Raffaella Margutti Harvard Institute for Theory and Computation On behalf of the Harvard SN forensic team Kyoto2013 What happens when jets barely break out of a star Type Ic SN core ID: 310510
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Slide1
The signature of the CE in the weakest relativistic explosions
Raffaella Margutti
Harvard – Institute for Theory and Computation
On behalf of the Harvard SN forensic team
Kyoto2013
What happens when jets barely break out of a star?Slide2
Type
Ic
SN
core
H envelope
MASSIVE STAR
WINDS
CE
Why only ~ few % of type
Ibc
SN harbors a CE
?
1
How does the CE manifest its presence
?
2Slide3
How does the central engine manifest its presence?
Temporal Variability
Prompt gamma-ray emission
(e.g.
Morsony+10
)
X-ray flares
(Margutti+13; Chincarini+10;Bernardini+12; Margutti+11a; Margutti+11b )
X-ray plateau
Magnetar
(e.g.
Dall’Osso+10
) or accretion (e.g.
Kumar+08
)
Margutti et al.,2013
ApJ
778 18, (arXiv:1308.1687)
Energy partitioning + Late-time X-ray excess
GRB100316D/SN2010bhSlide4
Γβ
Ek
Ejecta
kinetic energy profile
Hydrogen-stripped progenitor
Core-collapse
Hydrodynamical
collapse
(Tan
2001)
(Γβ)
-5.2
OPTICAL
Thermal emission
RADIO
NON Thermal emissionSlide5
Kyoto2013
Margutti +13;
Kamble
+13;
Soderberg
+06, +10Slide6
Γβ
Ek
Ejecta
kinetic energy profile
Hydrogen-stripped progenitor
Core-collapse
Hydrodynamical
collapse
(Tan 2001)
(Γβ)
-5.2
(Γβ)
-0.6
Central EngineSlide7
Kyoto 2013
Hydrod
. collapse
Non-collimated
Non-relativistic
COLLIMATED (jets)
Relativistic
Energy partitioningSlide8
Take-away list:
1.
Kyoto 2013
The key difference between an ordinary explosion and an engine-powered explosion is the way the energy budget is
PARTITIONED
. Slide9
Kyoto 2013
Hydrod
. collapse
Energy partitioningSlide10
Kyoto 2013
-->Continuum
Less energetic than
GRBs
(local universe)
Mildly relativistic
Less collimated than
GRBs
10 times more common than
GRBs
Collimation
Their
Ek
profile still requires a CESlide11
Take-away list:
1.
Kyoto 2013
The key difference between an ordinary explosion and an engine-powered explosion is the way the energy budget is
PARTITIONED
. There is a continuum of properties, that bridges the gap between ultra-relativistic, collimated explosions and ordinary SNe, populated by:Sub-E
GRBs and relativistic SNe
2.Slide12
Kyoto 2013
do we care so much about these intermediate explosions
WHY
?
GRB100316D/SN2010bh
Margutti et al.,2013 ApJ 778 18Slide13
Kyoto 2013
X-rays
RadioSlide14
100316D/2010bh
MILD decay + Extremely SOFT emission
Central
engine
Faster
blob
Slower blob
Collision
EXTERNAL SHOCK
Pre Burst
Prompt Emission
Ambient medium interaction
Afterglow
STANDARD GRB MODEL
Synchrotron
Engine
ON
Engine
OFFSlide15
UCSC 2013
Synchrotron emission
Fireball Dynamics
GRBsSlide16
UCSC 2013
Synchrotron emission
Fireball Dynamics
Not synchrotron
GRBsSlide17
UCSC 2013
100316D/ 2010bh
Synchrotron
Radio
X-rays
SED,
t
=36 days
Radio
X-raysSlide18
Inverse Compton emission
100316D/2010bh
10 days
37 days
Accretion on BH
Magnetar
spin-down
CE
…an X-ray excess…
What is the origin?
t
-0.8
“modified” fall-back scenario”
~10^52 erg
Rapidly rotating!! (ms!)Slide19
Take-away list:
1.
Kyoto 2013
The key difference between an ordinary explosion and an engine-powered explosion is the way the energy budget is
PARTITIONED
. There is a continuum of properties, that bridges the gap between ultra-relativistic, collimated explosions and ordinary SNe, populated by:Sub-E
GRBs and relativistic SNe
2.Sub-energetic
GRBs reveal the emission of the CE at late times, either in the form of a rapidly rotating magnetar or a BH (in a non-standard fall-back accretion scenario)
3.Slide20
Kyoto 2013
The big picture: H-stripped explosions
Ordinary
SNe
Ibc
NO Engine, NO JET
GRBs
Engine
Fully developed jet
Sub-E
GRBs
Engine
Weak jet
We can study the engine with late-time radio and X-rays
Jet
CE
Jet
CESlide21
Kyoto 2013
Radio
X-rays
The EndSlide22
BACK-UP SLIDESSlide23
UCSC 2013
Lazzati
+12,
Morsony
+07, +10
Is the SAME CE?
What is the fraction of
SNe
with CE?
What is the nature of the CE?Slide24Slide25
OPTICAL
RADIO
synchrotron
Wellons +12
Soderberg+04, +06,+10
F
ν,peak
(t
)
ν
peak
(
t
)
-5/2
-(p-1)/2
SN shock interaction with the medium
Drout
+11
LC width τ≈(Mej
3
/Ek)
1/4
V
phot
≈Ek/MejSlide26
Gamma-Ray Bursts
Log(Time
)
Log(Flux
)
γ
-rays
~30
s
~10^51 erg
X-rays
Optical
Radio
~hours
Central
engine
Faster blob
Slower blob
Collision
Ambient medium interaction
INTERNAL SHOCK
EXTERNAL SHOCK
Afterglow
Pre Burst
Prompt Emission
JETSlide27
Log(Time)
Log (Flux)
t
break1
(300
s
)
t
break2
(10^4
s
)
t
-3
t
-1
t
-2
PROMPT
AFTERGLOW
A typical
GRB
Explosion:
Black Hole (?)
SN bump
~10 daysSlide28
UCSC 2013
HIGH expansion
velocity!
30000-40000 km/
s
vs.10000 km/s
Modjaz
2006
GRB060218
GRB980425
Sanders 2012
Photosperic
Velocity (10
3
km/
s
)
SN/GRB
BL-SN
Ibc
SN2010ay
SNe
associated
w
.
GRBs
NO Hydrogen
FASTSlide29
UCSC 2013
SN1994I
SN2002ap
GRB/
SNe
“Standard”, envelope stripped SN
Ibc
Hydrogen-poor
Super Luminous
SNe
(M<-21)
(e.g. Gal-Yam 2012)
7x10
43
erg/
s
Broad-lined + large
Ek
+ large Ni mass = Very powerful / energetic explosions