Electromagnetic counterparts and r-process Tsvi Piran The Hebrew - - PowerPoint PPT Presentation

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Electromagnetic counterparts and r-process Tsvi Piran The Hebrew - - PowerPoint PPT Presentation

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Electromagnetic counterparts and r-process Tsvi Piran The Hebrew University Kenta Hotokezaka, Ehud Nakar Kyoto - Nov 2016 Outline 1. The Li-Paczynski Macronova (kilonova) 2. GRBs 060614/050709 and their Macronove 3. Plutonium 4. Dwarf

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SLIDE 1

Electromagnetic counterparts and r-process

Tsvi Piran

The Hebrew University Kenta Hotokezaka, Ehud Nakar

Kyoto - Nov 2016

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SLIDE 2

Outline

1. The Li-Paczynski Macronova (kilonova) 2. GRBs 060614/050709 and their Macronove 3. Plutonium 4. Dwarf Galaxies 5. The cocoon’ s macronova - the strongest EM counterpart? 6. Limits on magnetars from radio flares 7 . * The energy deposition rate 8. Conclusions

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SLIDE 3
  • Radioactive decay of the

neutron rich matter.

  • Eradioactive ≈ 0.001 Mc2 ≈

1050 erg

  • A weak short Supernova

like event.

  • 1. Macronova*(Li & Paczynski 1997)

Bohdan Paczynski

*Also called Kilonova

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SLIDE 4
  • Radioactive decay of the

neutron rich matter.

  • Eradioactive ≈ 0.001 Mc2 ≈

1050 erg

  • A weak short Supernova

like event.

  • 1. Macronova*(Li & Paczynski 1997)

Bohdan Paczynski

*Also called Kilonova Hektanova

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SLIDE 5
  • Radioactive decay of the

neutron rich matter.

  • Eradioactive ≈ 0.001 Mc2 ≈

1050 erg

  • A weak short Supernova

like event.

  • 1. Macronova*(Li & Paczynski 1997)

Bohdan Paczynski

*Also called Kilonova Hektanova Decanova

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SLIDE 6
  • After a second dE/dt∝t-1.3 (Freiburghaus+

1999; Korobkin + 2013)

Radioactive Decay*

Korobkin + 13; Rosswog, Korobkin + 13

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SLIDE 7

Photons escape from this region luminosity Decrease due to radioactive decay Increase as we see a large fraction of the matter. time The light curve depends on 1. mass 2. velocity 3.

  • pacity
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SLIDE 8

Photons escape from this region luminosity Decrease due to radioactive decay Increase as we see a large fraction of the matter. time The light curve depends on 1. mass 2. velocity 3.

  • pacity
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SLIDE 9
  • S. Rosswog, … Following Davies + 1994
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Lanthanides dominate the opacity

(Kassen & Barnes 13, Tanaka & Hotokezaka 13) )

κ= 10cm2/gm tmax ∝κ1/2 => l o n g e r Lmax ∝κ-0.65 => weaker

T ∝ κ-0.4 => redder

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SLIDE 11

Lanthanides dominate the opacity

(Kassen & Barnes 13, Tanaka & Hotokezaka 13) )

κ= 10cm2/gm tmax ∝κ1/2 => l o n g e r Lmax ∝κ-0.65 => weaker

T ∝ κ-0.4 => redder

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SLIDE 12

Lanthanides dominate the opacity

(Kassen & Barnes 13, Tanaka & Hotokezaka 13) )

κ= 10cm2/gm tmax ∝κ1/2 => l o n g e r Lmax ∝κ-0.65 => weaker

T ∝ κ-0.4 => redder

1 days 10

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SLIDE 13

Lanthanides dominate the opacity

(Kassen & Barnes 13, Tanaka & Hotokezaka 13) )

κ= 10cm2/gm tmax ∝κ1/2 => l o n g e r Lmax ∝κ-0.65 => weaker

T ∝ κ-0.4 => redder

1 days 10 1040 1041

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SLIDE 14

Lanthanides dominate the opacity

(Kassen & Barnes 13, Tanaka & Hotokezaka 13) )

κ= 10cm2/gm tmax ∝κ1/2 => l o n g e r Lmax ∝κ-0.65 => weaker

T ∝ κ-0.4 => redder

1 days 10 1040 1041

uv or optical -> IR

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SLIDE 15

GRB130603B @ 9 days AB

(6.6 days at the source frame)

nIR HST image (Tanvir + 13) V

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SLIDE 16

Swift Tanvir + 13, Berger + 13

Macronova?

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SLIDE 17

If correct

Confirmaiton of the GRB neutron star merger model (Eichler, Livio, TP & Schramm 1989). Confirmation of the Li-Paczynski Macronova (Li-Paczynski 1997). Confirmation that compact binary mergers are the source of heavy (A>130) r-process material: Gold, Silver, Platinum, Plotonium, Uranium etc…(Lattimer & Schramm, 75).

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The rate of Short GRBs Macronova and r- process

About 1/3 of Swift short (<2sec) GRBs are Collapsars The rate of non-Collapsar short GRBs (sGRbs) is 4.1+2.3-1.9 Gpc-3 yr-1 (depending on the assumed minimal luminosity). A LIGO detection rate of 3-100 per year (0.1-3 coinciding with a sGRB)* A typical time delay of ~3 Gyr after SFR=> an initial separation of ~2 x 1011 cm But selection effects? Maybe consistent with p(τ)~1/τ With beaming of ~30 and mass ejection of 0.02 Msun - compatible with R-process nucleosynthesis for A>110 elements.

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SLIDE 19

GRB 060614

Yang et al., 2015 Need M≃0.1M⨀ => BH-NS ?

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GRB 050709

Jin et al., 2016 Need M≃0.05M⨀ => BH-NS ?

!! !" !# !$ !% !& !' ! " $ !( "( #( ) )( !"# !"#$ %$#&'()*" *+,- .+/0- 123.4 5678.9 :')#; < = > !! !" !# !$ !% !& !' ! " $ !( "( #( ) )(

!"! !"# !"$ !"% !"& '"! '"# # ( ) '! !"#$ %&'()*+ ,-.+/ *+,-.,/01 2'!!"345 !"! !"# !"$ !"% !"& '"! '"# # ( ) '!

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Are Macronova Frequent?

There are 3 (6) possible (nearby) historical candidates with a good enough data In 3/3 (3/ 6) there are possible Macronovae

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R-Process

0.1 1 10 100 1000 10000 0.0001 0.001 0.01 0.1 1 R(z=0) [Myr-1] Mej [Msun]

Short GRBs Galactic NS2 LIGO/Virgo limit Advanced (5yr) R-element mass (A>90) Macronova candidate

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SLIDE 23

R-Process

0.1 1 10 100 1000 10000 0.0001 0.001 0.01 0.1 1 R(z=0) [Myr-1] Mej [Msun]

Short GRBs Galactic NS2 LIGO/Virgo limit Advanced (5yr) R-element mass (A>90) Macronova candidate

*

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SLIDE 24

0.1 1 10 100 1000 10000 0.0001 0.001 0.01 0.1 1 R(z=0) [Myr-1] Mej [Msun]

Short GRBs Galactic NS2 LIGO/Virgo limit Advanced (5yr) R-element mass (A>90) Macronova candidate

Wanderman Piran 15

*

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SLIDE 25

0.1 1 10 100 1000 10000 0.0001 0.001 0.01 0.1 1 R(z=0) [Myr-1] Mej [Msun]

Short GRBs Galactic NS2 LIGO/Virgo limit Advanced (5yr) R-element mass (A>90) Macronova candidate

Wanderman Piran 15

*

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SLIDE 26

0.1 1 10 100 1000 10000 0.0001 0.001 0.01 0.1 1 R(z=0) [Myr-1] Mej [Msun]

Short GRBs Galactic NS2 LIGO/Virgo limit Advanced (5yr) R-element mass (A>90) Macronova candidate

Can we break the yield - rate degeneracy?

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SLIDE 27

0.1 1 10 100 1000 10000 0.0001 0.001 0.01 0.1 1 R(z=0) [Myr-1] Mej [Msun]

Short GRBs Galactic NS2 LIGO/Virgo limit Advanced (5yr) R-element mass (A>90) Macronova candidate

*

Can we break the yield - rate degeneracy?

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SLIDE 28

t t Rare Events Frequent events

Radioactive Elements

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SLIDE 29

High 244Pu at the early solar system =>

244Pu Radioactive decay time ~ 100 Myear

A nearby event near solar system Mixing time < 150 Myr Large fluctuations possible => Event rate is low Lack of Cu => 10 Myr < Mixing length

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SLIDE 30

Tissot + 16t

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SLIDE 31

The early solar system

244Pu (half life 81Myr)

Wallner + 14

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Rare and “massive” events

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r-process material in Dwarf Galaxies

(Beniamini+ 16a,b)

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SLIDE 34
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SLIDE 35
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The Secret Signatures of GRB cocoons

Nakar & TP ApJ 16 in press

From Mizuta

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The idea in a single picture

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The Jet drills a hole in the star

Zhang, Woosley & MacFadyen 2004

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Jet breakout

(Bromberg Nakar, TP, Sari 11 ApJ 2011)

The engine must be active until the jet’ s head breaks out!*

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SLIDE 40

A prediction of the Collapsar model

T90 = Te-TB

Observed duration Engine time Break out time

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SLIDE 41

A prediction of the Collapsar model

T90 = Te-TB

T90

Observed duration Engine time Break out time

dN(T90)/dt

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SLIDE 42

A prediction of the Collapsar model

TB

T90 = Te-TB

T90

Observed duration Engine time Break out time

dN(T90)/dt

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SLIDE 43

Short Long

?

T90

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SLIDE 44

Short Long

?

dlog(N)/dT90 T90

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A second look

(Bromberg Nakar, TP & Sari, 2011) T90 d N / d T

9

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SLIDE 46

A second look

(Bromberg Nakar, TP & Sari, 2011)

A direct observational proof of the Collapsar model.

T90 d N / d T

9

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SLIDE 47

Short (Non-Collapsars)

Collapsars

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SLIDE 48

Short (Non-Collapsars)

Collapsars

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SLIDE 49
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SLIDE 50
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Swift Short (Non- Collapsars) GRBs

Collapsars

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Swift Short (Non- Collapsars) GRBs

Collapsars

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SLIDE 53

Swift Short (Non- Collapsars) GRBs

Collapsars Short Swift GRBs with T90>0.7sec are not “short”!

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SLIDE 54

EGRB≈Eejecta≈Ec

Macronova + Radio flare

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SLIDE 55

Cocoon’ s structure

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3D simulation

4Msun, R*=4x1010cm. Lj =1051erg/s, θ=8ο Using Pluto with high resolution ΔR=107cm. Credit: Ore Gottlieb

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SLIDE 57

3D simulation

4Msun, R*=4x1010cm. Lj =1051erg/s, θ=8ο Using Pluto with high resolution ΔR=107cm. Credit: Ore Gottlieb

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2D simulation 110sec after breakout

4Msun, R*=4x1010cm. Lj =1051erg/s, θ=8ο Using Pluto with high resolution ΔR=107cm. Credit: Ore Gottlieb

Jet Star Wide angle Γ≈10 material

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The cocoons

Harrison, Goetlieb and Nakar in prep, 2016

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Emission component

Newtonian Cocoon - cooling (photospheric) emission Newtonian cocoon - macronova Relativistic Jet cocoon - cooling (photospheric) emission Relativistic Jet cocoon - afterglow

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The cocoons

Harrison, Goetlieb & Nakar in prep, 2016

Light “relativistic” Jet cocoon Heavy “Newtonian” stellar cocoon Jet

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Cocoon Dynamics

R Rθ

Stellar Envelope

L=Ecc/R

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SLIDE 63

η3 η2 η1

Full mixing

η=1

Partial mixing No mixing

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Partial Mixing

Harrison, Goetlieb and Nakar in prep, 2016

Light “relativistic” Jet cocoon Heavy “Newtonian” Stellar cocoon

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2D simulation 110sec after breakout

Jet Star Wide angle Γ≈10 material

4MO, R*=4x1010cm. Lj =1051erg/s, θ=8ο Using Pluto with high resolution ΔR=107cm. Credit: Ore Gottlieb

.

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Γβ Energy per Log interval Newtonian Relativistic

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Short GRBs

Nagakura et al. 2014; Murguia-Berthier et al. 2014, 2016

From Hotokezaka & TP 2015

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SLIDE 68
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SGRB cocoon signatures

+ =>

  • Rel. Cocoon cooling
  • Rel. Cocoon Afterglow,

scaling from the regular SGRB afterglow This is a wide angle signal 0.5 rad is stronger than typical SGRB orphan afterglow

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Macronova cocoon signature

Heating due to radioactive decay Blue signal at around 0.5-1 day! Brighter or comparable to the classical Macronova

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Summary

Cocoons are the forgotten cousins in the GRB story. They carry a comparable amount of energy to the GRB and are wider than the GRBs. Short GRBs have their own cocoons whose signatures might be the best EM counterpart to

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The radio - flare (Nakar & Piran 2011) Testing the Macronova interpretation

A long lasting radio flare due to the interaction of the ejecta with surrounding matter may follow the macronova.

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The radio - flare (Nakar & Piran 2011) Testing the Macronova interpretation

A long lasting radio flare due to the interaction of the ejecta with surrounding matter may follow the macronova.

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The radio - flare (Nakar & Piran 2011) Testing the Macronova interpretation

A long lasting radio flare due to the interaction of the ejecta with surrounding matter may follow the macronova.

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The radio - flare (Nakar & Piran 2011) Testing the Macronova interpretation

A long lasting radio flare due to the interaction of the ejecta with surrounding matter may follow the macronova.

Supernova -> Supernova remnant GRB -> Afterglow Macronova -> Radio Flare

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Search for the flare from GRB 130603B by the EVLA

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Search for the flare from GRB 130603B by the EVLA

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Search for the flare from GRB 130603B by the EVLA

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Radio limits on Magnetars

Horesh + 16 060614 130603B

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Do GRBs need magnetars?

Quasars eject magnetic jets. => GRBs also have magnetic jets => Mangetars But quasars produce magnetic jets without magnetars

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Where?

Prompt? Afterglow? Is impossible to have both from the same magnetar?

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If a magnetar did this What did that?

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If a magnetar did this What did that?

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Energy Generation

Hotokezaka, Sari & TP + 16

N+n N+p e νe γ

tf = 2⇡3 G2

F

~7 m5

ec4 ≈ 104sec

˙ E = ✏e mec2 tf ✓ t tF ◆−α 1 ⌧ ∝ 1 E Z d3pe Z d3pν Relativistic 1 ⌧ ∝ E5 → ↵ = 6/5 Newtonian 1 ⌧ ∝ E7/2 → ↵ = 9/7

GF

tf = 2⇡3 G2

F

~7 m5

ec4 ≈ 104sec

˙ E = ✏e mec2 tf ✓ t tF ◆−α 1 ⌧ ∝ d dE Z d3pe Z d3pν

E3 or E3/2

E3

Z Z Relativistic 1 ⌧ ∝ E5 → ↵ = 6/5 Newtonian 1 ⌧ ∝ E7/2 → ↵ = 9/7

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Efficiency

Hotokezaka, Wajano +…TP 16; Barnes +

Photon losses: The ejecta becomes

  • ptically thin to gamma-rays long

before it becomes optically thin to

  • ptical/IR photons => photon

leakage during the macronova peak (Hotokezaka + 16) Electron losses: Unlike previous believes not all the electrons energy is deposited (Barnes + 16)

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Summary

The nIR flare that followed the short GRB 130603B could have been a

  • Macronova. If so than:

✓Short GRBs arise from mergers. ✓Gold and other A>130 elemets are

produced in mergers. (But large mej). A radio flare may confirm this! A second & third Macronovae suggest a BH-NS merger

244Pu suggests that R-process production

is in rare events. Cocoon produces a short bright macronova We wait for the sGRB-GW coincidence

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SLIDE 87

Summary

The nIR flare that followed the short GRB 130603B could have been a

  • Macronova. If so than:

✓Short GRBs arise from mergers. ✓Gold and other A>130 elemets are

produced in mergers. (But large mej). A radio flare may confirm this! A second & third Macronovae suggest a BH-NS merger

244Pu suggests that R-process production

is in rare events. Cocoon produces a short bright macronova We wait for the sGRB-GW coincidence

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SLIDE 88

Summary

The nIR flare that followed the short GRB 130603B could have been a

  • Macronova. If so than:

✓Short GRBs arise from mergers. ✓Gold and other A>130 elemets are

produced in mergers. (But large mej). A radio flare may confirm this! A second & third Macronovae suggest a BH-NS merger

244Pu suggests that R-process production

is in rare events. Cocoon produces a short bright macronova We wait for the sGRB-GW coincidence