Letter from A.W. Musgrove & John B. Peat to James B. Finley

Rev. Musgrove writes to Finley affirming the appropriateness of his continued appointment in Dayton, though he is sorry not to be serving in Finley\u27s district. [Musgrove is a Local Preacher serving under Rev. William Herr. He and Herr have been organizing the Finley Chapel]. Musgrove declares his staunch loyalty to the Methodist Episcopal Church, in spite of offers from other denominations. John B. Peat is staying overnight with Musgrove and writes his own letter to Uncle Finley on the same sheet of stationery. [Peat is married to Finley\u27s niece, Lavina Finley]. Peat is pleased with the recent appointment of Rev. David Reed to his home congregation -- the Asbury MEC in Cincinnati. He reports that members of the congregation are beginning to be troubled by True Wesleyans. [Wesleyan Methodist Church, breakaway denomination founded in 1841 over the issues of slavery and church governance]. Abstract Number - 798https://digitalcommons.owu.edu/finley-letters/2302/thumbnail.jp

Mg II h&k fine structure prominence modelling and the consequences for observations

Aims. Using 2D Mg II h[amp]k solar prominence modelling, our aim is to understand the formation of complex line profiles and how these are seen by the Interface Region Imaging Spectrograph (IRIS). Additionally, we see how the properties of these simulated observations are interpreted through the use of traditional 1D prominence modelling. Methods. We used a cylindrical non-local thermodynamic equilibrium (NLTE) 2D complete redistribution (CRD) code to generate a set of cylindrical prominence strands, which we stacked behind each other to produce complex line profiles. Then, with the use of the point spread functions (PSFs) of IRIS, we were able to predict how IRIS would observe these line profiles. We then used the 1D NLTE code PROM in combination with the Cross Root Mean Square method (xRMS) to find the properties recovered by traditional 1D prominence modelling. Results. Velocities of magnitude lower than 10 km s−1 are sufficient to produce asymmetries in the Mg II h[amp]k lines. However, convolution of these with the PSFs of IRIS obscures this detail and returns standard looking single peaks. By increasing the velocities by a factor of three, we recover asymmetric profiles even after this convolution. The properties recovered by xRMS appear adequate at first, but the line profiles chosen to fit these profiles do not satisfactorily represent the line profiles. This is likely due to the large line width of the simulated profiles. Conclusions. Asymmetries can be introduced by multithread models with independent Doppler velocities. The large line width created by these models makes it difficult for traditional 1D forward modelling to find good matches. This may also demonstrate degeneracies in the solution recovered by single-species 1D modelling

The European Solar Telescope

The European Solar Telescope (EST) is a project aimed at studying the magnetic connectivity of the solar atmosphere, from the deep photosphere to the upper chromosphere. Its design combines the knowledge and expertise gathered by the European solar physics community during the construction and operation of state-of-the-art solar telescopes operating in visible and near-infrared wavelengths: the Swedish 1m Solar Telescope, the German Vacuum Tower Telescope and GREGOR, the French Télescope Héliographique pour l'Étude du Magnétisme et des Instabilités Solaires, and the Dutch Open Telescope. With its 4.2 m primary mirror and an open configuration, EST will become the most powerful European ground-based facility to study the Sun in the coming decades in the visible and near-infrared bands. EST uses the most innovative technological advances: the first adaptive secondary mirror ever used in a solar telescope, a complex multi-conjugate adaptive optics with deformable mirrors that form part of the optical design in a natural way, a polarimetrically compensated telescope design that eliminates the complex temporal variation and wavelength dependence of the telescope Mueller matrix, and an instrument suite containing several (etalon-based) tunable imaging spectropolarimeters and several integral field unit spectropolarimeters. This publication summarises some fundamental science questions that can be addressed with the telescope, together with a complete description of its major subsystems