Massive star winds are understood to be structured. Structures can come in the form of co-rotating interaction regions, which are globally organized flow streams that thread the winds. Structures can also be stochastic in nature, generically referred to as "clumps". The theory for interpreting the radio emissions from randomly distributed microclumps in single star winds is established. Results are presented here for macroclumping, in which the radiative transfer is sensitive to the clump geometry. Two cases are compared: spherical clumps and pancake-like fragments. The geometry of macroclumps can influence the power-law slope of the long wavelength spectral energy distribution.

The Polstar mission will provide for a space-borne 60cm telescope operating at UV wavelengths with spectropolarimetric capability capturing all four Stokes parameters (intensity, two linear polarization components, and circular polarization). Polstar’s capabilities are designed to meet its goal of determining how circumstellar gas flows alter massive stars' evolution, and finding the consequences for the stellar remnant population and the stirring and enrichment of the interstellar medium, by addressing four key science objectives. In addition, Polstar will determine drivers for the alignment of the smallest interstellar grains, and probe the dust, magnetic fields, and environments in the hot diffuse interstellar medium, including for the first time a direct measurement of the polarized and energized properties of intergalactic dust. Polstar will also characterize processes that lead to the assembly of exoplanetary systems and that affect exoplanetary atmospheres and habitability. Science driven design requirements include: access to ultraviolet bands: where hot massive stars are brightest and circumstellar opacity is highest; high spectral resolution: accessing diagnostics of circumstellar gas flows and stellar composition in the far-UV at 122-200nm, including the NV, SiIV, and CIV resonance doublets and other transitions such as NIV, AlIII, HeII, and CIII; polarimetry: accessing diagnostics of circumstellar magnetic field shape and strength when combined with high FUV spectral resolution and diagnostics of stellar rotation and distribution of circumstellar gas when combined with low near-UV spectral resolution; sufficient signal-to-noise ratios: ~103 for spectropolarimetric precisions of 0.1% per exposure; ~102 for detailed spectroscopic studies; ~10 for exploring dimmer sources; and cadence: ranging from 1-10 minutes for most wind variability studies, to hours for sampling rotational phase, to days or weeks for sampling orbital phase. The ISM and exoplanet science program will be enabled by these capabilities driven by the massive star science.

Dans le milieu interstellaire, parmi les 200 molécules observées, les hydrocarbures sont présents en abondance. La formation des hydrocarbures CHy(+) se fait entre un C+ et un atome d'hydrogène ou une molécule. Par la suite, ces hydrocarbures réagissent entre eux pour former des hydrocarbures plus gros. Ils sont donc les précurseurs de tous les hydrocarbures présents dans le milieu interstellaire ; il est par conséquent nécessaire de les étudier en détail. Ces hydrocarbures CHy(+) sont soumis à divers processus physiques dans le milieu interstellaire notamment la collision avec un électron, l'absorption d'un photon ultraviolet ou d'un rayon cosmique. Ils vont être excités par ces processus et gagner un excès d'énergie qu'ils vont libérer par fragmentation, ce qui a pour conséquence de redistribuer les espèces. Des simulations précises dans la chimie du milieu interstellaire nécessitent donc une connaissance précise des taux de réaction et des rapports de branchement de fragmentation. Afin de documenter tous ces rapports de branchement, peu importe le processus physique ou chimique mis en jeu, nous avons construit expérimentalement des « breakdown curves » semi-empiriques qui sont les rapports de branchement des voies de fragmentation en fonction de l'énergie interne déposée lors du processus.L'expérience a été réalisée en utilisant le multi détecteur silicium AGAT et l'accélérateur ANDROMEDE. Les molécules CHy(+) produites à haute vitesse (3 u.a) collisionnent avec des atomes d’Hélium au repos dans le référentiel du laboratoire. Le dispositif expérimental permet de détecter tous les fragments, même les neutres, et de résoudre toutes les voies de fragmentation. Nous avons mesuré les rapports de branchement de fragmentation des CHyq+ (y=2-4, q=0-3) et les distributions d'énergie cinétique des fragments neutres.A partir des rapports de branchement, des distributions d'énergie cinétique et des énergies de dissociation théorique, nous avons construit les breakdown curves qui se sont révélés en bon accord avec des rapports de branchement expérimentaux déjà existant dans la littérature pour la photodissociation, la recombinaison dissociative et les collisions électroniques. Enfin, un modèle a été développé pour prédire les rapports de branchement de réactions chimiques ainsi que leur évolution avec la température. / In the interstellar medium, among the 200 molecules observed, the hydrocarbons are in abundance. The formation of hydrocarbons CHy(+) is done between a C+ and a hydrocarbon atom or molecule. Thereafter, these hydrocarbons are reacting between them to form bigger hydrocarbons. Therefore, they are the precursor of all the hydrocarbons present in the interstellar medium, so it is necessary to study them in details. These hydrocarbons CHy(+) are under a lot of different physical processes in the interstellar medium including the collision with an electron, the absorption of an ultra violet photon or a cosmic ray. They will be excited by these processes and gain excess energy they will liberate by fragmentation which leads to a redistribution of species. Therefore, a precise knowledge of the rate of reaction and of the branching ratios of the fragmentation is needed to do specific simulations in the chemistry of the interstellar medium. In order to document all these branching ratios, no matter the physical or chemical process at stake, we experimentally built semi-empirical breakdown curves which are the branching ratios of the paths of fragmentation as a function of the internal energy of the molecule.The experiment was done using the AGAT silicon multi-detector and the ANDROMEDE accelerator. CHy(+) molecules produced at high velocity (3 u.a.) are collided with He atom at rest in the lab. Thanks to the experimental developments, all fragments, neutral or charged, are separately identified, allowing to resolve all fragmentation channels. Therefore, we have been able to measure fragmentation branching ratios for CHyq+ (y=2-4, q=0-3) and the kinetic energy distributions of the neutral fragments.From the branching ratios, the kinetic energy distributions and the theoretical dissociation energies we built BDCs that revealed to be in accordance with the experimental branching ratios which already exists in the literature concerning the photo dissociation, the dissociative recombination and the electronic collisions. Finally, a model has been developed to predict the chemical reactions of the branching ratios as well as to predict their evolution with the temperature.

京都大学 / 0048 / 新制・課程博士 / 博士(理学) / 甲第19497号 / 理博第4157号 / 新制||理||1597(附属図書館) / 32533 / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)教授 鶴 剛, 教授 谷森 達, 准教授 成木 恵 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM

京都大学 / 新制・課程博士 / 博士(理学) / 甲第24405号 / 理博第4904号 / 新制||理||1700(附属図書館) / 京都大学大学院理学研究科物理学・宇宙物理学専攻 / (主査)教授 鶴 剛, 教授 井岡 邦仁, 教授 永江 知文 / 学位規則第4条第1項該当 / Doctor of Science / Kyoto University / DFAM

For a set of merging galaxies in the local Universe, we use archival Chandra X-ray data along with published 2.6 mm CO and 21 cm HI fluxes to determine the hot, cold, and warm interstellar gas masses, respectively. We determine how the relative amount of the different gas phases vary with merger stage, star formation rate, star formation efficiency, and stellar mass. We use these results to test models of stellar feedback during merger-triggered starbursts.

This thesis approaches the task of designing a control system for the Parallel Actuator Mount developed by Dr. John Ridgely and Mr. Garrett Gudgel. It aims to create a base framework that directly controls the telescope and can be expanded to accept external command. It incorporates lower priced components and develops more easily approachable software with great functionality. An open-loop method for velocity control is established. Developing repeatable tests is a major focus. Testing finds the control methods developed result in velocity error of less than 5% and position error of less than 1.5% despite several mechanical issues and inaccuracies. Design guidelines are established that allow for the easy implementation of a Parallel Actuator Mount on other systems. This paper proves that the Parallel Actuator Mount is a potentially viable system for aiming a telescope when an astronomer does not require full sky coverage. The tests showed too much error to fully recommend the system as built and tested, but there are paths to increase accuracy of the system without greatly increasing the complexity or cost. The inclusion of a method of feedback, including a plate solver and an inertial measurement unit, would greatly improve the system. It may also be of use to modify the software to include a variable time step for the velocity control.

Beta Cephei-type variables are early B-type stars that are characterized by oscillations observable in their optical light curves. At least one Beta Cep-variable also shows periodic variability in X-rays. Here we study the X-ray light curves in a sample of beta Cep-variables to investigate how common X-ray pulsations are for this type of stars. We searched the Chandra and XMM-Newton X-ray archives and selected stars that were observed by these telescopes for at least three optical pulsational periods. We retrieved and analyzed the X-ray data for kappa Sco, beta Cru, and alpha Vir. The X-ray light curves of these objects were studied to test for their variability and periodicity. While there is a weak indication for X-ray variability in beta Cru, we find no statistically significant evidence of X-ray pulsations in any of our sample stars. This might be due either to the insufficient data quality or to the physical lack of modulations. New, more sensitive observations should settle this question.

The O9IV star HD 57682, discovered to be magnetic within the context of the Magnetism in Massive Stars (MiMeS) survey in 2009, is one of only eight convincingly detected magnetic O-type stars. Among this select group, it stands out due to its sharp-lined photospheric spectrum. Since its discovery, the MiMeS Collaboration has continued to obtain spectroscopic and magnetic observations in order to refine our knowledge of its magnetic field strength and geometry, rotational period and spectral properties and variability. In this paper we report new Echelle SpectroPolarimetric Device for the Observation of Stars (ESPaDOnS) spectropolarimetric observations of HD 57682, which are combined with previously published ESPaDOnS data and archival Hα spectroscopy. This data set is used to determine the rotational period (63.5708 ± 0.0057 d), refine the longitudinal magnetic field variation and magnetic geometry (dipole surface field strength of 880 ± 50 G and magnetic obliquity of 79° ± 4° as measured from the magnetic longitudinal field variations, assuming an inclination of 60°) and examine the phase variation of various lines. In particular, we demonstrate that the Hα equivalent width undergoes a double-wave variation during a single rotation of the star, consistent with the derived magnetic geometry. We group the variable lines into two classes: those that, like Hα, exhibit non-sinusoidal variability, often with multiple maxima during the rotation cycle, and those that vary essentially sinusoidally. Based on our modelling of the Hα emission, we show that the variability is consistent with emission being generated from an optically thick, flattened distribution of magnetically confined plasma that is roughly distributed about the magnetic equator. Finally, we discuss our findings in the magnetospheric framework proposed in our earlier study.

We present time-resolved and phase-resolved variability studies of an extensive X-ray high-resolution spectral data set of the δ Ori Aa binary system. The four observations, obtained with Chandra ACIS HETGS, have a total exposure time of ≈ 479 ks and provide nearly complete binary phase coverage. Variability of the total X-ray flux in the range of 5–25 Å is confirmed, with a maximum amplitude of about ±15% within a single ≈ 125 ks observation. Periods of 4.76 and 2.04 days are found in the total X-ray flux, as well as an apparent overall increase in the flux level throughout the nine-day observational campaign. Using 40 ks contiguous spectra derived from the original observations, we investigate the variability of emission line parameters and ratios. Several emission lines are shown to be variable, including S xv, Si xiii, and Ne ix. For the first time, variations of the X-ray emission line widths as a function of the binary phase are found in a binary system, with the smallest widths at ϕ = 0.0 when the secondary δ Ori Aa2 is at the inferior conjunction. Using 3D hydrodynamic modeling of the interacting winds, we relate the emission line width variability to the presence of a wind cavity created by a wind–wind collision, which is effectively void of embedded wind shocks and is carved out of the X-ray-producing primary wind, thus producing phase-locked X-ray variability. Based on data from the Chandra X-ray Observatory and the MOST satellite, a Canadian Space Agency mission, jointly operated by Dynacon Inc., the University of Toronto Institute of Aerospace Studies, and the University of British Columbia, with the assistance of the University of Vienna.