This chapter addresses philosophical questions raised in contemporary work on cosmology. It provides an overview of the Standard Model for cosmology and argues that its deficiency in addressing theories regarding the very early universe can be resolved by introducing a dynamical phase of evolution that eliminates the need for a special initial state. The chapter also discusses recent hypotheses about dark matter and energy, issues that it relates to philosophical debates about underdetermination.

The law of gravitation, an example of physical law The relation of mathematics to physics The great conservation principles Symmetry in physical law The distinction of past and future Probability and uncertainty: the quantum mechanical view of nature Seeking new laws.

The existence of a thermodynamic arrow of time in the present universe implies that the initial state of the observable portion of our universe at the tt"big bangtt" must have been very tt"specialtt". We argue that it is not plausible that these special initial conditions have a dynamical origin.

When attempting to assess the strengths and weaknesses of various principles in their potential role of guiding the formulation of a theory of quantum gravity, it is crucial to distinguish between principles which are strongly supported by empirical data – either directly or indirectly – and principles which instead rely heavily on theoretical arguments for their justification. Principles in the latter category are not necessarily invalid, but their a priori foundational significance should be regarded with due caution. These remarks are (...) illustrated in terms of the current standard models of cosmology and particle physics, as well as their respective underlying theories, i.e., essentially general relativity and quantum theory. For instance, it is clear that both standard models are severely constrained by symmetry principles: an effective homogeneity and isotropy of the known universe on the largest scales in the case of cosmology and an underlying exact gauge symmetry of nuclear and electromagnetic interactions in the case of particle physics. However, in sharp contrast to the cosmological situation, where the relevant symmetry structure is more or less established directly on observational grounds, all known, nontrivial arguments for the “gauge principle” are purely theoretical. Similar remarks apply to the larger theoretical structures represented by general relativity and quantum theory, where – actual or potential – empirical principles, such as the equivalence principle or EPR-type nonlocality, should be clearly differentiated from theoretical ones, such as general covariance or renormalizability. It is argued that if history is to be of any guidance, the best chance to obtain the key structural features of a putative quantum gravity theory is by deducing them, in some form, from the appropriate empirical principles. Theoretical principles may still be useful however in formulating a concrete theory. It is subsequently argued that the appropriate empirical principles for deducing the key structural features of quantum gravity should at least include quantum nonlocality, irreducible indeterminacy, relativistic causality), the thermodynamic arrow of time, homogeneity and isotropy of the observable universe on the largest scales. In each case, it is explained – when appropriate – how the principle in question could be implemented mathematically in a theory of quantum gravity, why it is considered to be of fundamental significance and also why contemporary accounts of it are insufficient. For instance, the high degree of uniformity observed in the Cosmic Microwave Background is usually regarded as theoretically problematic because of the existence of particle horizons, whereas the currently popular attempts to resolve this situation in terms of inflationary models are, for a number of reasons, less than satisfactory. However, rather than trying to account for the required empirical features dynamically, an arguably much more fruitful approach consists in attempting to account for these features directly, in the form of a lawlike initial condition within a theory of quantum gravity. (shrink)