Cosmology Beyond Einstein by Adam Ross Solomon (auth.)

By Adam Ross Solomon (auth.)

This paintings investigates the theoretical and cosmological implications of enhancing Einstein's idea of normal relativity. It explores sessions of adjustments to gravity: these during which the graviton is given a small mass, and people within which Lorentz invariance is spontaneously damaged. It elucidates the character of cosmological perturbations in theories of huge bimetric gravity, together with a in all likelihood lethal instability. Theories of gravity past basic relativity might clarify why the growth of the Universe is accelerating, obviating the necessity for a gloomy strength, and will additionally have an effect on the evolution of the early Universe. subsequent, it investigates the character of spacetime in immense gravity theories that include diversified spacetime metrics. finally, the most powerful constraints to this point are put on the dimensions of Lorentz-violating results within the gravity area in the course of inflation.

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31) where M ≡ M f /Mg . Therefore the f -metric Planck mass is a redundant parameter. We will generally perform this rescaling implicitly in later chapters, although for now we will leave both Planck masses in to help to elucidate some of the physical features of the theory. In terms of free parameters bigravity is simpler than massive gravity: we have traded a constant matrix ( f μν ) for a constant number (M f ) which is not even physically relevant. 7 however that the f -metric cosmological constant, β4 , is physically relevant in bigravity but not in massive gravity, as it is independent of gμν and hence only contributes to the equation of motion for f μν .

In this section we review that history, before moving onto the modern formulations of ghost-free massive gravity and bigravity, and elucidating their cosmological solutions. We refer the reader to [17, 18] for in-depth reviews on massive gravity and its history. 1 Building the Massive Graviton The Fierz–Pauli Mass Term Let us begin by considering linearised gravity described by a spin-2 field, h μν . We will routinely refer to this field as the graviton. 1) gμν = ημν + MPl 1, and keeping in the action only terms quadratic in h μν .

Cosmological parameters. Astron. Astrophys. (2014). 5076 36. D. Baumann, TASI lectures on inflation. 5424 Chapter 2 Gravity Beyond General Relativity Is this quintessence o[r] dust? 2 At the core of this thesis is the question of modifying general relativity. In the previous chapter, we introduced general relativity and its cosmological solutions, culminating in a discussion of two key aspects of the cosmological standard model: CDM at late times and inflation at early times. In this chapter, we extend that discussion to theories of gravity beyond general relativity, and in particular the theories which will receive our attention in this thesis: massive gravity, massive bigravity, and Einstein-aether theory.

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