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Series: CDSNS Colloquium

We investigate deterministic superdiusion in nonuniformly hyperbolic system
models in terms of the convergence of rescaled distributions to the normal
distribution following the abnormal central limit theorem, which differs
from the usual requirement that the mean square displacement grow
asymptotically linearly in time. We obtain an explicit formula for the
superdiffusion constant in terms of the ne structure that originates in the
phase transitions as well as the geometry of the configuration domains of
the systems. Models that satisfy our main assumptions include chaotic
Lorentz gas, Bunimovich stadia, billiards with cusps, and can be apply to
other nonuniformly hyperbolic systems with slow correlation decay rates of
order O(1/n)

Series: CDSNS Colloquium

Upon quantization, hyperbolic Hamiltonian systems generically exhibit
universal spectral properties effectively described by Random
Matrix Theory. Semiclassically this remarkable phenomenon can be
attributed to the existence of pairs of classical periodic orbits
with small action differences. So far, however, the scope of this
theory has, by and large, been restricted to single-particle systems.
I will discuss an extension of this program to hyperbolic
coupled map lattices with a large number of sites (i.e., particles).
The crucial ingredient is a two-dimensional symbolic dynamics which
allows an effective representation of periodic orbits and their
pairings. I will illustrate the theory with a specific model of
coupled cat maps, where such a symbolic dynamics can be constructed
explicitly.

Series: CDSNS Colloquium

A metric on the 2-torus T^2 is said to be "Liouville" if in some coordinate system it has the form ds^2 = (F(q_1) + G(q_2)) (dq_1^2 + dq_2^2). Let S^*T^2 be the unit cotangent bundle.A "folklore conjecture" states that if a metric is integrable (i.e. the union of invariant 2-dimensional tori form an open and dens set in S^*T^2) then it is Liouville: l will present a counterexample to this conjecture.Precisely I will show that there exists an analytic, non-separable, mechanical Hamiltonian H(p,q) which is integrable on an open subset U of the energy surface {H=1/2}. Moreover I will show that in {H=1/2}\U it is possible to find hyperbolic behavior, which in turn means that there is no analytic first integral on the whole energy surface.This is a work in progress with V. Kaloshin.

Series: CDSNS Colloquium

The Parameterization Method
is a functional analytic framework for studying invariant manifolds
such as stable/unstable manifolds of periodic orbits and invariant
tori. This talk will focus on numerical applications such as computing
manifolds associated with long periodic orbits, and computing periodic
invariant circles (manifolds consisting of several disjoint circles
mapping one to another, each of which has an iterate conjugate to an
irrational rotation). I will also illustrate how to combine Automatic
Differentiation with the Parameterization Method to simplify problems
with non-polynomial nonlinearities.

Series: CDSNS Colloquium

We shall take a look at computer-aided techniques that can be
used to prove the existence of stationary solutions of radially
symmetric PDEs. These techniques combine existing numerical methods with
functional analytic estimates to provide a computer-assisted proof by
means of the so-named 'radii-polynomial' approach.

Series: CDSNS Colloquium

Series: CDSNS Colloquium

We consider a restricted four-body problem, modeling the dynamics of a
light body (e.g., a moon) near a Jupiter trojan asteroid. We study two
mechanisms of instability. For the first mechanism, we assume that the
orbit of Jupiter is circular, and we investigate the hyperbolic invariant
manifolds associated to periodic orbits around the equilibrium points. The
conclusion is that the light body can undergo chaotic motions inside the
Hill sphere of the trojan, or well outside that region. For the second
mechanism, we consider the perturbative effect due to the eccentricity of
the orbit of Jupiter. The conclusion is that the size of the orbit of the
light body around the trojan can keep increasing, or keep decreasing, or
undergo oscillations. This phenomenon is related to the Arnold Diffusion
problem in Hamiltonian dynamics

Series: CDSNS Colloquium

In this talk, I will present new models to describe the evolution of games. Our dynamical system models are inspired by the Fokker-Planck equations on graphs. We will present properties of the models, their connections to optimal transport on graphs, and computational examples for generalized Nash equilibria. This presentation is based on a recent joint work with Professor Shui-Nee Chow and Dr. Wuchen Li.

The shape sphere: a new vista on the three body problem (David Alcaraz conference: Video conference)

Series: CDSNS Colloquium

Video Conference David Alcaraz confernce. Newton's famous three-body problem defines dynamics on the space of
congruence classes of
triangles in the plane. This space is a three-dimensional non-Euclidean
rotationally symmetric metric space ``centered'' on the shape sphere.
The shape sphere is
a two-dimensional sphere whose points represent oriented similarity
classes of planar triangles.
We describe how the sphere arises from the three-body problem
and encodes its dynamics. We will see how the classical solutions of
Euler and Lagrange,
and the relatively recent figure 8 solution are encoded as points or curves
on the sphere. Time permitting, we will show how the sphere pushes us
to formulate natural topological-geometric questions about three-body
solutions and
helps supply the answer to some of these questions. We may take a brief
foray into the planar N-body problem
and its associated ``shape sphere'' : complex projective N-2 space.

Series: CDSNS Colloquium

Dynamical systems have proven to be a useful tool for the design of space missions. For instance, the use of invariant manifolds is now common to design transfer strategies. Solar Sailing is a proposed form of spacecraft propulsion, where large membrane mirrors take advantage of the solar radiation pressure to push the spacecraft. Although the acceleration produced by the radiation pressure is smaller than the one achieved by a traditional spacecraft it is continuous and unlimited. This makes some long term missions more accessible, and opens a wide new range of possible applications that cannot be achieved by a traditional spacecraft. In this presentation we will focus on the dynamics of a Solar sail in a couple of situations. We will introduce this problem focusing on a Solar sail in the Earth-Sun system. In this case, the model used will be the Restricted Three Body Problem (RTBP) plus Solar radiation pressure. The effect of the solar radiation pressure on the RTBP produces a 2D family of "artificial'' equilibria, that can be parametrised by the orientation of the sail. We will describe the dynamics around some of these "artificial'' equilibrium points. We note that, due to the solar radiation pressure, the system is Hamiltonian only for two cases: when the sail is perpendicular to the Sun - Sail line; and when the sail is aligned with the Sun - sail line (i.e., no sail effect). The main tool used to understand the dynamics is the computation of centre manifolds. The second example is the dynamics of a Solar sail close to an asteroid. Note that, in this case, the effect of the sail becomes very relevant due to the low mass of the asteroid. We will use, as a model, a Hill problem plus the effect of the Solar radiation pressure, and we will describe some aspects of the natural dynamics of the sail.