Dissertations / Theses on the topic 'Variable magnetic field'

La thèse de doctorat comporte trois parties rédigées en anglais. Les deux premières parties correspondent principalement à l'étude de l'énergie de l'état fondamental. La dernière partie est consacrée à l'analyse de l'effet de pinning dans la supraconductivité.Dans une première partie de cette thèse, nous considérons la fonctionnelle de Ginzburg -Landau avec un champ magnétique variable appliqué dans un domaine borné et régulier de dimension 2. Nous déterminons le comportement asymptotique du paramètre d'ordre dans le régime o\`u le paramètre de Ginzburg-Landau et le champ magnétique sont grands et de même ordre. Comme conséquence, nous montrons que le paramètre d'ordre est localisé asymptotiquement dans la région où le profil du champ magnétique appliqué est petit.Dans une autre partie, nous considérons la fonctionnelle de Ginzburg -Landau avec un champ magnétique variable appliqué dans un domaine borné et régulier de dimension 2. Le profil du champ magnétique appliqué varie régulièrement et peut s'annuler exactement à l'ordre 1 le long d'une courbe. En supposant que la l'intensité du champ magnétique appliqué varie entre deux échelles caractéristiques, et que le paramètre de Ginzburg- Landau tend vers l'infini, nous déterminons une formule asymptotique précise pour minimiser l'énergie et montrer que les minimiseurs de l'énergie ont des vortex. Nous mettons en évidence que la présence d'un champ magnétique variable implique que la distribution de la vorticité dans l'échantillon n'est pas uniforme.Dans la dernière partie, nous étudions l'énergie de Ginzburg-Landau d'un supraconducteur avec un champ magnétique variable et un terme de pinning dans un domaine borné et régulier de dimension 2. En supposant que le paramètre de Ginzburg-Landau et l'intensité du champ magnétique sont grands et de même ordre, nous déterminons une formule asymptotique précise pour l'énergie. De plus, nous discutons l'existence des solutions non-triviales et déterminons le comportement asymptotique du troisième champ critique de la supraconductivité
The PHD thesis has three parts, the first and the second part correpond mainly to study the groundstate energy, the last one being devoted to the analysis of the pinning effect in superconductivity.In a first part of this thesis, we consider the Ginzburg-Landau functional with a variable applied magnetic field in a bounded and smooth two-dimensional domain. We determine an accurate asymptotic formula for the minimizing energy when the Ginzburg-Landau parameter and the magnetic field are large and of the same order. As a consequence, it is shown how bulk superconductivity decreases in average as the applied magnetic field increases.In another part, we consider the Ginzburg-Landau functional with a variable applied magnetic field in a bounded and smooth two-dimensional domain. The profile of the applied magnetic field varies smoothly and is allowed to vanish non-degenerately along a curve. Assuming that the strength of the applied magnetic field varies between two characteristic scales, and that the Ginzburg-Landau parameter tends to , we determine an accurate asymptotic formula for the minimizing energy and show that the energy minimizers have vortices. The new aspect in the presence of variable magnetic field is that the distribution of vortices in the sample is not uniform.In the final part, we study the Ginzburg-Landau energy of a superconductor with a variable magnetic field and a pinning term in a bounded and smooth two-dimensional domain . Supposing that the Ginzburg-Landau parameter and the intensity of magnetic field are large and of the same order, we determine an accurate asymptotic formula for the minimizing energy. Also, we discuss the existence of non-trivial solutions and prove an asymptotics of the third critical field

In this paper we investigate the multiwavelengths properties of the magnetic early B-type star HR7355. We present its radio light curves at several frequencies, taken with the Jansky Very Large Array, and X-ray spectra, taken with the XMM X-ray telescope. Modeling of the radio light curves for the Stokes I and V provides a quantitative analysis of the HR7355 magnetosphere. A comparison between HR7355 and a similar analysis for the Ap star CUVir, allows us to study how the different physical parameters of the two stars affect the structure of the respective magnetospheres where the non-thermal electrons originate. Our model includes a cold thermal plasma component that accumulates at high magnetic latitudes that influences the radio regime, but does not give rise to X-ray emission. Instead, the thermal X-ray emission arises from shocks generated by wind stream collisions close to the magnetic equatorial plane. The analysis of the X-ray spectrum of HR7355 also suggests the presence of a non-thermal radiation. Comparison between the spectral index of the power-law X-ray energy distribution with the non-thermal electron energy distribution indicates that the non-thermal X-ray component could be the auroral signature of the non-thermal electrons that impact the stellar surface, the same non-thermal electrons that are responsible for the observed radio emission. On the basis of our analysis, we suggest a novel model that simultaneously explains the X-ray and the radio features of HR7355 and is likely relevant for magnetospheres of other magnetic early type stars.

To improve the speed measurement of construction equipment, different sensor technologies have been investigated. Many of these sensor technologies are very interesting but to keep the extent of the thesis only two was chosen for testing, magnetic absolute angle sensors using Hall and GMR technology, to investigate if those are a valid replacement for the current measurement system that is using a passive sensor. Tests show that these sensors are capable of speed measurement, but because of noisy angle estimates they need filtering for good speed computation. This filtering introduces a large time delay that is of significance for the quality of the estimate. A Kalman filter has been implemented in an attempt to lower the time delays but since only a very simple model has been used it does not give any improvements over ordinary low pass filtering. For these sensors the mounting tolerance is of great interest. For best performance the offset between the sensor and magnet centres need to be kept small for both sensors. This is due to a non-linearity effect this causes. The distance between the sensors and the magnet is not critical for linearity issues, but only for the quality of the signal, where it might drop out when the distance is too large. This is where the sensor using GMR technology stands out. Compared to the Hall technology sensor, the GMR sensor can handle distances that are more than 10 times larger. The conclusion is that these sensors can be a valid replacement of the current measurement system. They will introduce more functionality with the capability of detecting rotational direction and zero velocity. In an application with more than one sensor they can also be used for more purposes, like detecting slip in clutches etc. Depending on the application, the time delays may not be critical, else more work need to be done to improve the estimate, e.g. with a more advanced model for the Kalman filter.

 

This thesis describes new methods of evaluating the efficiency of three-phase induction machines using synthetic loading. Synthetic loading causes the induction machine to draw full-load current without the need to connect a mechanical load to the machine's drive shaft. The synthetic loading methods cause the machine to periodically accelerate and decelerate, producing an alternating motor-generator action. This action causes the machine, on average over each synthetic loading cycle, to operate at rated rms current, rated rms voltage and full-load speed, thereby producing rated copper losses, iron loss and friction and windage loss. The excitation voltages are supplied from a PWM inverter with a large capacity DC bus capable of supplying rated rms voltage. The synthetic loading methods of efficiency evaluation are verified in terms of the individual losses in the machine by using a new dynamic model that accounts for iron loss and all parameter variations. The losses are compared with the steady-state loss distribution determined using very accurate induction machine parameters. The parameters were identified using a run-up-to-speed test at rated voltage and the locked rotor and synchronous speed tests conducted with a variable voltage supply. The latter tests were used to synthesise the variations in stator leakage reactance, magnetising reactance and the equivalent iron loss resistance over the induction machine's speed range. The run-up-to-speed test was used to determine the rotor resistance and leakage reactance variations over the same speed range. The test method results showed for the first time that the rotor leakage reactance varied in the same manner as the stator leakage and magnetising reactances with respect to current. When all parameter variations are taken into account there is good agreement between theoretical and measured results for the synthetic loading methods. The synthetic loading methods are applied to three-phase induction machines with both single- and double-cage rotors to assess the effect of rotor parameter variations in the method. Various excitation waveforms for each method were used and the measured and modelled efficiencies compared to conventional efficiency test results. The results verify that it is possible to accurately evaluate the efficiency of three-phase induction machines using synthetic loading.

To investigate if magnetic fields are present in Wolf–Rayet stars, we selected a few stars in the Galaxy and one in the Large Magellanic Cloud (LMC). We acquired low-resolution spectropolarimetric observations with the European Southern Observatory FORS 2 (FOcal Reducer low dispersion Spectrograph) instrument during two different observing runs. During the first run in visitor mode, we observed the LMC Wolf–Rayet star BAT99 7 and the stars WR 6, WR 7, WR 18, and WR 23 in our Galaxy. The second run in service mode was focused on monitoring the star WR 6. Linear polarization was recorded immediately after the observations of circular polarization. During our visitor observing run, the magnetic field for the cyclically variable star WR 6 was measured at a significance level of 3.3σ (〈Bz〉 = 258 ± 78 G). Among the other targets, the highest value for the longitudinal magnetic field, 〈Bz〉 = 327 ± 141 G, was measured in the LMC star BAT99 7. Spectropolarimetric monitoring of the star WR 6 revealed a sinusoidal nature of the 〈Bz〉 variations with the known rotation period of 3.77 d, significantly adding to the confidence in the detection. The presence of the rotation-modulated magnetic variability is also indicated in our frequency periodogram. The reported field magnitude suffers from significant systematic uncertainties at the factor of 2 level, in addition to the quoted statistical uncertainties, owing to the theoretical approach used to characterize it. Linear polarization measurements showed no line effect in the stars, apart from WR 6. BAT99 7, WR 7, and WR 23 do not show variability of the linear polarization over two nights.

The evolution of protoplanetary disks is believed to be driven largely by angular momentum transport resulting from magnetized disk winds and turbulent viscosity. The ionization of the disk that is essential for these processes has been thought to be due to host star coronal X-rays but could also arise from energetic particles produced by coronal flares, or traveling shock waves, and advected by the stellar wind. We have performed test-particle numerical simulations of energetic protons propagating into a realistic T. Tauri stellar wind, including a superposed small-scale magnetostatic turbulence. The isotropic (Kolmogorov power spectrum) turbulent component is synthesized along the individual particle trajectories. We have investigated the energy range [0.1-10] GeV, consistent with expectations from Chandra X-ray observations of large flares on T. Tauri stars and recent indications by the Herschel Space Observatory of a significant contribution of energetic particles to the disk ionization of young stars. In contrast with a previous theoretical study finding a dominance of energetic particles over X-rays in the ionization throughout the disk, we find that the disk ionization is likely dominated by X-rays over much of its area, except within narrow regions where particles are channeled onto the disk by the strongly tangled and turbulent magnetic field. The radial thickness of such regions is 5 stellar radii close to the star and broadens with increasing radial distance. This likely continues out to large distances from the star (10 au or greater), where particles can be copiously advected and diffused by the turbulent wind.

Time-series spectropolarimetric observations of polar WX LMi and asynchronous polar BY Cam are presented. Magnetic field properties, radial velocities and optical polarization are investigated via consecutive observations with good phase sampling during a single orbital cycle. Both systems are found to have a decentred dipole magnetic field configuration. One of the poles of WX LMi has a field strength of 49 MG, while the other pole may have possible field strengths of 69, 104 or 207 MG, depending on the harmonic numbers of the cyclotron humps observed in the circularly polarized spectrum. For BY Cam, a field strength of 168 MG is found for one of the poles, while field strengths of 70, 160 or 212 MG are possible for the other pole.

A rather strong mean longitudinal magnetic field of the order of a few hundred gauss was detected a few years ago in the Of?p star CPD −28° 2561 using FORS2 (FOcal Reducer low dispersion Spectrograph 2) low-resolution spectropolarimetric observations. In this work, we present additional low-resolution spectropolarimetric observations obtained during several weeks in 2013 December using FORS 2 mounted at the 8-m Antu telescope of the Very Large Telescope (VLT). These observations cover a little less than half of the stellar rotation period of 73.41 d mentioned in the literature. The behaviour of the mean longitudinal magnetic field is consistent with the assumption of a single-wave variation during the stellar rotation cycle, indicating a dominant dipolar contribution to the magnetic field topology. The estimated polar strength of the surface dipole Bd is larger than 1.15 kG. Further, we compared the behaviour of the line profiles of various elements at different rotation phases associated with different magnetic field strengths. The strongest contribution of the emission component is observed at the phases when the magnetic field shows a negative or positive extremum. The comparison of the spectral behaviour of CPD −28° 2561 with that of another Of?p star, HD 148937 of similar spectral type, reveals remarkable differences in the degree of variability between both stars. Finally, we present new X-ray observations obtained with the Suzaku X-ray Observatory. We report that the star is X-ray bright with log LX/Lbol ≈ −5.7. The low-resolution X-ray spectra reveal the presence of a plasma heated up to 24 MK. We associate the 24 MK plasma in CPD −28° 2561 with the presence of a kG strong magnetic field capable to confine stellar wind.

Cette thèse se concentre sur la thématique de l'éjection électromagnétique appliquée dans le cadre de l'industrie du recyclage des métaux. L'objectif de celle-ci est la modélisation et la réalisation d'une architecture de conversion d'énergie permettant la réalisation de cette éjection. Le champ magnétique variable généré est utilisé afin de séparer d'un flux de déchets les matériaux métalliques non ferromagnétique tel que l'aluminium ou le cuivre par le biais d'une force de Laplace engendrée par la conjonction entre le champ magnétique crée et le champ magnétique induit par les courants de Foucault dans les matériaux conducteurs. L'architecture développée se compose de plusieurs éléments: un redresseur, un onduleur et un inducteur. La partie redresseur, à large plage de fonctionnement connectée sur le réseau d'alimentation triphasée permet d'obtenir une tension continu réglable et assure un prélèvement sinusoïdale de courant en phase avec la tension. La partie onduleur, permet de contrôler la puissance transmise, en adaptant l'amplitude et la fréquence du courant traversant la dernière partie du système que forme l'inducteur, responsable de la création du champ magnétique alternatif. Le choix du redresseur s'est porté sur la structure classique du redresseur abaisseur de tension de type Buck en raison de la faible impédance de l'inducteur utilisé. Bien que cette structure permette d'abaisser la tension triphasée, sa plage de fonctionnement peut être facilement augmentée sans l'ajout de composant passif. Le contrôle classique de ce redresseur ne se base que sur ses grandeurs de sorties ce qui peut engendrer des oscillations non contrôlées causées par la mise en résonance du filtre LC d'entrée excité par les harmoniques générés par les commutations des transistors. Nous avons proposé dans cette thèse une nouvelle méthode de contrôle qui traite à la fois de ses grandeurs d'entrée et de sortie et qui permet de contrôler les éventuelles oscillations du filtre LC d'entrée tout en bénéficiant d'une meilleure réponse dynamique lorsque le système est soumis à un échelon de charge. Cette méthode de contrôle se base sur les propriétés de platitude des systèmes différentielles, ainsi elle ne dépend pas du point de fonctionnement et garantit la stabilité large signal du système. Le choix de l'onduleur monophasé s'est porté sur une structure en pont complet permettant l'application de trois niveaux de tension et un large choix de contrôle de l'amplitude, de la forme et de la fréquence du courant traversant l'inducteur. Différents contrôle de ce convertisseur ont été étudiés et comparés. Ceux-ci permettent de faire varier la puissance injectée dans l'inducteur, ont un impact sur le contenu harmonique du courant le traversant et sur les contraintes des différents composants du système. Une modélisation de l'inducteur ainsi qu'une estimation de la valeur du champ magnétique nécessaire à l'éjection est effectuée. Les différentes méthodes proposées sont validées par des résultats de simulations numérique mais également par le biais de tests expérimentaux réalisés sur le système complet
This thesis focuses on the subject of electromagnetic ejection applied in the context of the metal recycling industry. The aim of this thesis is the modeling and the development of an architecture of energy conversion allowing the realization of this ejection. The generated variable magnetic field is used to separate non-ferromagnetic metallic materials such as aluminum or copper from a waste stream by means of a Laplace force generated by the conjunction between the magnetic field created and the magnetic field induced by the eddy currents in the conductive materials.The developed architecture is composed of several elements: a rectifier, an inverter and an inductor. The rectifier part with a wide operating range connected to the three-phase grid network allows to obtain an adjustable DC voltage and ensures a sinusoidal current in phase with the voltage. The inverter part allows to control the transferred power, by adjusting the amplitude and frequency of the current flowing through the last part of the system represented by the inductor, responsible for the generation of the variable magnetic field.The rectifier is based on the classical Buck rectifier structure because of the low impedance of the inductor used. Although this structure allows to lower the three-phase grid voltage, its operating range can be easily increased without the addition of passive components. The classical control of this rectifier is based only on its output variables which can lead to uncontrolled oscillations caused by the resonance of the lightly damped input LC filter excited by the harmonics generated by the switching of transistors. In this thesis, we proposed a new control method that deals with both its input and output variables and that allows both to control the oscillations of the input LC filter while obtaining a better dynamic response when the system is subjected to a load step. This control method is based on the flatness properties of differential systems, so it does not depend on the operating point and guarantees the large signal stability of the system.The single-phase inverter is based on a full bridge structure allowing the application of three voltage levels and a wide choice of control of the amplitude, shape and frequency of the current flowing through the inductor. Different controls of this converter have been studied and compared. These allow to vary the power injected in the inductor, have an impact on the harmonic content of the current flowing through it and on the constraints of the different components of the system.A modeling of the inductor as well as an estimation of the value of the magnetic field necessary for the ejection is carried out. The different methods proposed are verified by numerical simulations but also by experimental tests performed on the whole system

碩士
淡江大學
電機工程學系碩士班
94
With the progression of the technology advancement, there are more and more electric equipment produced in our living environment. In that, most of the equipment will result in a magnetic field. Although it is not sure that human is cursed with magnetic field in many researches, more of people believe that human will get hurt when staying in magnetic for a long time. The objective of this thesis is to design a magnetic field generator. This thesis, includes the effect of system optioning in high frequency magnetic field, and the theory regarding simulation. The simulation software is used to build the module and simulate the distribution of the generating magnetic field. This work designs a high frequency magnetic field generator. The frequency of the generator is 100KHz, and the field intensity is 50Gauss. The LC parallel resonant compensation is adopted in the power supply of the magnetic field generator to enhance exciting current and to reduce the secondary current of the high frequency generator. The dimension for the bio-exposure experimental space is 40mm(L) × 40mm(W) × 50mm(H) in the air gaps of the magnetic field generator. Finally, this study utilizes the FEMLAB software based on the finite element method to simulate the magnetic field of generator, and compare the effect between different designs.

In the present PhD work, three sophisticated models based on the "Engineering" modeling approach have been utilized to conveniently describe and thoroughly analyze details of Lightning events at the CN Tower. Both the CN Tower and the Lightning Channel are represented by a number of connected in series Transmission Line sections in order to account for the variations in the shape of the tower and for plasma processes that take place within the Lightning Channel. A sum of two Heidler functions is used to describe the "uncontaminated" Return Stroke current, which is injected at the attachment point between the CN Tower and the Lightning Channel. Reflections and refractions at all points of mismatched impedances are considered until their contribution becomes less than 1% of the originally injected current wave. In the proposed models, the problem with the current discontinuity at the Lightning Channel front, commonly taken care of by introducing a "turn-on" term when computing radiation fields, is uniquely treated by introducing reflected and transmitted components. For the first time, variable speed of propagation of the Return Stroke current front has been considered and its influence upon the predicted current distributions along the whole Lightning Channel path and upon the radiated distant fields analyzed. Furthermore, as another novelty, computation of the electromagnetic field is accomplished in Cartesian Coordinates. This fact permits to relax the requirement on the verticality of the Lightning Channel, normally imposed in Cylindrical Coordinates. Therefore, it becomes possible to study without difficulty the influence of a slanted Lightning Channel upon the surrounding electromagnetic field. Since the proposed sophisticated Five-Section Model has the capability to represent very closely the structure of the CN Tower and to emulate faithfully the shape of, as well as physical processes within the Lightning Channel, it is believed to have the potential of truthfully reproducing observed fields. The developed modeling approach can be easily adapted to study the anticipated radiated fields at tall structures even before construction.

This work is motivated by the Variable Specific Impulse Magnetoplasma Rocket (VASIMR) experiment. This device uses a helicon antenna to generate a plasma inside a dielectric tube, which is radially confined and directed towards the rocket nozzle by an axial magnetic field. An ion cyclotron heating antenna further heats the ions, and a magnetic nozzle accelerates the plasma along the confining magnetic field as it leaves the rocket, ultimately allowing it to detach from the magnetic field and produce thrust. The experimental research presented here provides insight into the physical mechanisms of power flow in a helicon system by providing an overall system power balance in the form of heat flux measurements, and exploring changes in the heat fluxes in different parts of the system in response to varying operational parameters. An infrared (IR) camera measures the total heat flux into the dielectric tube surface, and axially scanned bolometer and UV photodiode probes measure the radial power loss from particles and radiation. Results from IR camera measurements on three different helicon systems are presented: the VASIMR VX-50 experiment, the VASIMR VX-CR experiment, and the University of Texas at Austin (UT) helicon experiment. These results demonstrate the development of the IR camera diagnostic for use on helicon systems of varying scale and geometry, and show reasonable agreement as to the fraction of input power lost to the dielectric tube walls. On the UT experiment, the results presented account for essentially all of the input power, providing a full system power balance. The data from all three experiments indicate that radial transport of ions to the interior wall is the dominant mechanism of power loss, with UV radiation contributing a small percentage. Additional experiments on the UT helicon explore energy and particle transport to the wall due to capacitive coupling of ions near the antenna. These experiments show clear damage to the dielectric tube surface directly under the antenna, due to physical plasma etching of the surface by bombarding ions that are accelerated into the wall by local electric fields from the antenna.
text

en este trabajo de tesis se proponen nuevos conceptos y métodos para el diseño de electroimanes ffc, con lo cual se define el estado actual del arte en la materia. se consideran sistemas basados en bobinados múltiples controlados individualmente y sistemas de electroimanes con geometría variable (siendo ésta la principal innovación que se aporta, definiendo el concepto de electroimán activo). ambos conceptos fueron a su vez desarrollados para eliminar los complejos procesos de maquinado necesarios en los electroimanes actualmente en uso a nivel global, lográndose otras ventajas que serían expuestas oportunamente. se implementas un prototipo de sistema de geometría variable, el cual fue probado y verificado utilizando un aparato existente en el laboratorio.

Supergiant stars of spectral types B and A are characterized by variable and structured winds, as revealed by variability of optical and ultraviolet spectral lines. Non- radial pulsations and magnetically supported loops have been proposed as explanations for these phenomena. The latter hypothesis is tested using a time series of 65 high-resolution (λ/∆λ ∼ 65, 000) circular polarization (Stokes I and V ) spectra of the late B type supergiant Rigel (β Ori, B8 Iae), obtained with the instruments ESPaDOnS and Narval at the Canada-France-Hawaii Telescope and the Bernard Lyot Telescope, respectively. Examination of the unpolarized (Stokes I) spectra using standard spectral analysis tools confirms complex line profile variability during the 5 month period of observations; the high spectral resolution allows the identification of a weak, transient Hα feature similar in behaviour to a High Velocity Absorption event. Analysis of the Stokes V spectra using the cross-correlation technique Least Squares Deconvolution (LSD) yields no evidence of a magnetic field in either LSD Stokes V profiles or longitudinal field measurements, with longitudinal field 1σ error bars of ∼ 12 G for individual observations, and a mean field in the best observed period of 3 ± 2 G. Synthetic LSD profiles fit to the observations using a Monte Carlo approach yield an upper limit on the surface dipolar field strength of Bdip ≤ 50 G for most orientations of the rotational and magnetic axes, lowered to Bdip ≤ 35 G if the mean LSD profile from the most densely time-sampled epoch (with an LSD SNR of ∼80,000) is used. A simple two-spot geometry representing the footpoints of a magnetic loop emerging from the photosphere yields upper limits on the spot magnetic fields of 60–600 G, depending on the filling factor of the spots. Given existing measurements of the mass loss rate and the wind terminal velocity, these results cannot rule out a magnetically confined wind as, for Bdip ≤ 15 G, η∗ ≥ 1. However, the detailed pattern of line profile variability seems inconsistent with the periodic wind modulation characteristic of known magnetic early-type stars, suggesting that magnetic fields do not play a dominant role in Rigel’s variable winds.
Thesis (Master, Physics, Engineering Physics and Astronomy) -- Queen's University, 2012-04-29 02:10:41.308

This MSc report discusses the attributes of W Ursae Majoris (W UMa) stars and an investigation into the Minimum Entropy (ME) method, a digital technique applied to the determination of their periods of variability. A Python code programme was written to apply the ME method to photometric data collected on W UMa stars by the All Sky Automated Survey (ASAS). Starting with the orbital period of the binaries estimated by ASAS, this programme systematically searches around this period for the period which corresponds to the lowest value of entropy. Low entropy here means low scatter (or spread) of data across the phase-magnitude plane. The ME method divides the light curve plot area into a number of elements of the investigators choosing. When a particular orbital period is applied to this photometric data, the resulting distribution of this data in the light curve plane corresponds to a speci c number of data points in each element into which this plane has been divided. This data spread is measured and calculated in terms of entropy and the lowest value of entropy corresponds to the lowest spread of data across the light curve plane. This should correspond to the best light curve shape available from the data and therefore the most accurate orbital period available. Subsequent to the testing of this Python code on perfect sine waves, it was applied, and its results compared, to the 62 ASAS eclipsing binary stars which were investigated by Deb and Singh (2011). The method was then applied to selected stars from the ASAS data base.
School of Environmental Sciences
M. Sc. (Astronomy)