Anisotropic Cosmological Model with a Generalized Chaplygin Gas

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Finsler GeometryFinsler geometry may be considered as a generalizedRiemannian .can be considered as a physical geometry on which matterdynamic takes place while Riemannian geometry is thegravitational geometry.connect the Riemannian metric structure of the space-time tophysical vector fieldsA long range vector field of cosmological origin is consideredin relation to a physical geometry where the Cartanconnection has a fundamental role
an electromagnetic field or a gauge vector field may emergeout by a physical source of the universecan be incorporated into the geometry causing an anisotropicstructureSo the geometrical anisotropies are caused byinternal variables.The variation of anisotropy is expressed in terms of theCartan torsion tensor of the Finslerian manifold
Page 1 and 2: Anisotropic Cosmological Modelwith
Page 3: Mathematical FormalismA Generalized
Page 7 and 8: The induced Finslerian metric tenso
Page 9 and 10: In the framework of Finsler geometr
Page 11 and 12: *The equation of the geodesics is g
Page 13 and 14: •A Finsler space is a Riemanian s
Page 15 and 16: Field equations in both formalisms
Page 17 and 18: Conclusion N°1With the same fluid
Page 19 and 20: Conclusion N°2With the same fluid
Page 21 and 22: Exact solutionsH ( t)3= " µ H43! =
Page 23 and 24: w = 0!""chapchapmmAPwP= #=If2000000
Page 25 and 26: 0,0220,020mu/H 0=-0.01a(t)0,0180,01
Page 27 and 28: q-120mu/H 0=-0.01-140-160-180-200-2
Page 29 and 30: 0,0002mu/H 0=0.010,0000-0,0002-0,00
Page 31 and 32: If$Ptottot= $= P+ !(t)" !(t)1!(t)=
Page 33 and 34: !!!!!!!!µµ+""++#+"+=$12010)(11201
Page 35 and 36: If"m* 01A)3(&'34µH2(1 + )0H0%#$1+!
Page 37 and 38: alpha=0.41,000,950,900,850,800,750,
Page 39 and 40: !!!!"#$$$$%&++=+= '= ''= 'µµµ(((
Page 41 and 42: Conservation of momentum-energystre
Page 43 and 44: 1,20mu/H 0=-0.021,151,10density rho
Page 45 and 46: Model3Friedman like equats.8 !G = 1
Page 47 and 48: Near the critical point one can wri
Page 49 and 50: 0))ln(31exp(66)(1)(0)())ln(31)exp((
Page 51 and 52: From Numerical solutions of dynamic
Page 53 and 54: 0mu/H 0=-0.01-20ln(abs(Pchap )-40-6
Page 55 and 56:
))3(1(21411))(3(2)3(1))3(1(6143)(3)
Page 57 and 58:
µ!!µ!µ!!µ!µ!!!µ!!µµ!3)52152
Page 60 and 61:
)(4 113532122123321311241!!!!!!!bbb
Page 62 and 63:
Eigenvalues:""12==! TrM! TrM22+ ( t
Page 64 and 65:
A general fourth order theory of gr
Page 66 and 67:
)]44)(2(ˆˆˆ)4()ˆ[2(4]ˆ31)(219[
Page 68 and 69:
•(b) Shear, distortion in shape w
Page 70 and 71:
)]4347()26[()](3)(3)(9))()([2()(1ˆ
Page 72 and 73:
*The shear tensor measures any tend
Page 74 and 75:
Conclusions:The goal is:• Undrsta
Page 76:
Thank You
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Anisotropic Cosmological Model with a Generalized Chaplygin Gas

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