The Cocoon emission in the early macronova in …Beyond r-process: The Cocoon emission in the early...
Transcript of 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>)
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
Ram Pressure Balance
Engine Ejecta
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
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
vb /vej = 2 (Ioka Nakamura 2017)
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
vb /vej = 2 (Ioka Nakamura 2017)
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
Time since GW170817 [day]
GW170817's Cocoon
! = 1 cm2 g -1
! = 0.3 –3 cm2 g -1
EE, and Plateau Emission
Kisaka+17
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]
Time since GW170817 [day]
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]
Time since GW170817 [day]
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)
Time since GW170817 [day]
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)
Time since GW170817 [day]
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
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)
Time since GW170817 [day]
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
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)
Time since GW170817 [day]
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]
R-Band
The Cocoon outshining R-process (preliminary)
-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)
Time since GW170817 [day]
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
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)
Time since GW170817 [day]
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]
U-Band
Temperature & Color (preliminary)
1.E+03
1.E+04
1.E+05
0 1 2 3
T [K
]
Time since GW170817 [day]
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
]
Time since GW170817 [day]
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)