Silicon monoxide (SiO) maser emission has been observed towards many late-type stars. The conditions necessary for the formation of SiO masers dictate that they be produced in a region which is inside the silicate dust formation point close to the surface of the star. Very Long Baseline Interferometry (VLBI) has shown that these masers do indeed lie close to the stellar surface at a distance of a few stellar radii. This extended atmosphere is a complex region dominated by stellar pulsations and permeated by circumstellar shocks. This dissertation presents the results of a multi-epoch VLBI study of the v=1, J=1-0, 43-GHz SiO maser emission towards the symbiotic binary R Aquarii. Four epochs of full-polarization observations were recorded using the Very Long Baseline Array a facility the National Radio Astronomy Observatory. The first high-resolution images of the extended atmosphere of a Mira variable in a symbiotic binary have been produced. The SiO masers towards R Aquarii have been found to exhibit a ring-like morphology ~31 mas (~6.8 AU) in diameter. The emission changes significantly over a time period of ~1-2 months with almost no similarity in structure on timescales >6 months. An analysis of the four epochs of observations has provided the first direct evidence of SiO maser proper motions. These observations, taken as the Mira variable approached maximum light, show that over a 98-day period the masers have an average inward proper motion of ~1 mas. This contraction of the maser shell implies an infall velocity of ~4 km/s for the SiO masers during this phase of the stellar pulsation cycle. In addition to the total intensity images, maps of the linear and circular polarization morphology were also produced. These images show that the SiO masers are significantly polarized, and that the polarization structure and intensity change on timescales as short as ~1-2 months. For three of the four epochs, a mean fractional circular polarization of 4% was determined implying a magnetic field strength Bsec(theta) = 13 G. For one of the four epochs, the mean fractional circular polarization was found to be ~14% indicating a magnetic field strength Bsec(theta) = 46 G. The fractional linear polarization is fairly constant for all four epochs with mean values ranging from 20.8-25.0%, and peak values as high as ~83% for isolated maser features. Maps of the linear polarization vectors show an orderly structure over large portions of the maser shell indicating a uniform magnetic field topology in these regions of the extended atmosphere of R Aquarii. / Ph. D.

The Department of Homeland Security reports that over 90% of cyberattacks stem from security vulnerabilities in software, costing the U.S. $109 billion dollars in damages in 2016 alone according to The White House. As NIST estimates that today's software contains 25 bugs for every 1,000 lines of code, the prompt discovery of security flaws is now vital to mitigating the next major cyberattack. Over the last decade, the software industry has overwhelmingly turned to a lightweight defect discovery approach known as fuzzing: automated testing that uncovers program bugs through repeated injection of randomly-mutated test cases. Academic and industry efforts have long exploited the semantic richness of open-source software to enhance fuzzing with fast and fine-grained code coverage feedback, as well as fuzzing-enhancing code transformations facilitated through lightweight compiler-based instrumentation. However, the world's increasing reliance on closed-source software (i.e., commercial, proprietary, and legacy software) demands analogous advances in automated security vetting beyond open-source contexts. Unfortunately, the semantic gaps between source code and opaque binary code leave fuzzing nowhere near as effective on closed-source targets. The difficulty of balancing coverage feedback speed and precision in binary executables leaves fuzzers frequently bottlenecked and orders-of-magnitude slower at uncovering security vulnerabilities in closed-source software. Moreover, the challenges of analyzing and modifying binary executables at scale leaves closed-source software fuzzing unable to fully leverage the sophisticated enhancements that have long accelerated open-source software vulnerability discovery. As the U.S. Cybersecurity and Infrastructure Security Agency reports that closed-source software makes up over 80% of the top routinely exploited software today, combating the ever-growing threat of cyberattacks demands new practical, precise, and performant fuzzing techniques unrestricted by the availability of source code. This thesis answers the following research questions toward enabling fast, effective fuzzing of closed-source software: 1. Can common-case fuzzing insights be exploited to more achieve low-overhead, fine-grained code coverage feedback irrespective of access to source code? 2. What properties of binary instrumentation are needed to extend performant fuzzing-enhancing program transformation to closed-source software fuzzing? In answering these questions, this thesis produces the following key innovations: A. The first code coverage techniques to enable fuzzing speed and code coverage greater than source-level fuzzing for closed-source software targets. (chapter 3) B. The first instrumentation platform to extend both compiler-quality code transformation and compiler-level speed to closed-source fuzzing contexts (chapter 4) / Doctor of Philosophy / The Department of Homeland Security reports that over 90% of cyberattacks stem from security vulnerabilities in software, costing the U.S. $109 billion dollars in damages in 2016 alone according to The White House. As NIST estimates that today's software contains 25 bugs for every 1,000 lines of code, the prompt discovery of security flaws is now vital to mitigating the next major cyberattack. Over the last decade, the software industry has overwhelmingly turned to lightweight defect discovery through automated testing, uncovering program bugs through the repeated injection of randomly-mutated test cases. Academic and industry efforts have long exploited the semantic richness of open-source software (i.e., software whose full internals are publicly available, interpretable, and changeable) to enhance testing with fast and fine-grained exploration feedback; as well as testing-enhancing program transformations facilitated during the process by which program executables are generated. However, the world's increasing reliance on closed-source software (i.e., software whose internals are opaque to anyone but its original developer) like commercial, proprietary, and legacy programs demands analogous advances in automated security vetting beyond open-source contexts. Unfortunately, the challenges of understanding programs without their full source information leaves testing nowhere near as effective on closed-source programs. The difficulty of balancing exploration feedback speed and precision in program executables leaves testing frequently bottlenecked and orders-of-magnitude slower at uncovering security vulnerabilities in closed-source software. Moreover, the challenges of analyzing and modifying program executables at scale leaves closed-source software testing unable to fully leverage the sophisticated enhancements that have long accelerated open-source software vulnerability discovery. As the U.S. Cybersecurity and Infrastructure Security Agency reports that closed-source software makes up over 80% of the top routinely exploited software today, combating the ever-growing threat of cyberattacks demands new practical, precise, and performant software testing techniques unrestricted by the availability of programs' source code. This thesis answers the following research questions toward enabling fast, effective fuzzing of closed-source software: 1. Can common-case testing insights be exploited to more achieve low-overhead, fine-grained exploration feedback irrespective of access to programs' source code? 2. What properties of program modification techniques are needed to extend performant testing-enhancing program transformations to closed-source programs? In answering these questions, this thesis produces the following key innovations: A. The first techniques enabling testing of closed-source programs with speed and exploration higher than on open-source programs. (chapter 3) B. The first platform to extend high-speed program transformations from open-source programs to closed-source ones (chapter 4)

Yes / Gender archaeology has made significant strides toward deconstructing the hegemony of binary categorizations. Challenging dichotomies such as man/woman, sex/gender, and biology/culture, approaches informed by poststructuralist, feminist, and queer theories have moved beyond essentialist and universalist identity constructs to more nuanced configurations. Despite the theoretical emphasis on context, multiplicity, and fluidity, binary starting points continue to streamline the spectrum of variability that is recognized, often reproducing normative assumptions in the evidence. The contributors to this special issue confront how sex, gender, and sexuality categories condition analytical visibility, aiming to develop approaches that respond to the complexity of theory in archaeological practice. The papers push the ontological and epistemological boundaries of bodies, personhood, and archaeological possibility, challenging a priori assumptions that contain how sex, gender, and sexuality categories are constituted and related to each other. Foregrounding intersectional approaches that engage with ambiguity, variability, and difference, this special issue seeks to “de-contain” categories, assumptions, and practices from “binding” our analytical gaze toward only certain kinds of persons and knowledges, in interpretations of the past and practices in the present.

W Ursae Majoris-type (W UMa-type) variable stars are contact eclipsing binary stars whose evolution is unknown. Modelling to determine the physical parameters of as many W UMa-type variable stars as possible might provide some insight as to how these contact binaries form and evolve. The All Sky Automated Survey (ASAS) has discovered over ve thousand of these systems. Using data from the ASAS and from the Wide Angle Search for Planets (SuperWASP) project, models of selected ASAS contact binaries are being created to determine their physical parameters. Some W UMa-type variable stars are known to undergo changes in orbital period. For selected ASAS contact binaries, a period analysis has been performed using SuperWASP data to determine if the systems are undergoing changes in orbital period. Results of the modelling and period analyses of selected systems are presented. / Thesis (M. Sc. (Astronomy))

We report the direct imaging detection of a low-mass companion to a young, moderately active star V450. And, that was previously identified with the radial velocity (RV) method. The companion was found in high-contrast images obtained with the Subaru Telescope equipped with the HiCIAO camera and AO188 adaptive optics system. From the public ELODIE and SOPHIE archives we extracted available high-resolution spectra and RV measurements, along with RVs from the Lick planet search program. We combined our multi-epoch astrometry with these archival, partially unpublished RVs, and found that the companion is a low-mass star, not a brown dwarf, as previously suggested. We found the best-fitting dynamical masses to be m(1) = 1.141(-0.091)(+0.037)and m(2) = 0.279(-0.020)(+0.023) M-circle dot. We also performed spectral analysis of the SOPHIE spectra with the iSpec code. Hipparcos time-series photometry shows a periodicity of P = 5.743 day, which is also seen in the SOPHIE spectra as an RV modulation of the star A. We interpret it as being caused by spots on the stellar surface, and the star to be rotating with the given period. From the rotation and level of activity, we found that the system is 380(-100)(+220) Myr old, consistent with an isochrone analysis (220(-90)(+2120) Myr). This work may serve as a test case for future studies of low-mass stars, brown dwarfs, and exoplanets by combination of RV and direct imaging data.

We compile observations of early-type binaries identified via spectroscopy, eclipses, long-baseline interferometry, adaptive optics, common proper motion, etc. Each observational technique is sensitive to companions across a narrow parameter space of orbital periods P and mass ratios q. =. M-comp/M-1. After combining the samples from the various surveys and correcting for their respective selection effects, we find that the properties of companions to O-type and B-type main-sequence (MS) stars differ among three regimes. First, at short orbital periods P less than or similar to 20. days (separations a less than or similar to 0.4 au), the binaries have small eccentricities e... 0.4, favor modest mass ratios < q > less than or similar to 0.5, and exhibit a small excess of twins q. >. 0.95. Second, the companion frequency peaks at intermediate periods log P (days). approximate to. 3.5 (a approximate to 10 au), where the binaries have mass ratios weighted toward small values q. approximate to 0.2-0.3 and follow a Maxwellian " thermal" eccentricity distribution. Finally, companions with long orbital periods log P (days). approximate to 5.5-7.5 (a approximate to 200-5000 au) are outer tertiary components in hierarchical triples and have a mass ratio distribution across q. approximate to 0.1-1.0 that is nearly consistent with random pairings drawn from the initial mass function. We discuss these companion distributions and properties in the context of binary-star formation and evolution. We also reanalyze the binary statistics of solar-type MS primaries, taking into account that 30% +/-. 10% of single-lined spectroscopic binaries likely contain white dwarf companions instead of low-mass stellar secondaries. The mean frequency of stellar companions with q. >. 0.1 and log P (days). <. 8.0 per primary increases from 0.50. +/- 0.04 for solar-type MS primaries to 2.1. +/- 0.3 for O-type MS primaries. We fit joint probability density functions f (M-1, q, P, e) not equal f (M-1) f (q) f (P) f (e) to the corrected distributions, which can be incorporated into binary population synthesis studies.

Thesis (M. Sc.)--University of Canterbury, 2008. / Typescript (photocopy). Includes bibliographical references (p. 66-68).

W Ursae Majoris-type (W UMa-type) variable stars are contact eclipsing binary stars whose evolution is unknown. Modelling to determine the physical parameters of as many W UMa-type variable stars as possible might provide some insight as to how these contact binaries form and evolve. The All Sky Automated Survey (ASAS) has discovered over ve thousand of these systems. Using data from the ASAS and from the Wide Angle Search for Planets (SuperWASP) project, models of selected ASAS contact binaries are being created to determine their physical parameters. Some W UMa-type variable stars are known to undergo changes in orbital period. For selected ASAS contact binaries, a period analysis has been performed using SuperWASP data to determine if the systems are undergoing changes in orbital period. Results of the modelling and period analyses of selected systems are presented. / Thesis (M. Sc. (Astronomy))

We use the multi-epoch radial velocities acquired by the Apache Point Observatory Galactic Evolution Experiment (APOGEE) survey to perform a large-scale statistical study of stellar multiplicity for field stars in the Milky Way, spanning the evolutionary phases between the main sequence (MS) and the red clump. We show that the distribution of maximum radial velocity shifts (Delta RVmax) for APOGEE targets is a strong function of log g, with MS stars showing Delta RVmax as high as similar to 300 km s(-1), and steadily dropping down to similar to 30 km s(-1) for log g similar to 0, as stars climb up the red giant branch (RGB). Red clump stars show a distribution of Delta RVmax values comparable to that of stars at the tip of the RGB, implying they have similar multiplicity characteristics. The observed attrition of high Delta RVmax systems in the RGB is consistent with a lognormal period distribution in the MS and a multiplicity fraction of 0.35, which is truncated at an increasing period as stars become physically larger and undergo mass transfer after Roche Lobe overflow during H-shell burning. The Delta RVmax distributions also show that the multiplicity characteristics of field stars are metallicity-dependent, with metal-poor ([Fe/H] less than or similar to -0.5) stars having a multiplicity fraction a factor of 2-3 higher than metal-rich ([Fe/H] less than or similar to 0.0) stars. This has profound implications for the formation rates of interacting binaries observed by astronomical transient surveys and gravitational wave detectors, as well as the habitability of circumbinary planets.

Many young, massive stars are found in close binaries. Using population synthesis simulations. we predict the likelihood of a companion star being present when these massive stars end their lives as core-collapse supernovae (SNe). We focus on stripped-envelope SNe, whose progenitors have lost their outer hydrogen and possibly helium layers before explosion. We use these results to interpret new Hubble Space Telescope observations of the site of the broad-lined Type. Ic SN 2002ap, 14 years post-explosion. For a subsolar metallicity consistent with SN 2002ap, we expect a main-sequence (MS) companion present in about two thirds of all stripped-envelope SNe and a compact companion (likely a stripped helium star or a white dwarf/neutron star/black hole) in about 5% of cases. About a quarter of progenitors are single at explosion (originating from initially single stars, mergers, or disrupted systems). All of the latter scenarios require a massive progenitor, inconsistent with earlier studies of SN 2002ap. Our new, deeper upper limits exclude the presence of an MS companion star > 8-10 M., ruling out about 40% of all stripped-envelope SN channels. The most likely scenario for SN 2002ap includes nonconservative binary interaction of a primary star initially. 23 M.. Although unlikely (< 1% of the scenarios), we also discuss the possibility of an exotic reverse merger channel for broadlined Type. Ic events. Finally, we explore how our results depend on the metallicity and the model assumptions and discuss how additional searches for companions can constrain the physics that govern. the evolution of SN progenitors.