Name Title=Mr First Name=David Surname=Nicholls Institution=RSAA ANU Email Address=david@mso.anu.edu.au Student=on Title= Abstract= 13th March=on 14th March=on Workshop Dinner=on NOTE: would like to bring fiance to the Friday dinner as well. Name Title=Dr First Name=Charles Surname=Lineweaver Institution=ANU Email Address=charley@mso.anu.edu.au Presentation=on Title=Entropy, Gravity and Life in the Universe Abstract=I will describe our on-going attempts to relate gravitational collapse to entropy and the biological requirements for free energy. See Lineweaver & Egan 2008. 13th March=on 14th March=on Name Title=Dr First Name=Rosemary Surname=Mardling Institution=Monash University Email Address=mardling@sci.monash.edu.au Presentation=on Title=Stellar and planetary dynamics at Monash Abstract=I will give an overview of work done at Monash on stellar and planetary dynamics. Applications include extrasolar planets, the galactic centre, star clusters, and the three-body problem. 13th March=on 14th March=on Workshop Dinner=on Name Title=Dr First Name=Paul Surname=Lasky Institution=Swinburne University Email Address=plasky@astro.swin.edu.au Presentation=on Title=Shape, shear and flexion: Weak gravitational lensing effects on extended sources Abstract=Weak gravitational lensing is fast becoming a precision tool for extragalactic and cosmological astrophysics. Traditionally, weak lensing is studied by analysing the ellipticities of source galaxies using a linear expansion of the thin-lens gravitational lens equation. Here, an elliptic source is mapped to an elliptic image, and one simply measures the convergence, shear and magnification of the image relative to the source. It has recently been shown that expanding the thin-lens equation to higher-order allows an investigation into the change of shape of the image with respect to the source, an effect coined 'flexion'. Flexion is an additional measurement of weak lensing that makes no implicit assumptions about the source galaxy. I discuss our investigations of flexion in systems with varying degrees of complexity; from single lens models with analytic solutions to ray-tracing through large cosmological Nbody simulations. I discuss how each of these systems can be compared with observations, both current and future, to learn more about the nature of the dark sector of the Universe. 13th March=on Name Title=Prof First Name=Geoffrey Surname=Bicknell Institution=RSAA, ANU Email Address=geoff@mso.anu.edu.au Presentation=on Title=Feedback from Jets in AGN Abstract=Feedback from AGN-driven outflows may be necessary in order to explain the cut off in star formation in massive galaxies at high redshift. Can this be driven by AGN jets? Initially this was thought to be difficult in view of the bipolar morphology of classical radio galaxies. However, we have shown that a jet propagating through an inhomogeneous interstellar medium exhibits quite a different morphology from the classic case. I will present a number of simulations, which illustrate the range of possible physical interactions. In some cases the details of the interaction are pertinent to a class of radio galaxies known as Gigahertz Peak Spectrum Radio Sources. This latter class of source may be representative of the feedback interaction invoked to explain the Magorrian relation between black hole mass and bulge mass. 13th March=on 14th March=on Workshop Dinner=on Name Title=Mr First Name=Benjamin Surname=Barsdell Institution=Centre for Astrophysics and Supercomputing, Swinburne University of Technology Email Address=bbarsdel@astro.swin.edu.au Student=Yes Presentation=No Poster=No Presentation Title: - Abstract: - 13th March=on 14th March=on Workshop Dinner=on Name Title=Dr. First Name=Daniel Surname=Price Institution=CSPA, Monash University Email Address=daniel.price@sci.monash.edu.au Presentation=on Title=Magnetic fields in star formation Abstract=Magnetic fields are important at all levels of the star formation process all the way from galaxies to stars. However incorporating their effects into numerical simulations is challenging. I will discuss the role of magnetic fields at a range of scales in the star formation process, presenting recent results from numerical simulations that are able to resolve the formation of whole star clusters incorporating the effects of both magnetic fields and radiation. 13th March=on 14th March=on Workshop Dinner=on Name Title=Dr First Name=Darren Surname=Croton Institution=Swinburne Email Address=dcroton@astro.swin.edu.au Presentation=on Title=Semi-analytic models of galaxy formation Abstract= 13th March=on 14th March=on Workshop Dinner=on Name Title=Dr First Name=Maria Surname=Lugaro Institution=Monash Email Address=Maria.Lugaro@sci.monash.edu.au Presentation=off Title= Abstract= 13th March=on 14th March=on Workshop Dinner=on Title: Dr Name: Jarrod Surname: Hurley Institution: Swinburne E-mail: jhurley@swin.edu.au Student: NO Presentation: NO Poster: NO Presentation Title: Abstract: Attend on the 13th: YES Attend on the 14th: NO Attend dinner: YES Title: Dr Name: Peter Surname: McGregor Institution: RSAA/ANU E-mail: Peter.McGregor@anu.edu.au Student: NO Presentation: YES Poster: NO Presentation Title: Accretion and Outflow in Young Stellar Objects Abstract: Disk accretion in Young Stellar Objects is known to be time-variable, and so is the outflow activity as seen in Herbig-Haro objects on large scale. I will describe plans to model disk accretion through magnetic winds in collaboration with Raquel Salmeron. We hope to relate variations in near-infrared emission features arising in the disk atmosphere through accretion to the ejection of new jet structures to be detected at high angular resolution with NIFS on Gemini North. This should demonstrate whether the disk emission features can be formed by magnetic heating in the disk atmosphere, and show how directly variations in accretion activity are related to ejection events. Attend on the 13th: YES Attend on the 14th: YES Attend dinner: NO Title: Dr Name: Gregory Surname: Poole Institution: Swinburne E-mail: gpoole@astro.swin.edu.au Student: NO Presentation: YES Poster: NO Presentation Title: The Swinburne Centenary WiggleZ (SCWiggleZ) Simulations Abstract: I will describe a suite of very large cosmological dark matter simulations being run at Swinburne for the purposes of studying galaxy formation and large scale structure. Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Dr Name: Robert Surname: Crain Institution: Swinburne E-mail: rcrain@astro.swin.edu.au Student: NO Presentation: YES Poster: NO Presentation Title: Hydro simulations of galaxies, groups and clusters Abstract: I will review progress made in the GIMIC and OWLS cosmological gasdynamical simulations, focussing on environmental aspects of galaxy formation and the evolution of intergalactic and intracluster gas. Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Dr Name: Sarah Surname: Maddison Institution: Swinburne E-mail: smaddison@swin.edu.au Student: NO Presentation: YES Poster: NO Presentation Title: Grain growth in protoplanetary disksGrain growth in protoplanetary disks Abstract: In order to understand the first stages of planet formation, when tiny grains aggregate to form planetesimals, one needs to simultaneously model grain growth, vertical settling and radial migration of dust in protoplanetary disks. We have implemented an analytical prescription for grain growth bycoagulation, which assumes that grains stick perfectly upon collision, into our 3D, two-phase (gas+dust) SPH code. We then follow the evolution of the size and spatial distribution of a dust population in a classical T Tauri star disk, and discuss the implications of the combined effects of grain growth coupled with dust settling and radial migration on subsequent planetesimal formation. Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Dr Name: Raquel Surname: Salmeron Institution: ANU E-mail: raquel@mso.anu.edu.au Student: NO Presentation: YES Poster: NO Presentation Title: Jets and winds from young stellar objects Abstract: A common feature of astrophysical accreting systems is their association with powerful outflows that become supersonic, and highly collimated, as they accelerate away from the source. Their ubiquity suggests that these outflows play a role in regulating accretion, a notion strengthened by the observed correlation between accretion and outflow signatures in these objects. It is also generally accepted that these winds are accelerated centrifugally from the surfaces of the accretion disk that surrounds the source, and provide an efficient means of carrying away the excess angular momentum of the accreted matter. In my talk I will review the launching mechanism and properties of outflows associated with young stellar objects, present realistic models that take account of the disk structure and discuss their observational implications. Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Dr Name: Amanda Surname: Karakas Institution: Australian National University E-mail: akarakas@mso.anu.edu.au Student: NO Presentation: NO Poster: NO Presentation Title: Abstract: Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Dr Name: Bruce Surname: Peterson Institution: RSAA, ANU E-mail: peterson@mso.anu.edu.au Student: NO Presentation: NO Poster: NO Presentation Title: Abstract: Attend on the 13th: YES Attend on the 14th: YES Attend dinner: NO Title: Ms Name: Melissa Surname: Ness Institution: ANU E-mail: mkness@mso.anu.edu.au Student: YES Presentation: NO Poster: NO Presentation Title: Abstract: Attend on the 13th: YES Attend on the 14th: YES Attend dinner: NO Title: Mrs. Name: Katie Surname: Howard Institution: Macquarie University E-mail: khoward@ics.mq.edu.au Student: YES Presentation: YES Poster: YES Presentation Title: Analytic continuation of Spacetime Metrics Abstract: I propose a detailed discussion about the general problem of analyticity in current Spacetime physics, with the aim of understanding the Spacetime global structure and testing the cosmic censorship hypothesis. As a particular case, I bring some remarks about axially and spherically symmetric spacetimes. Exact solutions of the Einstein-Maxwell equations in a cosmological background and their further continuation beyond the event horizons are discussed. The general possibility and various methods of analytic extension of spacetime metrics are reviewed, with particular attention to solutions that lead to naked singularities, providing counterexamples to the cosmic censorship hypothesis. I consider formal continuation of different metrics to the region within the event horizon, from the “imaginary time” of the Lorentzian metric within Euclidean geometries to multi-black-hole solutions. We comment on a potential instability inside the horizon within the setting of a topologically complicated conformal spacetime. Attend on the 13th: YES Attend on the 14th: YES Attend dinner: NO Title: Dr Name: Frank Surname: Mills Institution: ANU E-mail: frank.mills@anu.edu.au Student: NO Presentation: YES Poster: NO Presentation Title: Observations and Modelling of Chemistry in Venus\' Atmosphere Abstract: Observations by instruments on Europe\'s Venus Express spacecraft and ground-based telescopes have provided much higher quality imaging and spectroscopy than previously existed. These observations have led to a number of discoveries over the past couple years. A selection of these observations will be discussed along with related numerical modelling. Attend on the 13th: YES Attend on the 14th: NO Attend dinner: NO Title: Mr Name: Peter Surname: Dobbie Institution: The University of Sydney E-mail: p.dobbie@physics.usyd.edu.au Student: YES Presentation: YES Poster: NO Presentation Title: GLOBAL 3D RADIATIVE MHD SIMULATIONS OF BLACK HOLE DISK ACCRETION AND OUTFLOWS Abstract: Accretion occurs throughout the Universe, driving the evolution of stars and galaxies and, in the case of accretion onto a black hole, providing Nature\'s most efficient known energy source: It is widely believed to power active galactic nuclei, gamma-ray bursts and some X-ray binaries. Despite analytical and numerical advances in accretion disk theory, a self-consistent explanation for the high mass accretion rates inferred for the most luminous sources and for the jets and outflows seen across the mass range of accreting objects has not been established. We describe new global 3D radiative and resistive MHD simulations we are developing to test a theory which mutually resolves these outstanding issues by modelling the effect on the disk dynamics of the vertical transport of angular momentum. Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Dr Name: Jackie Surname: Cooper Institution: Australian National University E-mail: jcooper@mso.anu.edu.au Student: NO Presentation: YES Poster: NO Presentation Title: Starburst-Driven Winds: Filament Formation and Emission Processes Abstract: Perhaps the most spectacular feature of starburst-driven winds are the line emitting filaments that extend along the minor axis of the host galaxy. Recent three-dimensional simulations of these winds (Cooper et al. 2008) have suggested that the filaments are formed by clouds of disk gas that are accelerated into the outflow by the ram-pressure of the wind. However, adiabatic simulations of the interaction of a supersonic wind with such a cloud indicate that it may be destroyed by hydrodynamical instabilities within short time frame. In order to better understand how a cloud could survive being accelerated into an outflow to form a filament, I have performed a series of high resolution simulations of the interaction of a single radiative fractal cloud interacting with a supersonic wind. I will present the results of these simulations and discuss the mechanism behind the survival of the filaments. I will also discuss what these simulations predict for the origin of t! he H-alpha and soft X-ray emission in starburst winds. Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Mr. Name: Loren Surname: Bruns Jr. Institution: University of Melbourne E-mail: l.brunsjr@pgrad.unimelb.edu.au Student: YES Presentation: NO Poster: NO Presentation Title: Abstract: Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Miss Name: Andrea Surname: Ruff Institution: Univeristy of Melbourne E-mail: aruff@unimelb.edu.au Student: YES Presentation: YES Poster: NO Presentation Title: TBA Abstract: TBA Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Mr Name: Stephen Surname: Petrie Institution: University of Melbourne E-mail: s.petrie@pgrad.unimelb.edu.au Student: YES Presentation: NO Poster: NO Presentation Title: Abstract: Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Mr Name: Mohammad Surname: Rafat Institution: School of Physics, The University of Sydney E-mail: rafat@physics.usyd.edu.au Student: YES Presentation: YES Poster: NO Presentation Title: Theory of Linear Acceleration Emission of Radio Pulsars Abstract: The electrodynamics of pulsars involves pair creation in the polar cap regions, and a recent model involves oscillatory pair production, with the oscillations associated with a large amplitude electrostatic wave (LAEW) (Luo and Melrose 2008). Electrons and positrons are accelerated to very high Lorentz factors in the LAEW, and as a result they emit linear acceleration emission (LAE). In this talk we present an analytical investigation of the dynamics of charged particles subject to LAEW and derive their velocity and trajectory exactly. We demonstrate that LAEW leads to relativistic pulsar winds consisting of pair plasma. We then derive the current due to a highly relativistic particle and use it to obtain the power spectrum. From the power spectrum we identify the cut-off frequency for linear acceleration emission in a LAEW in the hard X-ray. Our results show that LAE in a LAEW is a valid candidate for explaining pulsar radio and X-ray emissions, but it cannot expl! ain gamma-ray emissions. Attend on the 13th: YES Attend on the 14th: YES Attend dinner: NO Title: Mr First Name: Maxim Surname: Priymak Institution: University of Melbourne Email Address: m.priymak@pgrad.unimelb.edu.au Student: YES Presentation: YES Presentation Title: Neutron Star Magnetic Mountains: Realistic Mass-flux and Equation of State Abstract: Recent X-ray observations of recycled neutron stars (NS) in binary systems indicate a narrow range of spin frequencies, centred on ~300 Hz. Bayesian analysis predicts a maximum spin frequency of ~760 Hz of this X-ray pulsar sub-population. This is in direct contradiction to the prevailing evolutionary paradigm of these systems. A magnetically confined "mountain" of accreted matter at the magnetic poles of the NS can stall NS spin-up via gravitational radiation and accretion torque balance. Here we study how the eqn of state (EoS) of nuclear matter affects the max spin freq attained. We model an EoS containing various thermal and degenerate pressure contributions as well as composion altering nuclear reactions. A semi-phenomenological comparison of the mountain with this EoS with regards to an ideal isothermal EoS is made and is found to extend further from the NS surface. A 2D magnetohydrostatic simulation suite is modified for a preliminary adiabatic EoS. Equilibrium mountain configuration will interact with the NS magnetosphere and result in an altered accretion rate/mass flux on the NS surface, providing a feedback to the magnetic mountain equilibrium. A collaboration with Cornell university has been commenced to compute this interaction. Attend on the 13th March: YES Attend on the 14th March: YES Attend dinner: YES Title: Dr Name: Chiaki Surname: Kobayashi Institution: RSAA, ANU E-mail: chiaki@mso.anu.edu.au Student: NO Presentation: YES Poster: NO Presentation Title: Chemodynamical simulation of galaxies Abstract: We simulate the formation and evolution of galaxies including star formation, supernova feedback, and chemical enrichment. The star formation rate is enough suppressed to meet the observations, and heavy elements are distributed to the intergalactic medium by the galactic winds. In the Milky Way Galaxy, the evolution of elemental abundance ratios are in great agreement with observations. Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Dr Name: Qinghuan Surname: Luo Institution: USyd E-mail: luo@physics.usyd.edu.au Student: NO Presentation: NO Poster: NO Presentation Title: Abstract: Attend on the 13th: YES Attend on the 14th: YES Attend dinner: YES Title: Dr Name: Alexander Surname: Wagner Institution: ANU, RSAA E-mail: ayw@mso.anu.edu.au Student: NO Presentation: YES Presentation Title: Cosmic-ray shocks in Tycho's supernova remnant Abstract: Young supernova remnants (SNR), including Tycho's remnant, are believed to accelerate cosmic ray (CR) nuclei up to TeV energies. CR particles are accelerated in shocks and their large energy densities lead to modifications to the shock structure, in particular, the formation of a CR shock precursor. Using hydrodynamic shock models we investigate whether the faint Halpha emission ahead of a Balmer-dominated filament in Tycho's SNR is due to a CR precursor. Attend on 13th: YES Attend on 14th: YES Attend dinner: YES (if possible)