8,129 research outputs found
Foundations of Quantum Gravity : The Role of Principles Grounded in Empirical Reality
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 (merely) rely heavily on theoretical arguments for their
justification. These remarks are illustrated in terms of the current standard
models of cosmology and particle physics, as well as their respective
underlying theories, viz. general relativity and quantum (field) theory. 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 (analogous to the
manner in which, say, the idea that gravitation is a curved spacetime
phenomenon is arguably implied by the equivalence principle). It is
subsequently argued that the appropriate empirical principles for quantum
gravity should at least include (i) quantum nonlocality, (ii) irreducible
indeterminacy, (iii) the thermodynamic arrow of time, (iv) 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.Comment: 21 pages. Some (mostly minor) corrections. Final published versio
The Origin of Chaos in the Outer Solar System
Classical analytic theories of the solar system indicate that it is stable,
but numerical integrations suggest that it is chaotic. This disagreement is
resolved by a new analytic theory. The theory shows that the chaos among the
Jovian planets results from the overlap of the components of a mean motion
resonance among Jupiter, Saturn, and Uranus, and provides rough estimates of
the Lyapunov time (10 million years) and the dynamical lifetime of Uranus
(10^{18} years). The Jovian planets must have entered the resonance after all
the gas and most of the planetesimals in the protoplanetary disk were removed.Comment: 19 pages, 3 figures, to appear in Scienc
A possible contribution to CMB anisotropies at high l from primordial voids
We present preliminary results of an analysis into the effects of primordial
voids on the cosmic microwave background (CMB). We show that an inflationary
bubble model of void formation predicts excess power in the CMB angular power
spectrum that peaks between 2000 < l < 3000. Therefore, voids that exist on or
close to the last scattering surface at the epoch of decoupling can contribute
significantly to the apparent rise in power on these scales recently detected
by the Cosmic Background Imager (CBI).Comment: 5 pages, 3 figures. MNRAS accepted versio
First order resonance overlap and the stability of close two planet systems
Motivated by the population of multi-planet systems with orbital period
ratios 1<P2/P1<2, we study the long-term stability of packed two planet
systems. The Hamiltonian for two massive planets on nearly circular and nearly
coplanar orbits near a first order mean motion resonance can be reduced to a
one degree of freedom problem (Sessin & Ferraz Mello (1984), Wisdom (1986),
Henrard et al. (1986)). Using this analytically tractable Hamiltonian, we apply
the resonance overlap criterion to predict the onset of large scale chaotic
motion in close two planet systems. The reduced Hamiltonian has only a weak
dependence on the planetary mass ratio, and hence the overlap criterion is
independent of the planetary mass ratio at lowest order. Numerical integrations
confirm that the planetary mass ratio has little effect on the structure of the
chaotic phase space for close orbits in the low eccentricity (e <~0.1) regime.
We show numerically that orbits in the chaotic web produced primarily by first
order resonance overlap eventually experience large scale erratic variation in
semimajor axes and are Lagrange unstable. This is also true of the orbits in
this overlap region which are Hill stable. As a result, we can use the first
order resonance overlap criterion as an effective stability criterion for pairs
of observed planets. We show that for low mass (<~10 M_Earth) planetary systems
with initially circular orbits the period ratio at which complete overlap
occurs and widespread chaos results lies in a region of parameter space which
is Hill stable. Our work indicates that a resonance overlap criterion which
would apply for initially eccentric orbits needs to take into account second
order resonances. Finally, we address the connection found in previous work
between the Hill stability criterion and numerically determined Lagrange
instability boundaries in the context of resonance overlap.Comment: Accepted for publication in Ap
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