## Search

Now showing items 1-8 of 8

#### Gravitational energy as dark energy: Average observational quantities

(University of Canterbury. Physics and Astronomy, 2009)

In the timescape scenario cosmic acceleration is understand as an apparent effect, due to gravitational energy
gradients that grow when spatial curvature gradients become significant with the nonlinear growth of cosmic ...

#### Gravitational energy as dark energy: Average observational quantities

(University of Canterbury. Physics and Astronomy, 2010)

In the timescape scenario cosmic acceleration is understand as an apparent effect, due to gravitational energy
gradients that grow when spatial curvature gradients become significant with the nonlinear growth of cosmic ...

#### From time to timescape: Einstein's unfinished revolution

(University of Canterbury. Physics and Astronomy, 2009)

I argue that Einstein overlooked an important aspect of the relativity of time in never quite realizing his quest to embody Mach’s principle in his theory of gravity. As a step towards that goal, I broaden the Strong ...

#### Cosmic clocks, cosmic variance and cosmic averages

(University of Canterbury. Physics and Astronomy, 2007)

Cosmic acceleration is explained quantitatively, purely in general
relativity with matter obeying the strong energy condition, as an apparent effect
due to quasilocal gravitational energy differences that arise in the ...

#### Cosmic structure, averaging and dark energy

(Cambridge Scientific PublishersUniversity of Canterbury. Physics and Astronomy, 2014)

These lecture notes review the theoretical problems associated with coarse-graining the
observed inhomogeneous structure of the universe at late epochs, of describing average cosmic
evolution in the presence of growing ...

#### Cosmic clocks, cosmic variance and cosmic averages

(University of Canterbury. Physics and Astronomy, 2007)

Cosmic acceleration is explained quantitatively, purely in general
relativity with matter obeying the strong energy condition, as an apparent effect
due to quasilocal gravitational energy differences that arise in the ...

#### Apparent cosmic acceleration from type Ia supernovae

(2017)

Parameters that quantify the acceleration of cosmic expansion are
conventionally determined within the standard
Friedmann-Lema\^{\i}tre-Robertson-Walker (FLRW) model, which fixes spatial
curvature to be homogeneous. ...

#### Dark Energy from Cosmic Structure

(2012)

Below scales of about 100=hMpc our universe displays a complex inhomogeneous structure dominated by voids, with clusters of galaxies in sheets and filaments. The coincidence that cosmic expansion appears to start accelerating ...