Built on

E. J. Copeland, M. Sami, and S. Tsujikawa, Dynamics of dark energy
1936
Earlier work this paper cites.
G. W. Horndeski, Second-order scalar-tensor field equations in a four-dimensional space
1974
Earlier work this paper cites.
H. Kodama and M. Sasaki, Cosmological Perturbation Theory
1984
Earlier work this paper cites.
C.-P. Ma and E. Bertschinger, Cosmological perturbation theory in the synchronous and conformal Newtonian gauges
Original
1995
Earlier work this paper cites.
Supernova Search Team
1998
Earlier work this paper cites.
Supernova Cosmology Project
1999
Earlier work this paper cites.
A. Lewis, A. Challinor, and A. Lasenby, Efficient computation of CMB anisotropies in closed FRW models
2000
Earlier work this paper cites.
J. Weller and A. Lewis, Large scale cosmic microwave background anisotropies and dark energy
2003
Earlier work this paper cites.
W. Hu and I. Sawicki, A Parameterized Post-Friedmann Framework for Modified Gravity
Original
2007
Earlier work this paper cites.
C. Cheung, P. Creminelli, A. L. Fitzpatrick, J. Kaplan, and L. Senatore, The Effective Field Theory of Inflation
Original
2008
Earlier work this paper cites.
C. Skordis, Consistent cosmological modifications to the Einstein equations
Original
2009
Earlier work this paper cites.
M. Park, K. M. Zurek, and S. Watson, A Unified Approach to Cosmic Acceleration
Original
2010
Earlier work this paper cites.

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2013

Simple numerical implementation of general dark energy models

Bloomfield, Jolyon K., Pearson, Jonathan A.

Understand

We present a formalism for the numerical implementation of general theories of dark energy, combining the computational simplicity of the equation of state for perturbations approach with the generality of the effective field theory approach.

An effective fluid description is employed, based on a general action describing single-scalar field models.
The formalism is developed from first principles, and constructed keeping the goal of a simple implementation into CAMB in mind.
Benefits of this approach include its straightforward implementation, the generality of the underlying theory, the fact that the evolved variables are physical quantities, and that model-independent phenomenological descriptions may be straightforwardly investigated.

Built on

E. J. Copeland, M. Sami, and S. Tsujikawa, Dynamics of dark energy
1936
Earlier work this paper cites.
G. W. Horndeski, Second-order scalar-tensor field equations in a four-dimensional space
1974
Earlier work this paper cites.
H. Kodama and M. Sasaki, Cosmological Perturbation Theory
1984
Earlier work this paper cites.
C.-P. Ma and E. Bertschinger, Cosmological perturbation theory in the synchronous and conformal Newtonian gauges
Original
1995
Earlier work this paper cites.
Supernova Search Team
1998
Earlier work this paper cites.
Supernova Cosmology Project
1999
Earlier work this paper cites.
A. Lewis, A. Challinor, and A. Lasenby, Efficient computation of CMB anisotropies in closed FRW models
2000
Earlier work this paper cites.
J. Weller and A. Lewis, Large scale cosmic microwave background anisotropies and dark energy
2003
Earlier work this paper cites.
W. Hu and I. Sawicki, A Parameterized Post-Friedmann Framework for Modified Gravity
Original
2007
Earlier work this paper cites.
C. Cheung, P. Creminelli, A. L. Fitzpatrick, J. Kaplan, and L. Senatore, The Effective Field Theory of Inflation
Original
2008
Earlier work this paper cites.
C. Skordis, Consistent cosmological modifications to the Einstein equations
Original
2009
Earlier work this paper cites.
M. Park, K. M. Zurek, and S. Watson, A Unified Approach to Cosmic Acceleration
Original
2010
Earlier work this paper cites.