lack holes in modified gravity models...black holes in modified gravity models arxiv:1312.4625+ work...
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BLACK HOLES IN MODIFIED GRAVITY MODELSarXiv:1312.4625 + WORK IN PROGRESS
Andrei Frolov
Jun-Qi Guo (SFU)Daoyan Wang (UBC)
José Tomás Gálvez Ghersi (SFU)Alex Zucca (SFU)
16th Canadian Conference on General Relativityand Relativistic Astrophysics
SFU Segal Building, Vancouver, BC, Canada7 July 2016
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 1 / 26
Why Study Modified Gravity?
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 2 / 26
THE BEST ANSWER I FOUND SO FAR...
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 2 / 26
MAYBE IT’S GRAVITY WE DON’T UNDERSTAND
MODIFY EINSTEIN-HILBERT ACTION TO INCLUDE OTHER STUFF, E.G.
S =
∫
§
f (R )16πG
+L m
ª
p
−g d 4 x
UV MODIFICATION:
f (R ) =R +R 2
M 2
Starobinsky (1980)
IR MODIFICATION:
f (R ) =R −µ4
R
Capozziello et. al. [astro-ph/0303041]Carroll et. al. [astro-ph/0306438]
FOR F(R) THEORY TO MAKE SENSE WE NEED:
f ′ > 0 – otherwise gravity is a ghost
f ′′ > 0 – otherwise gravity is a tachyon
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 3 / 26
MAYBE IT’S GRAVITY WE DON’T UNDERSTAND
MODIFY EINSTEIN-HILBERT ACTION TO INCLUDE OTHER STUFF, E.G.
S =
∫
§
f (R )16πG
+Lm
ª
p
−g d 4 x
UV MODIFICATION:
f (R ) =R +R 2
M 2
Starobinsky (1980)
IR MODIFICATION:
f (R ) =R −µ4
R
Capozziello et. al. [astro-ph/0303041]Carroll et. al. [astro-ph/0306438]
FOR F(R) THEORY TO MAKE SENSE WE NEED:
f ′ > 0 – otherwise gravity is a ghost
f ′′ > 0 – otherwise gravity is a tachyon
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 3 / 26
MAYBE IT’S GRAVITY WE DON’T UNDERSTAND
MODIFY EINSTEIN-HILBERT ACTION TO INCLUDE OTHER STUFF, E.G.
S =
∫
§
f (R )16πG
+Lm
ª
p
−g d 4 x
UV MODIFICATION:
f (R ) =R +R 2
M 2
Starobinsky (1980)
IR MODIFICATION:
f (R ) =R −µ4
R
Capozziello et. al. [astro-ph/0303041]Carroll et. al. [astro-ph/0306438]
FOR F(R) THEORY TO MAKE SENSE WE NEED:
f ′ > 0 – otherwise gravity is a ghost
f ′′ > 0 – otherwise gravity is a tachyon
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 3 / 26
MAYBE IT’S GRAVITY WE DON’T UNDERSTAND
MODIFY EINSTEIN-HILBERT ACTION TO INCLUDE OTHER STUFF, E.G.
S =
∫
§
f (R )16πG
+Lm
ª
p
−g d 4 x
UV MODIFICATION:
f (R ) =R +R 2
M 2
Starobinsky (1980)
IR MODIFICATION:
f (R ) =R −µ4
R
Capozziello et. al. [astro-ph/0303041]Carroll et. al. [astro-ph/0306438]
FOR F(R) THEORY TO MAKE SENSE WE NEED:
f ′ > 0 – otherwise gravity is a ghost
f ′′ > 0 – otherwise gravity is a tachyon
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 3 / 26
EXPECT DEVIATION FROM ΛCDM COSMOLOGYO
yaizu,Lima
&H
u(0807.2462
)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 4 / 26
INVOKE CHAMELEON TO SATISFY LOCAL TESTS
r/r
ρ (g
cm
-3)
0.1 1 10 100 1000
10-20
10-10
1
R/κ2 (n=4, | fR0|=0.1)
ρ
r/r100 1000 104
R/κ
2 (g
cm
-3)
10-24
10-23
|fR0|=0.001|fR0|=0.01|fR0|=0.05|fR0|=0.1
ρ
n=4
Hu & Sawicki (0705.1158)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 5 / 26
FIELD EQUATIONS IN F(R) GRAVITY
Vary the action with respect to the metric:
S =
∫
§
f (R )16πG
+Lm
ª
p
−g d 4 x
Einstein equations turn into a fourth-order equation:
f ′Rµν− f ′;µν+
f ′−1
2f
gµν = 8πG Tµν
A new scalar degree of freedom φ ≡ f ′−1 appears:
f ′ =1
3(2 f − f ′R ) +
8πG
3T
Can rewrite fourth-order field equation as two second order ones!
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 6 / 26
A NEW SCALAR DEGREE OF FREEDOM
Equation for φ ≡ f ′−1 is just a scalar wave equation:
φ =V ′(φ)−F
Matter directly drives the field φ by a force term:
F =8πG
3(ρ−3p )
Effective potential can be found by integrating
V ′(φ)≡d V
dφ=
1
3(2 f − f ′R )
In practice, easier to obtain in parametric form:
d V
d R≡
d V
dφ
dφ
d R=
1
3(2 f − f ′R ) f ′′
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 7 / 26
EXAMPLE I: (SAFE) UV MODIFICATION
0
0.5
1.0
1.5
2.0
2.5
–1 –0.5 0 0.5 1
V/M
φ
2
in vacuum
U (φ) =V (φ) +F (φ∗−φ)
f (R ) =R +R 2
M 2
φ =2R
M 2
V =1
3
R 2
M 2=
M 2
12φ2
massive scalar field!
scalar degree of freedomφ is heavy and hard toexcite
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 8 / 26
EXAMPLE I: (SAFE) UV MODIFICATION
0
0.5
1.0
1.5
2.0
2.5
–1 –0.5 0 0.5 1
in matter
V/M
φ
2
in vacuum
U (φ) =V (φ) +F (φ∗−φ)
f (R ) =R +R 2
M 2
φ =2R
M 2
V =1
3
R 2
M 2=
M 2
12φ2
massive scalar field!
scalar degree of freedomφ is heavy and hard toexcite
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 8 / 26
EXAMPLE II: (FAILED) IR MODIFICATION
0
0.1
0.2
0.3
0.4
0.5
0.2 0.4 0.6 0.8 1
V/µ2
φ
in vacuum
U (φ) =V (φ) +F (φ∗−φ)
f (R ) =R −µ4
R
φ =µ4
R 2
V =2
3
µ4
R−µ8
R 3
=2
3µ2
φ12 −φ
32
field φ is unstable!Dolgov & Kawasaki
(astro-ph/0307285)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 9 / 26
EXAMPLE II: (FAILED) IR MODIFICATION
0
0.1
0.2
0.3
0.4
0.5
0.2 0.4 0.6 0.8 1
in matter
V/µ2
φ
in vacuum
U (φ) =V (φ) +F (φ∗−φ)
f (R ) =R −µ4
R
φ =µ4
R 2
V =2
3
µ4
R−µ8
R 3
=2
3µ2
φ12 −φ
32
field φ is unstable!Dolgov & Kawasaki
(astro-ph/0307285)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 9 / 26
CAN WE COME UP WITH SOMETHING BETTER?
Hu and Sawicki [0705.1158]
f (R ) =R −α (R/R0)n
1+β (R/R0)nR0
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1.0
10-2 10-1 100 101 102
(R-F
)/R
0
R/R0
n=1n=2n=4
Starobinsky [0706.2041]
f (R ) =R+λ
1
(1+ (R/R0)2)n −1
R0
0.0
0.1
0.2
0.3
0.4
0.5
0.6
0.7
0.8
0.9
1.0
10-2 10-1 100 101 102
(R-F
)/R
0
R/R0
n=1n=2n=4
... and many other models ...
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 10 / 26
DISAPPEARING COSMOLOGICAL CONSTANT
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φABCD
E
F
G
Starobinsky [0706.2041]
f (R ) =R +λ
1+R 2−1−1
φ =−2λR
(1+R 2)2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 11 / 26
DISAPPEARING COSMOLOGICAL CONSTANT
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φBCD
E
F
G
A
Starobinsky [0706.2041]
f (R ) =R +λ
1+R 2−1−1
φ =−2λR
(1+R 2)2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 11 / 26
DISAPPEARING COSMOLOGICAL CONSTANT
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φBCD
E
F
G
A
Starobinsky [0706.2041]
f (R ) =R +λ
1+R 2−1−1
φ =−2λR
(1+R 2)2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 11 / 26
DISAPPEARING COSMOLOGICAL CONSTANT
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φB
D
E
F
G
AC
Starobinsky [0706.2041]
f (R ) =R +λ
1+R 2−1−1
φ =−2λR
(1+R 2)2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 11 / 26
DISAPPEARING COSMOLOGICAL CONSTANT
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φB
D
E
F
G
AC
Starobinsky [0706.2041]
f (R ) =R +λ
1+R 2−1−1
φ =−2λR
(1+R 2)2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 11 / 26
DISAPPEARING COSMOLOGICAL CONSTANT
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φB
D
E
F
G
AC
Starobinsky [0706.2041]
f (R ) =R +λ
1+R 2−1−1
φ =−2λR
(1+R 2)2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 11 / 26
DISAPPEARING COSMOLOGICAL CONSTANT
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φB
D
E
F
G
AC
Starobinsky [0706.2041]
f (R ) =R +λ
1+R 2−1−1
φ =−2λR
(1+R 2)2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 11 / 26
DISAPPEARING COSMOLOGICAL CONSTANT
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φB
D
E
F
G
AC
Starobinsky [0706.2041]
f (R ) =R +λ
1+R 2−1−1
φ =−2λR
(1+R 2)2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 11 / 26
DISAPPEARING COSMOLOGICAL CONSTANT
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φABCD
E
F
G
Starobinsky [0706.2041]
f (R ) =R +λ
1+R 2−1−1
φ =−2λR
(1+R 2)2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 11 / 26
SINGULARITY IS FINITE DISTANCE AWAY!
V/R0
–0.22
–0.20
–0.18
–0.16
–0.14
–0.12
–0.10
–0.18 –0.14 –0.10 –0.06 –0.02 0
curvature singularity
B
A
φδφ
in vacuum
φ∗
U (φ) =V (φ) +F (φ∗−φ)
in large R limit:
f (R ) =R+Λ+1
Rα
∞∑
n=0
µn
R n
φ ≡ f ′−1'−αµ0
Rα+1
d V
d R'
R f ′′
3=α(α+1)µ0
3 Rα+1
weak power-law singularity:
V (φ)' const−(α+1)µ0
3 |αµ0|γ|φ|γ
γ=α
α+1
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 12 / 26
SINGULARITY IS FINITE DISTANCE AWAY!
V/R0
–0.22
–0.20
–0.18
–0.16
–0.14
–0.12
–0.10
–0.18 –0.14 –0.10 –0.06 –0.02 0
curvature singularity
B
A
φδφ
in vacuum
φ∗
U (φ) =V (φ) +F (φ∗−φ)
in large R limit:
f (R ) =R+Λ+1
Rα
∞∑
n=0
µn
R n
φ ≡ f ′−1'−αµ0
Rα+1
d V
d R'
R f ′′
3=α(α+1)µ0
3 Rα+1
weak power-law singularity:
V (φ)' const−(α+1)µ0
3 |αµ0|γ|φ|γ
γ=α
α+1
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 12 / 26
SINGULARITY IS FINITE DISTANCE AWAY!
V/R0
–0.22
–0.20
–0.18
–0.16
–0.14
–0.12
–0.10
–0.18 –0.14 –0.10 –0.06 –0.02 0
curvature singularity
B
A
X
φδφ
in vacuum
in matter
φ∗
U (φ) =V (φ) +F (φ∗−φ)
in large R limit:
f (R ) =R+Λ+1
Rα
∞∑
n=0
µn
R n
φ ≡ f ′−1'−αµ0
Rα+1
d V
d R'
R f ′′
3=α(α+1)µ0
3 Rα+1
weak power-law singularity:
V (φ)' const−(α+1)µ0
3 |αµ0|γ|φ|γ
γ=α
α+1
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 12 / 26
NEED UV COMPLETION! CAN IT SAVE THE DAY?
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φABCD
E
F
G
Starobinsky [0706.2041]
f (R ) =R+λ
1+R 2−1−1
+R 2
M 2
φ =−2λR
(1+R 2)2+
2R
M 2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 13 / 26
NEED UV COMPLETION! CAN IT SAVE THE DAY?
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φBCD
E
F
Starobinsky [0706.2041]
f (R ) =R+λ
1+R 2−1−1
+R 2
M 2
φ =−2λR
(1+R 2)2+
2R
M 2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 13 / 26
NEED UV COMPLETION! CAN IT SAVE THE DAY?
V/R0
0
0.2
0.4
0.6
0.8
1.0
1.2
1.4
–1.5 –1.0 –0.5 0 0.5 1.0 1.5
φBCD
E
F
Starobinsky [0706.2041]
f (R ) =R+λ
1+R 2−1−1
+R 2
M 2
φ =−2λR
(1+R 2)2+
2R
M 2
A singularity (R =+∞)B stable dS min ( f ′ = 0 )C unstable dS max ( f ′ = 0 )D critical point ( f ′′ = 0 )E flat spacetime ( f ′ = 0 )F critical point ( f ′′ = 0 )G singularity (R =−∞)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 13 / 26
SPHERICAL SOLUTIONS IN F(R) GRAVITY
We need to solve a non-linear differential equation:
φ =−8π
3G (ρ−3p ) +V ′(φ)
How do we understand its solutions?
“EQUILIBRIUM” REGIME:
V ′(φ) =8π
3G (ρ−3p )
chameleon mechanism
“BALLISTIC” REGIME:
φ =−8π
3G (ρ−3p )
which one is realized depends on environment!
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 14 / 26
SPHERICAL SOLUTIONS IN F(R) GRAVITY
We need to solve a non-linear differential equation:
φ =−8π
3G (ρ−3p ) +V ′(φ)
How do we understand its solutions?
“EQUILIBRIUM” REGIME:
V ′(φ) =8π
3G (ρ−3p )
chameleon mechanism
“BALLISTIC” REGIME:
φ =−8π
3G (ρ−3p )
which one is realized depends on environment!
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 14 / 26
SPHERICAL SOLUTIONS IN F(R) GRAVITY
We need to solve a non-linear differential equation:
φ =−8π
3G (ρ−3p ) +V ′(φ)
How do we understand its solutions?
“EQUILIBRIUM” REGIME:
V ′(φ) =8π
3G (ρ−3p )
chameleon mechanism
“BALLISTIC” REGIME:
φ =−8π
3G (ρ−3p )
which one is realized depends on environment!
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 14 / 26
SPHERICAL SOLUTIONS IN F(R) GRAVITY
We need to solve a non-linear differential equation:
φ =−8π
3G (ρ−3p ) +V ′(φ)
How do we understand its solutions?
“EQUILIBRIUM” REGIME:
V ′(φ) =8π
3G (ρ−3p )
chameleon mechanism
“BALLISTIC” REGIME:
φ =−8π
3G (ρ−3p )
which one is realized depends on environment!
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 14 / 26
REGULAR STATIC SOLUTIONS EXIST, BUT...
Babichev & Langlois (0904.1382)
0 2 4 6 8 10-0.10
-0.08
-0.06
-0.04
-0.02
0.00
r
0.0 0.5 1.0 1.5 2.0 2.5-8.´10-9
-6.´10-9
-4.´10-9
-2.´10-9
0
Φ
Φmin
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 15 / 26
QUASI-STATIC BALL COLLAPSE IN F(R) GRAVITY
-0.09
-0.08
-0.07
-0.06
-0.05
-0.04
-0.03
-0.02
-0.01
0
0.01
0 0.2 0.4 0.6 0.8 1
φ
r/(1+r)
Potential well ofa compact object:
∆φ = −8π
3Gρ + V ′(φ)
︸ ︷︷ ︸
is this negligible?
∆Φ = 4πGρ
For light scalaron, excitations of f(R)
degree of freedom φ and Newtonian
potential Φ are related:
φ ≈φ∗−2
3Φ
Effective Newton’s constantchanges (non-linearly)!
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 16 / 26
DYNAMICAL COLLAPSE IN F(R) GRAVITY
General spherical symmetric spacetime metric (in Einstein frame):
d s 2 = e −2σ(x ,t )(−d t 2+d x 2) + r 2(x , t )dΩ2
Make a black hole by collapsing a pulse of another scalar field ψ!
4 dynamical equations (in flat metric dγ2 =−d t 2+d x 2):
r 2 = 2e −2σ(1− r 2V (φ), σ= ...
φ+2
r∇r ·∇φ = e −2σ
V ′(φ) +κp
6T [ψ]
ψ+2
r∇r ·∇ψ=
√
√2
3κ
∇φ ·∇ψ
+ 2 constraints (in ∂t x and ∂t t + ∂x x directions)...
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 17 / 26
DYNAMICAL COLLAPSE IN HU-SAWICKI MODEL
0 2 4 6 80
2
4
6
8
10
x
r
Initial value
Final
value
0 2 4 6 8−2
−1
0
1
2
x
σ
Initial value
Final
value
0 2 4 6 80
0.2
0.4
0.6
0.8
1
x
f′
Initial value
Final value
0 2 4 6 8−0.5
0
0.5
1
1.5
2
x
ψ
Initial value
Final value
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 18 / 26
DYNAMICAL COLLAPSE IN STAROBINSKY MODEL
−1.5 −1 −0.5 0 0.5 1−4
−3
−2
−1
0x 10
−6
χ
U(χ)
χ stops at χ = 0.
0.96 0.97 0.98 0.99 1
−3.58
−3.57
−3.56x 10
−6
−0.5 0 0.5 1−4
−3
−2
−1
0x 10
−7
χ
U(χ)
de Sitter point
χ stops at χ = 0.
0 2 4 6 80
0.2
0.4
0.6
0.8
1
x
f′
Initial value
Final value
0 1 2 3 4 5 6 70
1
2
3
4
5
6
7
r = 0
Apparent horizon
x
t
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 19 / 26
INTERIOR SOLUTION IS KASNER! (+ 1 SCALAR)
10−4
10−3
10−2
10−7
10−6
10−5
10−4
r
τnumerical resultsfitting
10−4
10−3
10−2
102
103
104
r
exp(−
2σ)
numerical resultsfitting
10−4
10−3
10−2
10−2
10−1
r
f′
numerical resultsfitting
10−4
10−3
10−2
1.57
1.58
1.59
1.6
1.61
r
ψ
numerical results
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 20 / 26
INTERIOR SOLUTION GOES TO VACUUM
10−4
10−3
10−2
−1011
−1010
−109
−108
−107
rEF
REF
numerical resultsfitting
10−5
10−4
10−3
10−2
10−1
4.5
5
5.5
6x 10
−7
R0(√
D − 1)
rJF
RJF
numerical resultsfitting
10−4
10−3
10−2
108
109
1010
1011
1012
rEF
CEF
numerical resultsfitting
10−3
10−2
10−1
107
108
109
1010
rJF
CJF
numerical resultsfitting
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 21 / 26
KASNER PARAMETERS VARY SPATIALLY
0 1 2 3 4−0.5
0
0.5
1
C
Kasner
parameters
p1 = p2 = p3 = 1/3
q =√
2/3
C =√
3/2 p1p2 = p3q
0 1 2 3 4 5 60
0.5
1
1.5
x
√
2/3
Cq
d s 2 =−dτ2+3∑
i=1
τ2pi d x 2i , φ = q lnτ
∑
pi = 1,∑
p 2i = 1−q 2
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 22 / 26
QUICK SUMMARY
Black holes in modified gravity are emptyinside, but not Schwarzschild-de Sitter!
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 23 / 26
BIG ASTROPHYSICAL QUESTIONS
Where do scalaron hair go after collapse?
How much scalaron radiation is produced?
Back-reaction on matter inbinary black hole collisions?
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 24 / 26
TEST FIELD IN SCHWARZSCHILD BACKGROUND
Schwarzschild-like static background:
d s 2 =−g (r )d t 2+d r 2
g (r )+ r 2 dΩ2
Redefine field and switch to tortoise coordinate:
φ(r, t ) =u (r, t )
r, d r∗ =
d r
g (r )
Then equation of motion becomes flat wave equation with effective mass:
φ =−∂ 2
t + ∂2
r∗−M
r g (r )u (r, t ), M =
g ′g
r
Still self-coupled, but much easier to understand than full collapse...
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 25 / 26
ACCRETION OF SCALARON BY A BLACK HOLE
Where do scalaron hair go after collapse?
Worked it out with José Tomás Gálvez Ghersi& Alex Zucca (SFU), stay tuned for the paper...
They fall down!
Complete spectral accretion code publicly available:https://github.com/andrei-v-frolov/accretion
(see movies attached)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 26 / 26
ACCRETION OF SCALARON BY A BLACK HOLE
Where do scalaron hair go after collapse?
Worked it out with José Tomás Gálvez Ghersi& Alex Zucca (SFU), stay tuned for the paper...
They fall down!
Complete spectral accretion code publicly available:https://github.com/andrei-v-frolov/accretion
(see movies attached)
Andrei Frolov (SFU) Black Holes in Modified Gravity Models CCGRRA-16 26 / 26