How Efficient is Rotational Mixing in Massive Stars ?

The VLT-Flames Survey for Massive Stars (Evans05,Evans06) provides recise measurements of rotational velocities and nitrogen surface abundances of massive stars in the Magellanic Clouds. Specifically, for the first time, such abundances have been estimated for stars with significant rotational velocities. This extraordinary data set gives us the unique possibility to calibrate rotationally and magnetically induced mixing processes. Therefore, we have computed a grid of stellar evolution models varying in mass, initial rotational velocity and chemical composition. In our models we find that although magnetic fields generated by the Spruit-Taylor dynamo are essential to understand the internal angular momentum transport (and hence the rotational behavior), the corresponding chemical mixing must be neglected to reproduce the observations. Further we show that for low metallicities detailed initial abundances are of prime importance, as solar-scaled abundances may result in significant calibration errors.Comment: To appear in the proceedings of "First Stars III", Santa Fe, New Mexico, July 16-20, 2007, 3 pages, 3 figure

How Efficient is Rotational Mixing in Massive Stars ?

The VLT-Flames Survey for Massive Stars (Evans05,Evans06) provides recise measurements of rotational velocities and nitrogen surface abundances of massive stars in the Magellanic Clouds. Specifically, for the first time, such abundances have been estimated for stars with significant rotational velocities. This extraordinary data set gives us the unique possibility to calibrate rotationally and magnetically induced mixing processes. Therefore, we have computed a grid of stellar evolution models varying in mass, initial rotational velocity and chemical composition. In our models we find that although magnetic fields generated by the Spruit-Taylor dynamo are essential to understand the internal angular momentum transport (and hence the rotational behavior), the corresponding chemical mixing must be neglected to reproduce the observations. Further we show that for low metallicities detailed initial abundances are of prime importance, as solar-scaled abundances may result in significant calibration errors.Comment: To appear in the proceedings of "First Stars III", Santa Fe, New Mexico, July 16-20, 2007, 3 pages, 3 figure

Stellar Winds on the Main-Sequence II: the Evolution of Rotation and Winds

Aims: We study the evolution of stellar rotation and wind properties for low-mass main-sequence stars. Our aim is to use rotational evolution models to constrain the mass loss rates in stellar winds and to predict how their properties evolve with time on the main-sequence. Methods: We construct a rotational evolution model that is driven by observed rotational distributions of young stellar clusters. Fitting the free parameters in our model allows us to predict how wind mass loss rate depends on stellar mass, radius, and rotation. We couple the results to the wind model developed in Paper I of this series to predict how wind properties evolve on the main-sequence. Results: We estimate that wind mass loss rate scales with stellar parameters as $\dot{M}_\star \propto R_\star^2 \Omega_\star^{1.33} M_\star^{-3.36}$. We estimate that at young ages, the solar wind likely had a mass loss rate that is an order of magnitude higher than that of the current solar wind. This leads to the wind having a higher density at younger ages; however, the magnitude of this change depends strongly on how we scale wind temperature. Due to the spread in rotation rates, young stars show a large range of wind properties at a given age. This spread in wind properties disappears as the stars age. Conclusions: There is a large uncertainty in our knowledge of the evolution of stellar winds on the main-sequence, due both to our lack of knowledge of stellar winds and the large spread in rotation rates at young ages. Given the sensitivity of planetary atmospheres to stellar wind and radiation conditions, these uncertainties can be significant for our understanding of the evolution of planetary environments.Comment: 26 pages, 14 figures, 2 tables, to be published in A&

Towards a unified model of stellar rotation II: Model-dependent characteristics of stellar populations

Rotation has a number of important effects on the evolution of stars. Apart from structural changes because of the centrifugal force, turbulent mixing and meridional circulation caused by rotation can dramatically affect a star's chemical evolution. This leads to changes in the surface temperature and luminosity as well as modifying its lifetime. Observationally rotation decreases the surface gravity, causes enhanced mass loss and leads to surface abundance anomalies of various chemical isotopes. The replication of these physical effects with simple stellar evolution models is very difficult and has resulted in the use of numerous different formulations to describe the physics. Using stellar evolution calculations based on several physical models we discuss the features of the resulting simulated stellar populations which can help to distinguish between the models.Comment: 14 pages, 13 figures. Accepted for publication in MNRA

The subject and architecture

Invited Presentation on my book Architecture for a Free Subjectivity. In March of 1982, Skyline, the Institute for Architecture and Urban Studies serial, published the landmark interview between Paul Rabinow, an American anthropologist, and Michel Foucault, which would only appear two years later under the title “Space, Knowledge, and Power,” in Rabinow’s edited book The Foucault Reader. Foucault said that in the spatialization of knowledge and power beginning in the 18th century, architecture is not a signifier or metaphor for power, it is rather the “technique for practising social organization.” The role of the IAUS in the architectural dissemination of Foucault’s ideas on the subject and space in the North American academy – such as the concept “heterotopia,” and Foucault’s writing on surveillance and Jeremy Bentham’s Panopticon, subsequently analysed by Georges Teyssot, who was teaching at the Venice School – is well known. Teyssot’s work is part of the historical canalization of Foucauldianism, and French subjectivity more broadly, along its dizzying path, via Italy, to American architecture schools, where it solidified in the 1980s paradigm that would come to be known as American architecture theory. Foucault was already writing on incarceration and prisons, from the 1970s. (In the 1975 lectures he said “architecture was responsible for the invention of madness.”) But this work was not properly incorporated into architectural discussion until the early ’80s. What is not immediately apparent, what this history suggests to me is that subjectivity was not a marginal topic within “theory”, but was perhaps a platform and entry point for architecture theory. One of the ideas that I’m working on is that “theory” can be viewed, historically, as the making of architectural subjectivity, something that can be traced back to the Frankfurt School critique which begins with the modern subject..

A Study of aircraft lateral dynamics & ground stability

The stability of an aircraft on the runway is dependent on many factors. In this thesis, a mathematical model is developed that allows the ground stability and lateral dynamics of an aircraft to be analyzed while it is in the process of taking off or landing. Only two degrees-of-freedom will be considered: lateral displacement and angular rotation. Equations of motion for the model are developed using Newtonian mechanics. The major components of the aircraft that are included in the model are the main landing gear, the vertical tail, and the tail wheel. The model is developed into both linear and non-linear forms. Comparisons are made between a tricycle gear aircraft and a taildragger. Simulations for both the linear and non-linear model are performed to better understand stability. The results of these simulations are used to comment on the applicability of the linear model