the curvature perturbation from vector fields: the vector curvaton case mindaugas karčiauskas...
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![Page 1: The Curvature Perturbation from Vector Fields: the Vector Curvaton Case Mindaugas Karčiauskas Dimopoulos, Karčiauskas, Lyth, Rodriguez, JCAP 13 (2009)](https://reader036.vdocuments.net/reader036/viewer/2022062500/56649d4e5503460f94a2e6d2/html5/thumbnails/1.jpg)
The Curvature Perturbation from Vector Fields: the Vector Curvaton Case
The Curvature Perturbation from Vector Fields: the Vector Curvaton Case
Mindaugas KarčiauskasMindaugas Karčiauskas
Dimopoulos, Karčiauskas, Lyth, Rodriguez, JCAP 13
(2009)
Karčiauskas, Dimopoulos, Lyth, PRD 80 (2009)
Dimopoulos, Karčiauskas, Wagstaff,
arXiv:0907.1838
Dimopoulos, Karčiauskas, Wagstaff,
arXiv:0909.0475
Dimopoulos, Karčiauskas, Lyth, Rodriguez, JCAP 13
(2009)
Karčiauskas, Dimopoulos, Lyth, PRD 80 (2009)
Dimopoulos, Karčiauskas, Wagstaff,
arXiv:0907.1838
Dimopoulos, Karčiauskas, Wagstaff,
arXiv:0909.0475
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Density perturbationsDensity perturbations● Primordial curvature perturbation – a unique
window to the early Universe;
● Origin of structure <= quantum fluctuations;
● Scalar fields - the simplest case;
● Why vector fields:
● Theoretical side:
● No fundamental scalar field has been discovered;
● The possible contribution from gauge fields is neglected;
● Observational side:
● Axis of Evil: alignment of 2-4-8-16 spherical harmonics of CMB;
● Large cold spot, radio galaxy void;
● Primordial curvature perturbation – a unique window to the early Universe;
● Origin of structure <= quantum fluctuations;
● Scalar fields - the simplest case;
● Why vector fields:
● Theoretical side:
● No fundamental scalar field has been discovered;
● The possible contribution from gauge fields is neglected;
● Observational side:
● Axis of Evil: alignment of 2-4-8-16 spherical harmonics of CMB;
● Large cold spot, radio galaxy void;
Land & Magueijo (2005)Land & Magueijo (2005)
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The Vector Curvaton Scenario
The Vector Curvaton Scenario
● The energy momentum tensor ( ):
I. Inflationscale invariant spectrum
II. Light Vector Field
III. Heavy Vector Fieldvector field oscillationsPreasureless isotropic matter:
IV. Vector Field Decay.onset of the Hot Big Bang
● The energy momentum tensor ( ):
I. Inflationscale invariant spectrum
II. Light Vector Field
III. Heavy Vector Fieldvector field oscillationsPreasureless isotropic matter:
IV. Vector Field Decay.onset of the Hot Big Bang
Dimopoulos (2006)Dimopoulos (2006)
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Vector Field PerturbationsVector Field
Perturbations● Massive => 3 degrees of
vector field freedom;
● The power spectra
● The anisotropy parameters of particle production :
● Massive => 3 degrees of vector field freedom;
● The power spectra
● The anisotropy parameters of particle production :
Parity conser-ving
theories:
Parity conser-ving
theories:
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Vector Field PerturbationsVector Field Perturbations
Statistically isotropicStatistically isotropic
Statistically anisotropicStatistically anisotropic
From observations, statistically anisotropic contribution <30%.From observations, statistically anisotropic contribution <30%.
Groeneboom & Eriksen (2009)Groeneboom & Eriksen (2009)
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The Curvature Perturbation
The Curvature Perturbation
● The total curvature perturbation
● The curvature perturbation (δN formula)
, where
● The anisotropic power spectrum of the curvature perturbation:
● For vector field perturbations
● The non-Gaussianity
● The total curvature perturbation
● The curvature perturbation (δN formula)
, where
● The anisotropic power spectrum of the curvature perturbation:
● For vector field perturbations
● The non-Gaussianity
● Current observational constraints:
● Expected from Plank if no detection:
● Current observational constraints:
● Expected from Plank if no detection: Pullen & Kamionkowski (2007)Pullen & Kamionkowski (2007)
Groeneboom & Eriksen (2009)Groeneboom & Eriksen (2009)
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● The vector field power spectra:
● The anisotropy in the power spectrum:
● Non-Gaussianity:
● The vector field power spectra:
● The anisotropy in the power spectrum:
● Non-Gaussianity:
Non-Minimal Vector Curvaton
Non-Minimal Vector Curvaton
●Scale invariance =>
=>=>
1. Anisotropic
2. Modulation is not subdominant
3.
4. Same preferred direction.
5. Configuration dependent modulation.
1. Anisotropic
2. Modulation is not subdominant
3.
4. Same preferred direction.
5. Configuration dependent modulation.
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● At the end of inflation: and .
● Scale invariance:
1. 2.
● 2nd case:
● Small coupling => can be a gauge field;
● Richest phenomenology;
● At the end of inflation: and .
● Scale invariance:
1. 2.
● 2nd case:
● Small coupling => can be a gauge field;
● Richest phenomenology;
Varying Kinetic FunctionVarying Kinetic FunctionSee Jacques’ talk on Wednesday
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Anisotropic
particle production
Anisotropic
particle production
Isotropic
particle production
Isotropic
particle production
Light vector field
Light vector field
Heavy vector field
Heavy vector field
At the end of inflationAt the end of inflation
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● The anisotropy in the power spectrum:
● The non-Gaussianity:
● The parameter space
&
● The anisotropy in the power spectrum:
● The non-Gaussianity:
● The parameter space
&
The Anisotropic Case,
The Anisotropic Case,
1. Anisotropic
2. Modulation is not subdominant
3.
4. Same preferred direction
5. Configuration dependent modulation
1. Anisotropic
2. Modulation is not subdominant
3.
4. Same preferred direction
5. Configuration dependent modulation
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● No scalar fields needed!
● Standard predictions of the curvaton mechanism:
● The parameter space:
● No scalar fields needed!
● Standard predictions of the curvaton mechanism:
● The parameter space:
The Isotropic Case,The Isotropic Case,
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● Vector fields can affect or even generate the curvature perturbation;
● If anisotropic particle production ( ):
● If isotropic particle => no need for production scalar fields
● Two examples: 1.
2.
● Vector fields can affect or even generate the curvature perturbation;
● If anisotropic particle production ( ):
● If isotropic particle => no need for production scalar fields
● Two examples: 1.
2.
ConclusionsConclusions
1. Anisotropic and .
2. Modulation is not subdominant
3. , where
4. Same preferred direction .
5. Configuration dependent modulation.
1. Anisotropic and .
2. Modulation is not subdominant
3. , where
4. Same preferred direction .
5. Configuration dependent modulation.
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Dimopoulos, Karčiauskas, Lyth, Rodriguez, JCAP 13
(2009)
Karčiauskas, Dimopoulos, Lyth, PRD 80 (2009)
Dimopoulos, Karčiauskas, Wagstaff,
arXiv:0907.1838
Dimopoulos, Karčiauskas, Wagstaff,
arXiv:0909.0475
Dimopoulos, Karčiauskas, Lyth, Rodriguez, JCAP 13
(2009)
Karčiauskas, Dimopoulos, Lyth, PRD 80 (2009)
Dimopoulos, Karčiauskas, Wagstaff,
arXiv:0907.1838
Dimopoulos, Karčiauskas, Wagstaff,
arXiv:0909.0475
![Page 14: The Curvature Perturbation from Vector Fields: the Vector Curvaton Case Mindaugas Karčiauskas Dimopoulos, Karčiauskas, Lyth, Rodriguez, JCAP 13 (2009)](https://reader036.vdocuments.net/reader036/viewer/2022062500/56649d4e5503460f94a2e6d2/html5/thumbnails/14.jpg)
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Anisotropy ParametersAnisotropy Parameters
● Anisotropy in the particle production of the vector field:
● Statistical anisotropy in the curvature perturbation:
● Anisotropy in the particle production of the vector field:
● Statistical anisotropy in the curvature perturbation:
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Random Fields with Statistical
Anisotropy
Random Fields with Statistical
Anisotropy
IsotropicIsotropic
- preferred direction- preferred direction
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Present Observational Constrains
Present Observational Constrains
● The power spectrum of the curvature perturbation:
& almost scale invariant;
● Non-Gaussianity from WMAP5 (Komatsu et. al.
(2008)):
● The power spectrum of the curvature perturbation:
& almost scale invariant;
● Non-Gaussianity from WMAP5 (Komatsu et. al.
(2008)):
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δN formalismδN formalism
● To calculate we use formalism (Sasaki, Stewart (1996); Lyth, Malik, Sasaki
(2005));
● Recently in was generalized to include vector field perturbations (Dimopoulos, Lyth,
Rodriguez (2008)):
where , , etc.
● To calculate we use formalism (Sasaki, Stewart (1996); Lyth, Malik, Sasaki
(2005));
● Recently in was generalized to include vector field perturbations (Dimopoulos, Lyth,
Rodriguez (2008)):
where , , etc.
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Estimation of Estimation of ● For subdominant contribution can
be estimated on a fairly general grounds;
● All calculations were done in the limit
● Assuming that one can show that
● For subdominant contribution can be estimated on a fairly general grounds;
● All calculations were done in the limit
● Assuming that one can show that
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Difficulties with Vector Fields
Difficulties with Vector Fields
● Excessive large scale anisotropyThe energy momentum tensor ( ):
● No particle productionMassless U(1) vector fields are conformally
invariant
● Excessive large scale anisotropyThe energy momentum tensor ( ):
● No particle productionMassless U(1) vector fields are conformally
invariant
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Avoiding excessive anisotropyAvoiding excessive anisotropy
● Orthogonal triad of vector fields Ford (1989)
● Large number of identical vector fields Golovnev, Mukhanov, Vanchurin (2008)
● Modulation of scalar field dynamics Yokoyama, Soda (2008)
● Vector curvaton; Dimopoulos (2006)
● Orthogonal triad of vector fields Ford (1989)
● Large number of identical vector fields Golovnev, Mukhanov, Vanchurin (2008)
● Modulation of scalar field dynamics Yokoyama, Soda (2008)
● Vector curvaton; Dimopoulos (2006)
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Particle ProductionParticle Production
● Massless U(1) vector no particle field is conformally => production; invariant
● A known problem in primordial magnetic fields literature;
● Braking conformal invariance:
● Add a potential, e.g.
● Modify kinetic term, e.g.
● Massless U(1) vector no particle field is conformally => production; invariant
● A known problem in primordial magnetic fields literature;
● Braking conformal invariance:
● Add a potential, e.g.
● Modify kinetic term, e.g.
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Stability of the ModelStability of the Model● Two suspected instabilities for longitudinal
mode:1. Ghost; 2. Horizon crossing; 3. Zero
mass;
1.Ghost:
● Only for subhorizon modes:
● Initially no particles & weak coupling;
2.Horizon crossing:
● Exact solution:
● Two suspected instabilities for longitudinal mode:
1. Ghost; 2. Horizon crossing; 3. Zero mass;
1.Ghost:
● Only for subhorizon modes:
● Initially no particles & weak coupling;
2.Horizon crossing:
● Exact solution:Independent constants: