Directed searches for broadband gravitational-waveemission in energetic core-collapse supernovae
Maurice H.P.M. van Putten
in collaboration with Amir Levinson, Filippo Frontera, Cristiano Guidorzi,
Massimo Della Valle and Lorenzo Amati
ApJ, 2015, under review, ApJ, 2015, 812:124, ApJ, 810:7MNRAS, 2015, 447, L11, MNRAS, 2014, 444:L58, ApJ, 2014, 786:146
LeCosPA, Taipei, December 14 2015 1
Outline
Core-collapse supernovae: new opportunities for GWs
Outlook on broadband long-duration GWs
2
BATSE, BeppoSAX and Swift: near-extremal black holes loosing angular momentum
Near-optimal searches for broadband emission by MF
A case study: Type Ib/c SN 2010br (D = 10 Mpc)
(c)2015 van Putten
(c)2012 van Putten 3
Dynamical curvature
Rotating tidal field
ω = 2Ωorbit , Ωorbit ≅Ma3
a
h = h0 + h1(t) =MD
+ h1(t)
Dimensionless strain
D
(c)2015 van Putten
Gravitational waves
GR: a coupled elliptic-hyperbolic system of equations
Newton’s law: elliptic part
GW waves: hyperbolic part
Gab(GW) = rotating Newtonian tidal field
http://carina.astro.cf.ac.uk/groups/relativity/
(in SO(3,1) four-covariant form, van Putten & Eardley 1996)
4(c)2015 van Putten
Gentle sources...
PSR 1913+16
P = 7.75 hre = 0.617F(e) = 11.8LGW = 0.2% LSolar
Hulse-Taylor 1974(Nobel Prize 1993)
Inspiral rate 1 cm/day
5
Extreme transient sources...
(c)2015 van Putten
(c)2012 van Putten(c)2014 van Putten
SN1987A (Type II)
Radio-loud, asphericalrelativistic radio jets Turtle et al. 1987
Nisenson & Papaliolios 1999
Eν ≅ 1053 erg
Formation of high density matter in CC-SNe
6
Bisnovatyi-Kogan, G. S. 1970, Astron. Zh., 47, 813van Putten, Della Valle, Levinson, 2011, A&A, 535, L6
Probably powered by magnetic winds from an angular momentum-rich inner engine
Ek ≅ 1×1051 erg
(c)2015 van Putten
(c)2012 van Putten 7
GWB from SN1987A?
7
angular momentum-rich BH-disk or torus formation?
LGW ~ 1051 erg s−1
?
van Putten, 2015, ApJ, 810:7; van Putten, 2008, ApJ,684:L91 Levinson, van Putten & Pick, 2015, ApJ, 812:124;
Minor non-axisymmetry in matter about the ISCO:
Major output in long duration GW burst:
(c)2015 van Putten
(c)2012 van Putten 8
Ascending and descending chirps
LGW ~ 1051 erg s−1
van Putten, 2008, ApJ,684:L91 Levinson, van Putten & Pick, 2015, ApJ, 810:124
Non-axisymmetric fall back matter Non-axisymmetric matter at the ISCO
−40 −20 0 20 40−20
−10
0
10
20
x axis (a.u.)
y ax
is (a
.u.)
(c)
100 101 102 103
100
Fourier index k
sign
al |c
k2 | (a.
u.)
(d)
b m
−40 −20 0 20 40−20
−10
0
10
20
(a)
x
y
−10 −5 0 5 10−10
−5
0
5
10
(b)
x
y
b r1b r2
(c)2015 van Putten
(c)2012 van Putten(c)2014 van Putten
GRB 980425/SN1998bw
Radio-loud, aspherical
CC-SNe: diverse and energetic
9
About 20% of all CC-SNe are Type Ib/c supernovae:- H and He stripped progenitors- Probably in compact binaries - 1% branching ratio into LGRBs
van Putten, Della Valle & Levinson, 2011, A&A, 535:L6
(c)2015 van Putten
(c)2012 van Putten 10
Swift phenomenology
LGRBs, SGRBs, SGRBEEs, LGRBNs:
soft EE satisfy same Amati relation
Van Putten, Lee, Della Valle, Amati & Levinson, 2014, MNRAS, 444, L58
Common and universal inner engine: rotating black hole
(c)2015 van Putten
11
Modified Bardeen accretion
M = e m − Lj
J = j m − 2Lj
ΩH
⎧
⎨⎪⎪
⎩⎪⎪
Hyper-accretion with outflows
0 0.1 0.2 0.3 0.4 0.5 0.6 0.7 0.8 0.9 10
0.05
0.1
0.15
0.2
0.25
a/M
accr
etio
n ef
ficie
ncy
1ISCO=const.a/M=const. 1H=const.
Surge continues unless efficiency is anomalously highEnd point is a rapidly rotating black hole
van Putten, 2015, ApJ, in press
(c)2015 van Putten
12
Formation of near-extremal BHs
Surge in mass and angular momentumEnd point will be near-extremal close to the Thorne limit
Bardeen accretion:
0 0.2 0.4 0.6 0.8 10
0.1
0.2
0.3
0.4
0.5
a/M
M1
0 2 4 6 8 100
0.2
0.4
0.6
0.8
1
M [Solar]
a/M
0 2 4 6 8 100
500
1000
1500
2000
2500
3000
M [Solar]
f ISC
O [H
z]
4 6 8 105
10
15
20
25
r ISC
O
M [Solar]
M1ISCOM1H
M = e mJ = j m
⎧⎨⎪
⎩⎪
van Putten, 2015, ApJ, 812:7
(c)2015 van Putten
(c)2012 van Putten 13
BATSE light curves of LGRBs
van Putten, 2012, PTP, 127, 331
(c)2015 van Putten
(c)2012 van Putten 14
BH spin-down against ISCO: confrontation with in BATSE
nLC from matched filtering analysis
−1 0 1 2 30
0.2
0.4
0.6
0.8
1
2 s < T90 < 20 s
coun
t rat
e (a
.u.)
nLCBHS
−1 0 1 2 3−0.5
0
0.5
deviation± 3m
−1 0 1 2 30
0.2
0.4
0.6
0.8
1
T90 > 20 s
coun
t rat
e (a
.u.)
nLCBHS
−1 0 1 2 3−0.5
0
0.5
deviation± 3m
van Putten & Gupta, 2009, MNRAS, 394, 2238van Putten, 2012, Prog. Theor. Phys., 127, 331
van Putten, 1999, Science, 284, 115van Putten & Levinson, 2002, Science, 295, 1874
BH feedback to ISCO
(c)2015 van Putten
15
Lwi = 4
3Lwc T
τ⎛⎝⎜
⎞⎠⎟
Enhanced luminosity from intermittency
van Putten, 2015, MNRAS, 447, L11
e.g. with random reversals of the orientation of magnetic fields in the inner engine
Intermittent luminosity >> continuous luminosity:
Intermittent feedback:
(c)2015 van Putten
(c)2012 van Putten 16
Intermittent inner engines
y!axi
s
PRESSURE
y!axi
sy!
axi
s
z!axis
y!axi
s
MAGNETIC FIELD STRENGTH
z!axis
van Putten, 2015, MNRAS, 447, L11
LGRB from intermittent outflows
(c)2015 van Putten
Magnetically striped long-lived relativistic MHD ejecta
van Putten, 2015, MNRAS, 447, L11
17
velocity density
hydrostatic pressure azimuthal magnetic field
“Double shot” experiment:
(c)2015 van Putten
(c)2012 van Putten 18
Calorimetric ratios
R* ≡
E*Erot
≅ E*(1− 2)M
:
Rj + Rk + RD + RS ≅ 1Jets kinetic energy
accompanying supernova
dissipation inner disk or torus
entropy creation event horizon
van Putten, 2015, ApJ, 812:7
(c)2015 van Putten
(c)2012 van Putten 19
Rj ≡Ej
Erot
≅ 0.2% ε0.16
⎛⎝⎜
⎞⎠⎟−1
Rk ≡ESN
Erot
≅ 0.5%
Effective calorimetric ratios
Spin down against HD matter:
Jet-to-rotational energy: Kinetic energy-to-spin energy:
RD =O(1), RjD =Rj
RD
<<1
(c)2015 van Putten
20
Frame dragging
ALMA/ESO
SDP.81
Non-relativistic frame dragging around the Earth
Relativistic frame dragging
Gravity Probe B: Everitt et al., 2011, PRL. 106, 221101LAGEOS II: Ciufolini, I., & Pavils, E.C., 2004, Nature, 431, 958
van Putten, 2015, MG13, 1799
Er ≅ 6 ×1054 M
10M
⎛⎝⎜
⎞⎠⎟
erg
Equivalent to frame dragging at 5 million Schwarzschild radii of an extreme Kerr BH with the same angular momentum as the Earth
(c)2015 van Putten
(c)2014 van Putten - HUST 21
ω
ωbag
radiation
van Putten, 1999, Science, 284, 115, van Putten, 2001, Phys. Rev. Lett., 84, 091101; van Putten & Levinson, 2002, Science, 295, 1874; van Putten, 2002, ApJ, 575, L71; Bromberg, Levinson, van Putten, 2006, NewA, 11, 619; van Putten, 2012, Prog. Theor. Phys., 127,331van Putten, 2008, ApJ, 684, L91
From forced turbulence,Non-axisymmetric instabilities excited by heating, magnetic pressure
(Dirchlet BC)
(Ingoing radiative BC)
(outgoing radiative BC at infinity))
Magnetic moment in lowest energy state
Black hole in its lowest energy state supports open flux tubes from H to infinity
LGRB-GWB from BH feedback to the ISCO
(c)2015 van Putten
Broadband GW emission from CC-SNe
22
van Putten, Levinson, Frontera, Guidorzi, Amati & Della Valle, 2015
(under review)
(c)2015 van Putten
(c)2012 van Putten
LIGO-Virgo and KAGRA GW detectorshttp://www.ligo.caltech.edu, http://www.ego-gw.it
(c)2014 van Putten 23(c)2015 van Putten
(c)2012 van Putten 24
Butterfly filter on df/dt
Side step Fourier by TSMF using a bank of chirp templates
(c)2015 van Putten
(c)2014 van Putten - HUST 25
Mixed ascending-descending chirp templates
van Putten, Guidorzi & Frontera, 2014, ApJ, 786, 146
Universal: applies to broadband frequency analysis of light curves of gamma-rays and gravitational waves
Two principle parameters:T and f0Numerical solution to ODE of BH spin-down against ISCO
(c)2015 van Putten
(c)2014 van Putten - HUST 26
BeppoSAX sample of LGRBs at 2 kHz
van Putten, Guidorzi & Frontera, 2014, ApJ, 786, 146
0.59 photons/0.5 ms bin: trivial autocorrelation
1.26 photons/0.5 ms bin: non-trivial autocorrelation
(c)2015 van Putten
(c)2012 van Putten 27
BeppoSAX phenomenology
Smooth extension of Kolmogorov spectrum
van Putten, Guidorzi & Frontera, 2014, ApJ, 786, 146
no evidence for proto-PSR
Matched filtering analysis of 2 kHz light curves (1.26 photons/0.5ms bin)
Beloborodov, A. M., Stern, B. E., & Svensson, R. 1998, ApJL, 508, L25Beloborodov, A. M., Stern, B. E., & Svensson, R. 2000, ApJ, 535, 158
(c)2015 van Putten
(c)2014 van Putten - HUST 28
0 1 2 3 4 5 6 7 8 9 10x 105
−5
0
5x 10−19
sample index
synt
hetic
stra
in
0 500 1000 1500 2000 2500 3000 3500 4000
10−16
10−15
frequency [Hz]
Four
ier c
oeffi
cien
tFourier versus TSMF
Fourier spectrum
Spectrum extracted by TSMFusing 8.64 million chirp templates
van Putten, 2015, ApJ, 812:7
Synthetic shot noise
(c)2015 van Putten
(c)2012 van Putten 29
heff ~MD
⎛⎝⎜
⎞⎠⎟EGW
M⎛⎝⎜
⎞⎠⎟
12~ 10−21
heff(r ) = heff
τT
⎛⎝⎜
⎞⎠⎟
12~ 10−22
Probing GWBs from CC-SNe
Chirp detection by TSMF (tau=1 s)van Putten, Tagoshi, Tatsumi, Masa-Katsu & Della Valla,
2011, PRD, 83, 044046
(c)2015 van Putten
Apply butterfly/TSMF to Type Ib/c event SN2010br (z=0.0023)
- Discovered April 10 2010 during LIGO sixth science run- Extremely nearby: D=10 Mpc (once / decade)- Challenging: optical light curve not resolved, anomalously weak or late-time discovery
(c)2012 van Putten 30
LIGO S6 data
(c)2015 van Putten
tSN2010br
discovery2 week S6 data
true time-of-onset?
(c)2012 van Putten 31
Butterfly filtered LIGO S6 data
(c)2015 van Putten
(c)2012 van Putten 32
Maximal sensitivity source detection by TSMF
45
van Putten, 2015 (under review)
Two-parameter search(scaling T and f0)
Coarse grained search: one-parameter scaling (T only)
(c)2015 van Putten
(c)2012 van Putten 33
Application of L1-H1 coincidence criteria
(c)2015 van Putten
van Putten, 2015 (under review)
(c)2012 van Putten 34
Conclusions and outlook BATSE, BeppoSAX, Swift:
LGRBs: near-extremal black holes loosing angular momentum to ISCO
Formation of BH-disk or torus systems in energetic CC-SNe:
- CC-SNe: high density matter in aspherical SN1987A- CC-SNe: some produce BHs rather than NS- SNIc: parent population normal long GRBs- SNIc: about 100/yr within 100 Mpc
GWBs from SNIc are competitive with mergers if just 1% is successful
Strategy
Directed searches for LGWB in nearby CC-SNe from optical surveys, e.g., 0.1/yr in M51, M82 (J.-E. Heo et al., 2016, NewA, 42, 24)
Apply TSMF over weeks/minutes using one/two-parameter template banks
Sensitivity range ~100 Mpc for Advanced LIGO-Virgo, KAGRA (c)2015 van Putten