in prep

1E+39

1E+40

1E+41

1E+42

1E+43

1E+44

0 1 2 3

L bl[

erg

s-1]


GW170817 GW170817 [Waxman+17] R-process [Kisaka+15] Prompt [1e51 erg/s ×~2s] Narrow Prompt [1e51 erg/s ×~2s] Wide EE [1e49 erg/s ×~100s] Narrow EE [1e49 erg/s ×~100s] Wide Plateau [1e46 erg/s ×~1e4s] Narrow Plateau [1e46 erg/s ×~1e4s] Wide

1E+39

1E+40

1E+41

1E+42

1E+43

1E+44

0 1 2 3

L bl[

erg

s-1]


GW170817 [Kasliwal+17 & Drout+17] GW170817 [Waxman+17] R-process Emission [Kisaka+15] Prompt Phase's Cocoon [Narrow Jet] Prompt Phase's Cocoon [Wide Jet] Extended Phase's Cocoon [Narrow Jet] Extended Phase's Cocoon [Wide Jet] Plateau Phase's Cocoon [Narrow Jet] Plateau Phase's Cocoon [Wide Jet]

The Cocoon outshining R-process (preliminary)

-20

-18

-16

-14

-12

-10

-8

-6

13

15

17

19

21

23

25

270 1 2

MA

B

mA

B (D

=40M

pc)


GW170817 R-process [Kisaka+15] Prompt [1e51 erg/s ×~2s] Narrow Prompt [1e51 erg/s ×~2s] Wide EE [1e49 erg/s ×~100s] Narrow EE [1e49 erg/s ×~100s] Wide Plateau [1e46 erg/s ×~1e4s] Narrow Plateau [1e46 erg/s ×~1e4s] Wide

J-Band

HH+19 in prep

-20

-18

-16

-14

-12

-10

-8

-6

13

15

17

19

21

23

25

270 1 2

MA

B

mA

B (D

=40M

pc)


GW170817 [Kasliwal+17 & Drout+17] R-process Emission [Kisaka+15] Prompt Phase's Cocoon [Narrow Jet] Prompt Phase's Cocoon [Wide Jet] Extended Phase's Cocoon [Narrow Jet] Extended Phase's Cocoon [Wide Jet] Plateau Phase's Cocoon [Narrow Jet] Plateau Phase's Cocoon [Wide Jet]

J-Band


-20

-18

-16

-14

-12

-10

-8

-6

13

15

17

19

21

23

25

270 1 2

MA

B

mA

B (D

=40M

pc)



R-Band

HH+19 in prep

-20

-18

-16

-14

-12

-10

-8

-6

13

15

17

19

21

23

25

270 1 2

MA

B

mA

B (D

=40M

pc)



R-Band


-20

-18

-16

-14

-12

-10

-8

-6

-4

-2

13

15

17

19

21

23

25

27

29

31

0 1 2

MA

B

mA

B (D

=40M

pc)



U-Band

HH+19 in prep

-20

-18

-16

-14

-12

-10

-8

-6

-4

-2

13

15

17

19

21

23

25

27

29

31

0 1 2

MA

B

mA

B (D

=40M

pc)



U-Band

Temperature & Color (preliminary)

1.E+03

1.E+04

1.E+05

0 1 2 3

T [K

]


GW170817 Prompt [1e51 erg/s ×~2s] Narrow Prompt [1e51 erg/s ×~2s] Wide EE [1e49 erg/s ×~100s] Narrow EE [1e49 erg/s ×~100s] Wide Plateau [1e46 erg/s ×~1e4s] Narrow Plateau [1e46 erg/s ×~1e4s] Wide

HH+19 in prep

1.E+03

1.E+04

1.E+05

0 1 2 3

T [K

]


GW170817 [Kasliwal+17 & Drout+17]

Prompt Phase's Cocoon [Narrow Jet]

Prompt Phase's Cocoon [Wide Jet]

Extended Phase's Cocoon [Narrow Jet]

Extended Phase's Cocoon [Wide Jet]

Plateau Phase's Cocoon [Narrow Jet]

Plateau Phase's Cocoon [Wide Jet]

The Prediction

HH+19 in prep

SummaryThe Cocoon outshines r-process likely to have contaminated the early macronova in GW170817

Large Opening Angles for the central engine are excluded

Prediction of A Bright Early Counterparts to peak and outshine r-process in the first a few hours (if powered by the EE/PL emission of the engine)

The Cocoon emission in the early macronova in …Beyond r-process: The Cocoon emission in the early...

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