External Seminars

The following talks take place at DAMTP, the Cavendish Laboratory or the Institute of Astronomy and are not organised by this group. However, they might by related to research that is done within this group at DAMTP.

The Origin of Exozodiacal Dust

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Structure of the inner Milky Way through its red population

As the effect of interstellar extinction in the infrared, using bright red sources it is possible to penetrate the inner disc of the Galaxy. Red clump giants and red supergiants are two particularly useful populations to this aim, as they are bright on the NIR and while the former are dynamically relaxed, the latter trace very recent and massive stellar formation. In this talk I show how, using these stars, we can look for the traces of large structures such as the bar of the Milky Way.

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High Field Magnetic White Dwarfs Simulated in the Laboratory

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Effective constitutive relations and variational principles for waves in composites

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This talk is in MR9, CMS

Evolution of infalling group and cluster galaxies

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Detecting Gravitational Waves (and doing other cool physics) with Millisecond Pulsars

The first millisecond pulsar was discovered in 1982. Since that time their use as highly-accurate celestial clocks has improved continually, so that they are now regularly used to measure a variety of general relativistic effects and probe a variety of topics in basic physics, such as the equation of state of matter at supra-nuclear densities. One of their most exciting uses though, is the current North American (NANOGrav) and international (the International Pulsar Timing Array) efforts to directly detect nanohertz frequency gravitational waves, most likely originating from the ensemble of supermassive black hole binaries scattered throughout the universe. In this talk I’ll describe how we are using an ensemble of pulsars to try to make such a measurement, how we could make a detection within the next 5-10 years, and how we get a wide variety of very interesting secondary science from the pulsars in the meantime.

Galaxy formation on a moving mesh

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X-raying Galaxy Ecosystems

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Cytoplasmic streaming from microfilament self-organisation

Many plant cells exhibit large-scale active circulation of their entire fluid contents, a process termed cytoplasmic streaming. The driving mechanism is known: myosin-coated organelles entrain cytoplasm as they process along actin filament bundles fixed at the periphery. Still unknown, however, is the developmental process which constructs the well-ordered actin configurations required for coherent cell-scale flow. Experiments on streaming regeneration in Characean algal cells, whose longitudinal flow is perhaps the most regimented of all, suggest that microfilament self-organization is at work. We propose a robust model of streaming emergence that combines motor dynamics with both micro- and macroscopic hydrodynamics to explain how several independent processes, each ineffectual on its own, can reinforce to ultimately develop the patterns of streaming observed in the Characeae and other streaming species.

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Merging Galactic, Stellar, and Planetary Dynamics

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Cosmology on a Moving Mesh

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Cold dark matter: cusps and cores

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New Ideas on Mechanisms of Angular Momentum Transport and Variability in Boundary Layers of Accretion Disks

Disk accretion onto a weakly magnetized central object, e.g. a white dwarf or a neutron star, is inevitably accompanied by the formation of a boundary layer near the surface, in which matter slows down from the highly supersonic orbital velocity of the disk to the rotational velocity of the star. Here I will describe a novel, robust mechanism of the angular momentum transport inside the astrophysical boundary layers. Using high resolution 2D and 3D hydrodynamical simulations in the equatorial plane of a boundary layer we generically find that the supersonic shear in the boundary layer excites non-axisymmetric quasi-stationary acoustic modes that are trapped between the surface of the star and a Lindblad resonance in the disk. These modes rotate in a prograde fashion, are stable for hundreds of orbital periods, and have a pattern speed that is less than and of order the rotational velocity at the inner edge of the disk. Dissipation of acoustic modes in weak shocks provides a universal mechanism for angular momentum and mass transport even in purely hydrodynamic (i.e. non-magnetized) boundary layers. Periodicity of these trapped modes may be relevant for explaining the variability seen in accreting compact objects.

Simulations of damped Lyman-alpha systems

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DAMTP Second Year PhD talks

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Astrophysics and Cosmology with Galaxy Clusters: the Role of Simulations

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The Formation Modes of z > 1 Galaxies and their Cosmological Implications

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New solutions of Laplace Tidal Equations over a sphere

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16th Cambridge/Oxford Applied Mathematics Meeting

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aka the Woolly Owl competition

Small Stars in Large Surveys - Large Surveys for Small Stars

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Forming massive seed black holes by direct collapse

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The fluid mechanics wave-particle duality

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The stellar IMF and the earliest phase of the assembly of the Milky Way

The shape of the canonical IMF is briefly reviewed. Using the present day stellar populations in globular clusters as a constraint on their birth configurations these may be compared to observational data on star forming regions. Correlations appear, e.g. between the radius and the shape of the IMF versus the mass of the embedded cluster. Rather remarkable information is unearthed on the very earliest events that shaped the birth of the Milky Way galaxy.

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The Origin of Spirals in Galaxies

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Sackler Lecture 2013

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