An investigation into the stage history of Shakespeare's Tempest, 1667-1838 : a thesis presented in partial fulfilment of the requirements for the degree of Master of Arts in English at Massey University

After the theatres were re-opened in England at the Restoration, there were many adaptions made of Shakespeare's plays, and this was a common occurrence throughout the eighteenth century, lasting to Victorian times. It was only in the middle of the nineteenth century that Shakespeare began to be appreciated in the original form. The Tempest was one play that suffered many changes. Sir William Davenant and John Dryden collaborated in the first alteration of 1667, and their version is noteworthy because their changes were to a great extent retained by subsequent adapters. Pandering to a neo-classical desire for artistic symmetry, Davenant, the major contributor, and Dryden paired several of the major characters. To complement the lovers (Miranda and Ferdinand), they added Dorinda (Miranda's younger sister) and Hoppolito, who had never seen a woman, to be her mate. Caliban was given a sister, Sycorax, who has eyes for Trincalo (sic), and for Ariel, a female spirit called Milcha was created. Other changes in the dramatis personae are minor. The Restoration Tempest is full of farcical situations which stem from the lovers' naivity and the grotesque antics of the low comedy characters. The masque of Juno, protectress of marriage, in Shakespeare's Act IV has been cut, and altogether the effect of the original vanishes, the new play being much coarser. In 1674, an operatic version of the Restoration Tempest was published, probably written by Thomas Shadwell. This was basically Dryden and Davenant's play, though many songs were added. An elaborate masque of Neptune and Amphitrite was added towards the end, though it is hard to associate these characters with the ending of the play. Throughout the play there was much opportunity for spectacle and the use of mechanical contrivances. From 1747, when David Garrick became the manager of the Drury Lane Theatre, many of Shakespeare's plays were given a new look. Shadwell's operatic Tempest had been a long-running success, and in 1756 Garrick turned it into a three-act opera. This incorporated thirty-two songs, only three of which were Shakespeare's, and little regard was paid to the original text. It was a failure and Garrick repudiated authorship of it. In 1757 he reverted to a version that was much closer to Shakespeare's than any other before it. Among the 400 or more lines that Garrick omitted, however, were several intensely poetic passages. John Philip Kemble's Tempest of 1789, which used just the bare outline of the original plot, was merely a vehicle for the presentation of a number of songs, and was poorly received by critics who had begun to clamour for real Shakespeare, not a hybrid version of him. Kemble's next attempt to produce the play was in 1806, when he tried to combine the original and the Restoration versions. The last appearance of the Dryden-Davenant Tempest was in 1821 when Frederic Reynolds produced it, but it was greated with acrid criticism. William Charles Macready restored Shakespeare's original to the stage in 1838; and even though his interpretation catered for the visual impact more than for the poetry, his version was the first serious attempt for over century and a half to present the unadulterated Tempest to English theatregoers. Apart from detailing and commenting on the above changes, I have given several reasons for them, namely the adapters' endeavours to cater for contemporary taste and opinions, the neo-classical desire for symmetry, eighteenth century pragmatism, and the popularity of opera and of spectacle

Enhancing student learning with case-based learning objects in a problem-based learning context: the views of social work students in Scotland and Canada

This paper summarizes the results of an evaluation of students' perspectives comparing learning from a multimedia case-based learning object with learning from text-based case studies. A secondary goal of the study was to test the reusability of the learning object in different instructional contexts. The learning object was deployed in the context of a problem-based learning approach to teaching social work students in three different courses in two different countries: Scotland (N=39) and Canada (N=57). Students completed a structured survey form including a series of statements using a five point Likert scale to quantify their views of the different case types (text-based and multimedia). Results indicate strong support for the use of multimedia case scenarios in social work education. Students felt their learning was enhanced using multimedia case studies compared to text-based case studies. A number of benefits, disadvantages and recommendations were identified that will help guide the future development, (re)use, and exchange of digitized learning resources in social work education

Response of Lithographic Mask Structures to Repetitively Pulsed X-rays: Dynamic Response

This paper addresses the issue of the dynamic response of thin lithographic mask structures to thermally induced stress fields. In particular, the impact of repetitively pulsed x‐ray sources are examined: the short duration (1–100 nsec) pulses induce large step changes in mask temperatures, which can, in turn, induce a dynamic response. The impact of conductive cooling of the mask is to reduce the repetitively pulsed problem to a series of isolated nearly identical thermal impulses of duration approximately equal to the cooling time. The importance of self‐weight and prestress is examined, and an analysis of the nonlinear dynamic response to thermal impulses is described

Fe K\alpha emission from photoionized slabs: the impact of the iron abundance

Iron K\alpha emission from photoionized and optically thick material is observed in a variety of astrophysical environments including X-ray binaries, active galactic nuclei, and possibly gamma-ray bursts. This paper presents calculations showing how the equivalent width (EW) of the Fe K line depends on the iron abundance of the illuminated gas and its ionization state -- two variables subject to significant cosmic scatter. Reflection spectra from a constant density slab which is illuminated with a power-law spectrum with photon-index \Gamma are computed using the code of Ross & Fabian. When the Fe K EW is measured from the reflection spectra alone, we find that it can reach values greater than 6 keV if the Fe abundance is about 10 times solar and the illuminated gas is neutral. EWs of about 1 keV are obtained when the gas is ionized. In contrast, when the EW is measured from the incident+reflected spectrum, the largest EWs are ~800 keV and are found when the gas is ionized. When \Gamma is increased, the Fe K line generally weakens, but significant emission can persist to larger ionization parameters. The iron abundance has its greatest impact on the EW when it is less than 5 times solar. When the abundance is further increased, the line strengthens only marginally. Therefore, we conclude that Fe K lines with EWs much greater than 800 eV are unlikely to be produced by gas with a supersolar Fe abundance. These results should be useful in interpreting Fe K emission whenever it arises from optically thick fluorescence.Comment: 5 pages, 5 figures, accepted by MNRAS Letter

Lifting the Veil on Obscured Accretion: Active Galactic Nuclei Number Counts and Survey Strategies for Imaging Hard X-Ray Missions

Finding and characterizing the population of active galactic nuclei (AGNs) that produces the X-ray background (XRB) is necessary to connect the history of accretion to observations of galaxy evolution at longer wavelengths. The year 2012 will see the deployment of the first hard X-ray imaging telescope which, through deep extragalactic surveys, will be able to measure the AGN population at the energies where the XRB peaks (~20-30 keV). Here, we present predictions of AGN number counts in three hard X-ray bandpasses: 6-10 keV, 10-30 keV, and 30-60 keV. Separate predictions are presented for the number counts of Compton thick AGNs, the most heavily obscured active galaxies. The number counts are calculated for five different models of the XRB that differ in the assumed hard X-ray luminosity function, the evolution of the Compton thick AGNs, and the underlying AGN spectral model. The majority of the hard X-ray number counts will be Compton thin AGNs, but there is a greater than tenfold increase in the Compton thick number counts from the 6-10 keV to the 10-30 keV band. The Compton thick population shows enough variation that a hard X-ray number counts measurement will constrain the models. The computed number counts are used to consider various survey strategies for the NuSTAR mission, assuming a total exposure time of 6.2 Ms. We find that multiple surveys will allow a measurement of Compton thick evolution. The predictions presented here should be useful for all future imaging hard X-ray missions

Constraining Radiatively Inefficient Accretion Flows with Polarization

The low-luminosity black hole Sgr A* provides a testbed for models of Radiatively Inefficient Accretion Flows (RIAFs). Recent sub-millimeter linear polarization measurements of Sgr A* have provided evidence that the electrons in the accretion flow are relativistic over a large range of radii. Here, we show that these high temperatures result in elliptical plasma normal modes. Thus, polarized millimeter and sub-millimeter radiation emitted within RIAFs will undergo generalized Faraday rotation, a cyclic conversion between linear and circular polarization. This effect will not depolarize the radiation even if the rotation measure is extremely high. Rather, the beam will take on the linear and circular polarization properties of the plasma normal modes. As a result, polarization measurements of Sgr A* in this frequency regime will constrain the temperature, density and magnetic profiles of RIAF models.Comment: 4 pages, 3 figures, accepted by ApJ Letter

The luminous X-ray hotspot in 4C 74.26: synchrotron or inverse-Compton emission?

We report the discovery of an X-ray counterpart to the southern radio hotspot of the largest-known radio quasar 4C 74.26 (whose redshift is z=0.104). Both XMM-Newton and Chandra images reveal the same significant (10arcsec, i.e. 19kpc) offset between the X-ray hotspot and the radio hotspot imaged with MERLIN. The peak of the X-ray emission may be due to synchrotron or inverse-Compton emission. If synchrotron emission, the hotspot represents the site of particle acceleration and the offset arises from either the jet exhibiting Scheuer's `dentist's drill' effect or a fast spine having less momentum than the sheath surrounding it, which creates the radio hotspot. If the emission arises from the inverse-Compton process, it must be inverse-Compton scattering of the CMB in a decelerating relativistic flow, implying that the jet is relativistic (Gamma >= 2) out to a distance of at least 800kpc. Our analysis, including optical data from the Liverpool Telescope, rules out a background AGN for the X-ray emission and confirms its nature as a hotspot, making it the most X-ray luminous hotspot yet detected.Comment: 9 pages, 9 figures, definitive version published by MNRA