Talks & Events
Ph.D. Thesis Defenses: 2004
The instabilities of astrophysical flames
Large-scale simulations of supernovae of Type Ia, which are essential for the ultimate understanding of the supernovae mechanism, need flame physics input at three stages: Ignition and early flame propagation, Large scale burning in a turbulent medium, and a transition to detonation, should one occur. The current state of the art in multidimensional calculations is to ignore the first point by simply imposing some already-ignited regions in the domain, and to treat large-scale burning by using a flame speed model which is based on scaling arguments. Very little rigorous work has been done on the third point, on discovering an astrophysically relevant mechanism for deflagration-to- detonation transitions (DDT). The state of terrestrial flame-turbulence research is greatly more sophisticated than the current astrophysical corpus, and we would like to begin placing astrophysical combustion research on the same rigorous footing as terrestrial combustion research. One aspect of our investigation of flame physics has been to examine the behavior of well-known flame instabilities such as Landau-Darrieus in the context of astrophysical flames and degenerate matter. These instabilities can distort and wrinkle the flame surface, increasing the amount of burning and thus the rate of energy input.
Can We See Lorentz-Violating Vector Fields in the CMB?
We investigate the perturbation theory of a fixed-norm, timelike Lorentz-violating vector field. After consistently quantizing the vector field to put constraints on its parameters, we compute the primordial spectra of perturbations generated by inflation in the presence of this vector field. We find that its perturbations are sourced by the perturbations of the inflaton; without the inflaton perturbation the vector field perturbations decay away leaving no primordial spectra of perturbations. Since the inflaton perturbation does not have a spin-1 component, the vector field generically does not generate any spin-1 "vector-type" perturbations. Nevertheless, it will modify the amplitude of both the spin-0 "scalar-type" and spin-2 "tensor-type" perturbation spectra, leading to violations of the inflationary consistency relationship.
Spectral Variability of Quasars in the Sloan Digital Sky Survey II. The C IV Line
Sloan Digital Sky Survey (SDSS) repeat spectroscopic observations have resulted in multiple-epoch spectroscopy for ~2500 quasars observed more than 50 days apart. From this sample, calibrating against stars observed simultaneously, we identify 315 quasars that have varied significantly between observations. We create an ensemble difference spectrum (bright phase minus faint phase) covering rest-frame wavelengths from 1000 Å to 6000 Å. This average difference spectrum is bluer than the average single-epoch quasar spectrum; a power-law fit to the difference spectrum yields a spectral index a l = -2.00, compared to an index of a l = -1.35 for the single-epoch spectrum. The difference spectrum also exhibits very weak or absent emission line features. Due to the lack of variability of the lines, measured photometric color is not always bluer in brighter phases, but depends on redshift and the filters used. Lastly, the difference spectrum is bluer than the ensemble quasar spectrum only for l rest < 2500 Å, indicating that the variability cannot result from a simple scaling of the average quasar spectrum.
We also examine the variability of the high-ionizaton C IVl1549 line in a sample of 105 quasars observed at multiple epochs. We find a strong correlation between the change in the C IV line flux and the change in the line width, but no correlations between the change in flux and changes in line center and skewness. The relation between line flux change and line width change is consistent with a model in which a broad line base varies with greater amplitude than the line core. Using moment analysis line-fitting techniques, we measure line fluxes, centers, widths and skewnesses for the C IV line at two epochs for each object. The well-known Baldwin Effect is seen for these objects, with a slope b = -0.12. The sample has a median intrinsic Baldwin Effect slope of b int = -0.86; the C IV lines in these high-luminosity quasars appear to be less responsive to continuum variations than those in lower luminosity objects. Additionally, we find no evidence for variability of the well known blueshift of the C IV line with respect to the low-ionization Mg IIl2798 line in the highest flux objects, indicating that this might be useful as a measure of orientation.
The dynamics of radiative shock waves: Linear and nonlinear evolution
The stability properties of one-dimensional radiative shocks with a power-law cooling function of the form L 0( r 2 T a are the main subject of this work. The linear analysis originally presented by Chevalier & Imamura, is thoroughly reviewed for several values of the cooling index a and higher overtone modes. Consistently with previous results, it is shown that the spectrum of the linear operator consists in a series of modes with increasing oscillation frequency. For each mode a critical value of the cooling index, a c , can be defined so that modes with a < a c are unstable, while modes with a > a c are stable.
The perturbative analysis is complemented by several numerical simulations to follow the time-dependent evolution of the system for different values of a. Particular attention is given to the comparison between numerical and analytical results (during the early phases of the evolution) and to the role played by different boundary conditions. It is shown that an appropriate treatment of the lower boundary yields results that closely follow the predicted linear behavior. During the nonlinear regime, the shock oscillations saturate at a finite amplitude and tend to a quasi-periodic cycle. The modes of oscillations during this phase do not necessarily coincide with those predicted by linear theory, but may be accounted for by mode-mode coupling.