ANISOTROPIC PERTURBATIONS DUE TO DARK ENERGY RICHARD BATTYE

ANISOTROPIC PERTURBATIONS DUE TO DARK ENERGY RICHARD BATTYE & ADAM MOSS astro-ph/0602377 JODRELL BANK OBSERVATORY UNIVERSITY OF MANCHESTER

DOMAIN WALL DOMINATED UNIVERSE w = -2/3 DIMENSIONS : ADAM MOSS TALK : SHOWED THERE EXIST LOCALLY STABLE CONFIGURATIONS BUT THEY DON'T APPEAR TO BE ATTRACTORS IN THE SIMPLE MODELS WE CONSIDERED – WORK CONTINUES

PLAN OF TALK ● MOTIVATION ● COSMOLOGICAL PERTURBATIONS THE STANDARD LORE SCALAR-VECTOR-TENSOR SPLIT ● ELASTIC DARK ENERGY (THE MODEL FORMERLY KNOWN AS SOLID DARK MATTER/ENERGY) BASIC IDEA ISOTROPIC AND ANISOTROPIC ELASTICITY SPEED SOUND FOR CUBIC SYMMETRY ● ANISOTROPIC PERTURBATIONS ANISOTROPY FROM ADIABATIC INITIAL CONDITIONS ANALYTIC & NUMERICAL CALCULATIONS CORRELATED MODES ON LARGE SCALES ●

ALIGNMENT IN CMB MAPS D'Oliveria-Costa et al Alignment of the l=2 and l=3 multipoles Eriksen et al North-South ratio of Ppower spectrum & 3 -pt correlation fn Land & Magueijo “Axis of Evil” correlated multipoles

BIANCHI TYPE VIIh UNIVERSE WMA P (T. Jaffe et al) BASIC IDEA ADD STANDARD ADIABATIC MODEL AND BEST FITTING BIANCHI TEMPLATE BIANCHI MODEL WMAP -BIANCHI now compatible with Gaussianity and isotropy

SCALAR-VECTOR-TENSOR SPLIT ENERGY-MOMENTUM TENSOR SCALAR VECTOR VELOCITY : ANISOTROPIC STRESS : SCALAR VECTOR TENSOR

LAGRANGIAN, EM TENSOR STANDARD ASSUMPTION ACTION : EM-TENSOR : STANDARD DEFINITIONS RELATIVISTIC ELASTICITY TENSOR : HENCE PARAMETERIZES FLUID PERTS THEORY DEVELOPED BY CARTER AND OTHERS IN 1970 s TO MODEL NEUTRON STAR

STANDARD ELASTICITY TENSOR } 3+1 SPLIT WHERE LAGRANGIAN & EULERIAN PERTURBATIONS STANDARD : 21 COMPONENTS 1 BULK MODULUS 20 SHEAR MODULI EULERIAN LAGRANGIAN

ISOTROPY (BUCHER & SPERGEL 1998, BATTYE, BUCHER & SPERGEL 1999) NB w=0, IS CDM ISOTROPIC TENSORS P = PRESSURE DOMAIN WALLS = BULK MODULUS w = -2/3 STABILITY = SHEAR MODULUS SOUND SPEEDS LONGITUDINAL (SCALAR) TRANSVERSE (VECTOR) ADIABATIC

POINT SYMMETRIES POSSIBLE SYMMETRIES ARE CLASSIFIED BY THE BRAVAIS LATTICES eg FROM LANDAU & LIFSCHITZ EG CUBIC CASE PRESSURE ISOTROPIC : ELASTICITY TENSOR : NON-ZERO MODULI TRICLINIC MONOCLINIC ORTHORHOMIBIC TETRAGONAL RHOMBOHEDRAL HEXAGONAL CUBIC ISOTROPIC 18 12 9 6 6 5 3 2 WHERE 1 = xx, 2 = yy, 3 = zz 4 = xy, 5 =yz, 6 = zx BULK MODULUS + 2 SHEAR MODULI

(BATTYE, CHACHOUA & MOSS 200 VARIABLE SOUND SPEEDS : SIMPLE CUBE FCC BCC

ANISOTROPY FROM ADIABATIC PERTS - ie. FROM INFLATION ● INITIAL CONDITIONS THOSE USED FOR INFLATION ● POWER SERIES SOLUTION ● "WOULD-BE SCALAR MODE" CUBIC SYMMETRY

TIME EVOLUTION : -1 SCALAR VECTOR TENSOR VELOCITY METRIC PERTS

SPATIAL DISTRIBUTION : k=0. 001 Mpc WHERE -1

AMPLITUDE OF EFFECT

CMB ANISOTROPIES : IN PROGRESS ROTATION ANISOTROPIC SYMMETRY ADAPTED (COMPUTE SPHERICAL HARMONICS (SASH) USING CAMB)eg VON DE LAGE & BETHE 1947 EXAMPLE OF SASH : l =4

CONCLUSIONS ● PERTURBATIONS IN DARK ENERGY ARE IMPORTANT ● ADIABATIC ELASTIC DARK ENERGY MODELS CAN BE STABLE ● THERE APPEAR TO BE ALIGNMENTS IN THE CMB ● QUALITATIVELY, THEY MAYBE DUE TO ANISOTROPIC DARK EN ● WE HAVE INVESTIGATED THE CASE OF CUBIC SYMMETRY ● NEXT (AND VERY IMPORTANT STEP) IS TO COMPUTE ● THEN WE CAN INVESTIGATE THE FIT TO THE DATA ● NB ONE IS NOT RESTRICTED TO CUBIC SYMMETRY