learning with pierre: from branes to gravity · revival of « massive gravity » via the vainshtein...
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Learning with Pierre:
from branes to gravity
Dire ici que pas tout est présenté
Cédric Deffayet
(IAP and IHÉS, CNRS Paris)
Les Houches 1999
« the primordial Universe »
APC, May the 3rd 2018
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• Frank Thuiller 1991 (Sur certains aspects géométriques des théories conformes bidimensionnelles)
• Emilian Dudas 1994 (Mécanismes de brisure de supersymétrie)
• François Pillon 1995 (Étude de la brisure de symétries dans des théories de cordes et de supergravité)
• Stéphane Lavignac 1997 (Le problème des hiérachies de masse dans les modèles supersymétriques)
• C.D. 2000 (Aspects cosmologiques des théories de supercordes)
• Jean-François Dufaux 2004 (Modèles branaires en théories de gravité généralisées)
• Leonardo Sala 2009 (Search for beyond the standard model physics at the CMS experiment : supersymmetry and extra dimensions)
• Alejandro Bohé 2011 (Production d'ondes gravitationnelles par les cordes cosmiques avec jonctions)
• Alexis Helou 2015 (Beyond the trapping horizon : the apparent universe & the regular black hole)
• Mauro Pieroni 2016 (Classification des modèles d’inflation et contraintes sur la physique fondamentale)
The PhD students of Pierre
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• Frank Thuiller 1991 (Sur certains aspects géométriques des théories conformes bidimensionnelles)
• Emilian Dudas 1994 (Mécanismes de brisure de supersymétrie)
• François Pillon 1995 (Étude de la brisure de symétries dans des théories de cordes et de supergravité)
• Stéphane Lavignac 1997 (Le problème des hiérachies de masse dans les modèles supersymétriques)
• C.D. 2000 (Aspects cosmologiques des théories de supercordes)
• Jean-François Dufaux 2004 (Modèles branaires en théories de gravité généralisées)
• Leonardo Sala 2009 (Search for beyond the standard model physics at the CMS experiment : supersymmetry and extra dimensions)
• Alejandro Bohé 2011 (Production d'ondes gravitationnelles par les cordes cosmiques avec jonctions)
• Alexis Helou 2015 (Beyond the trapping horizon : the apparent universe & the regular black hole)
• Mauro Pieroni 2016 (Classification des modèles d’inflation et contraintes sur la physique fondamentale)
The PhD students of Pierre
Cosmology
Gravitation
High energy
theoretical physics
Cosmology
Gravitation
High energy
theoretical physics
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Pierre was first my professor at the ENS (in 1993) where he was teaching
(special) relativity and then at the « master 2 » « CPM »
Promotion 1996 (thanks to F. Derue)
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Then my PhD director at Orsay LPT on
« Cosmological aspects of superstring theories »
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« Second string revolution »
and discovery of the string web of dualities
Brane-localized
degrees of freedom
Role played there by
« D(irichlet)-branes »
ADS-CFT correspondance (Maldacena)
1994-
1997-
Scientific context:
High energy theory
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1998- Discovery of the acceleration of the expansion of the Universe
(SCP and HZT teams 1998, Nobel prize 2011)
2001- Launch of WMAP mission (june 2001)
Advent of « Precision cosmology »
Scientific context:
Cosmology
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Very good timing for the
interests of Pierre !
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I started my PhD
in sept 1997….
… after one year….
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Today: I am going to discuss some long lasting fruits of a
simple equation obtained in our paper of 1999 : (the most cited paper of Pierre with more than 1000 citations)
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Today: I am going to discuss some long lasting fruits of a
simple equation obtained in our paper of 1999 : (the most cited paper of Pierre with more than 1000 citations)
19 years today !
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Today: I am going to discuss some long lasting fruits of a
simple equation obtained in our paper of 1999 : (the most cited paper of Pierre with more than 1000 citations)
Brane cosmology
Brane gravity
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1998- Arkani-Hamed, Dimopoulos, Dvali (ADD) brane worlds
1999- Randall-Sundrum (RS) models
2000- Dvali-Gabadadze-Porrati (DGP) models
« brane-worlds »
Usual space-time
(4 dimensions):
that of a brane gravity
Bulk space-time has
4+n dimensions
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This result is obtained by perturbation
theory (with a localized source)
I.e. one solves for h¹ º defined by
g¹ º = g(0)¹ º + h¹ º
Background
metric
Metric on the brane
Small perturbation
« generated » by a
localized matter
source
In ADD or RS brane worlds, the gravity potential V(r) between brane
localized sources behaves as in 3+1 dimensions at large distances
Einstein equations
Newton constant GNewton
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This result is obtained by perturbation
theory (with a localized source)
I.e. one solves for h¹ º defined by
g¹ º = g(0)¹ º + h¹ º
Background
metric
Metric on the brane
Small perturbation
« generated » by a
localized matter
source
In ADD or RS brane worlds, the gravity potential V(r) between brane
localized sources behaves as in 3+1 dimensions at large distances
Einstein equations
Contains brane localized sources
Newton constant GNewton
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This result is obtained by perturbation
theory (with a localized source)
I.e. one solves for h¹ º defined by
g¹ º = g(0)¹ º + h¹ º
Background
metric
Metric on the brane
Small perturbation
« generated » by a
localized matter
source
In ADD or RS brane worlds, the gravity potential V(r) between brane
localized sources behaves as in 3+1 dimensions at large distances
Newton constant GNewton
Einstein equations
Not suitable for cosmology !
Contains brane localized sources
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The brane localized matter is only sensitive
to the “curvature” of the metric on the
brane (and not the one of the bulk) …
… i.e. to the “intrinsic curvature” of the
surface mesured e.g. by G (4) .
The embedding of the surface into the
defines a so called “extrinsic curvature”
measured by a tensor K
Ex: vs.
Some space geometry !
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Geometrical relations between
•5D curvature: GAB(5)
•Intrinsic curvature (4D) : G (4)
•Extrinsic curvature: K
5D Curvature
Intrinsic
curvature Quadratic in the
extrinsic curvature
Generalized Gauss identities:
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1/ By equating the distributional source, we get:
Using this decomposition into Einstein equations (with
a distributional source)
Extrinsic
Curvature Energy-momentum
tensor »
2/ Inserting this is the generalized Gauss identities we find
Kown by the buk
Einstein equations Quadratic in S¹ º ( or ) » H2 + …
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I.e. we get
Or in cosmology
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This applies generically to brane worlds (of codimension 1)
E.g. 1.: Randall-Sundrum model (bulk is AdS5)
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E.g. 2.: Dvali-Gabadadze-Porrati (DGP 2000) model (bulk is Minkowski5)
The Newton potential (computed perturbatively) behaves as
However this is mediated by a resonance of massive gravitons
and hence
Pertubation theory :
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E.g. 2.: Dvali-Gabadadze-Porrati (DGP 2000) model (bulk is Minkowski5)
Cosmology (applying the technique of our 1999 paper) :
Equating the distributional source in the 5D Einstein equation
still yields
Inserting this is the generalized Gauss identities
But now
We get now a quadratic equation for the Hubble factor H
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(C.D. 2000)
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First concrete proposal to link the acceleration of the expansion
of the Universe to a large distance modification of gravity
(CD 2000; CD, Dvali, Gabadadze 2001)
« Modified gravity » and « cosmology » (from WoS)
« Modified gravity » (from WoS)
2000
2000
2016
2016
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Lead to a new phenomenology of scalar-tensor theories via the
« Galileons » and friends.
The DGP model has a strong coupling in the scalar
sector (CD, Dvali, Gabadadze, Vainshtein, 2002)
This can be extracted taking a « decoupling limit »
yielding a scalar theory with second order quadratic
equations of motions
(Luty, Porrati, Rattazzi, 2003)
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Lead to a new phenomenology of scalar-tensor theories via the
« Galileons » and friends.
The DGP model has a strong coupling in the scalar
sector (CD, Dvali, Gabadadze, Vainshtein, 2002)
This can be extracted taking a « decoupling limit »
yielding a scalar theory with second order quadratic
equations of motions
(Luty, Porrati, Rattazzi, 2003)
(
(Together with )
This quadratic structure comes from the generalized Gauss identities
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Generalized to Galileons (Nicolis, Rattazzi, Trincherini, 2009),
covariant Galileons (CD, Esposito-Farese, Vikman, 2009) ,
and the more recent « Beyond Horndeski » theories (Zumalacarregui, Garcia-Bellido, 2014; Gleyzes, Langlois, Piazza,
Vernizzi, 2015)
Lead to a new phenomenology of scalar-tensor theories via the
« Galileons » and friends.
The DGP model has a strong coupling in the scalar
sector (CD, Dvali, Gabadadze, Vainshtein, 2002)
This can be extracted taking a « decoupling limit »
yielding a scalar theory with second order quadratic
equations of motions
(Luty, Porrati, Rattazzi, 2003)
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Revival of « massive gravity » via the Vainshtein mechanism
(First) attempt to give a mass to the graviton:
Fierz and Pauli 1939
A massive and a massless graviton yield drastically
different physical results (e.g. for light bending) (van Dam, Veltman; Zakharov; Iwasaki, 1970)
A way out was suggested by Vainshtein in 1972
Criticized and new obstructions found by Boulware and
Deser in 1972
The DGP cosmology provided the first hint in favour of the
Vainshtein mechanism (CD,Dvali, Gabadadze, Vainshtein 2001)
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This lead to new efforts in the search of a consistent theory of
massive gravity using in particular the equivalent of the
decoupling limit of DGP model (Creminelli, Nicolis, Papucci, Trincherini, 2005; CD, Rombouts, 2005)
First explicit proof that the Vainshtein mechanism is working as
expected in massive gravity (Babichev, CD, Ziour, 2009)
Discovery of a family of massive gravity theory devoid of the
Boulware Deser pathologies (de Rham, Gabadadze 2010; de Rham, Gabadadze, Tolley, 2011)
2000
2016
« Massive gravity » (from WoS)
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Back to 1999
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GPS (of the GDR): « Groupe de Priorité Supersymétrique » …
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Not to be confused with the « Groupe de Pelotons de Sécurité »
(20 april 1999: « affaire des Paillottes » in Corsica …)
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Not to be confused with the « Groupe de Pelotons de Sécurité »
(20 april 1999: « affaire des Paillottes » in Corsica …)
Cargèse, Corsica
summer 1998
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Working under the supervision of
Pierre was very inspiring !
On the physics side,
he was always optimistic !
And also very pleasant on the human side!
We miss him a lot….