41 research outputs found
The Fellowship of Reconciliation\u27s Propaganda and Theodora Wilson Wilson\u27s Literary Contribution 1914-1917
During World War I Theodora Wilson Wilson, who shortly before the war had returned to her ancestral Quaker faith, made a unique contribution to the Fellowship of Reconciliation\u27s (FOR) propaganda. Instead of the usual expository writings aimed at the well educated, she wrote simple stories directed at casual readers. They emphasised the kind of activity, \u27doing\u27, the FOR leadership had decided to curtail after an attempt at tramping in the Midlands in the summer of 1915 had resulted in a near riot. Her perspective reflected that of many Friends. Some very limited attention has been given to these stories, but their contexts have not been explored adequately. This essay attempts to correct this deficiency and provides insight into an important Quaker stream within the FOR
Reluctant Absolutist: Malcolm Sparkes\u27 Conscientious Objections to World War I
The existing secondary literature has treated the appearance of World War I conscientious objectors (COs) before the tribunals as rather straightforward and uncomplicated. As the case of Malcolm Sparkes indicates, the process was much less straightforward and much more complex. The arduous process also shows that the power of the local tribunals was enlarged and that of the Pelham Committee reduced, due to the wrong decision - as the government acknowledged - by the local tribunal at Slough. The decision resulted in Sparkes becoming a reluctant or alternativist absolutist, a nomenclature hitherto ignored in the literature. Sparkes\u27 case also suggests that at least some Quaker and other nonconformist COs should be viewed through the prism of the Fellowship of Reconciliation rather than through the prism of the No-Conscription Fellowship or the Friends Service Committee
The interstellar oxygen-K absorption edge as observed by XMM-Newton
High resolution X-ray spectra of the Reflection Grating Spectrometer (RGS) on
board the XMM satellite are used to resolve the oxygen K absorption edge. By
combining spectra of low and high extinction sources, the observed absorption
edge can be split in the true interstellar (ISM) extinction and the
instrumental absorption. The detailed ISM edge structure closely follows the
edge structure of neutral oxygen as derived by theoretical R-matrix
calculations. However, the position of the theoretical edge requires a
wavelength shift. In addition the detailed instrumental RGS absorption edge
structure is presented. All results are verified by comparing to a subset of
Chandra LETG-HRC observations.Comment: LaTeX2e A&A style, 10 pages, 12 postscript figures, accepted for
publication in Astronomy and Astrophysic
First Light Measurements with the XMM-Newton Reflection Grating Spectrometers: Evidence for an Inverse First Ionisation Potential Effect and Anomalous Ne A bundance in the Coronae of HR 1099
The RS CVn binary system HR 1099 was extensively observed by the XMM-Newton
observatory in February 2000 as its first-light target. A total of 570 ks of
exposure time was accumulated with the Reflection Grating Spectrometers (RGS).
The integrated X-ray spectrum between 5-35 Angstrom is of unprecedented quality
and shows numerous features attributed to transitions of the elements C, N, O,
Ne, Mg, Si, S, Fe, and Ni. We perform an in-depth study of the elemental
composition of the average corona of this system, and find that the elemental
abundances strongly depend on the first ionisation potential (FIP) of the
elements. But different from the solar coronal case, we find an inverse FIP
effect, i.e., the abundances (relative to oxygen) increase with increasing FIP.
Possible scenarios, e.g., selective enrichment due to Ne-rich flare-like
events, are discussed.Comment: 5 pages, 4 figures. Accepted by A&A Letters, XMM issu
X-ray emitting young stars in the Orion Nebula
The Orion Nebula Cluster and the molecular cloud in its vicinity have been
observed with the ACIS-I detector on board the Chandra X-ray Observatory with
23 hours exposure. We detect 1075 X-ray sources: 91% are spatially associated
with known stellar members of the cluster, and 7% are newly identified deeply
embedded cloud members. This provides the largest X-ray study of a pre-main
sequence stellar population. We examine here the X-ray properties of Orion
young stars as a function of mass. Results include: (a) the discovery of rapid
variability in the O9.5 31 M_o star \theta^2A Ori, and several early B stars,
inconsistent with the standard model of X-ray production in small wind shocks;
(b) support for the hypothesis that intermediate-mass mid-B through A type
stars do not themselves produce significant X-ray emission; (c) confirmation
that low-mass G- through M-type T Tauri stars exhibit powerful flaring but
typically at luminosities considerably below the `saturation' level; (d)
confirmation that the presence or absence of a circumstellar disk has no
discernable effect on X-ray emission; (e) evidence that T Tauri plasma
temperatures are often very high with T >= 100 MK, even when luminosities are
modest and flaring is not evident; and (f) detection of the largest sample of
pre-main sequence very low mass objects showing high flaring levels and a
decline in magnetic activity as they evolve into L- and T-type brown dwarfs.Comment: 82 pages, 16 figures, 6 tables. To appear in the Astrophysical
Journal. For a version with high quality images and electronic tables, see
ftp://ftp.astro.psu.edu/pub/edf/orion1
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Integrated X-ray testing of the electro-optical breadboard model for the XMM reflection grating spectrometer
X-ray calibration of the Electro-Optical Breadboard Model (EOBB) of the XXM Reflection Grating Spectrometer has been carried out at the Panter test facility in Germany. The EOBB prototype optics consisted of a four-shell grazing incidence mirror module followed by an array of eight reflection gratings. The dispersed x-rays were detected by an array of three CCDs. Line profile and efficiency measurements where made at several energies, orders, and geometric configurations for individual gratings and for the grating array as a whole. The x-ray measurements verified that the grating mounting method would meet the stringent tolerances necessary for the flight instrument. Post EOBB metrology of the individual gratings and their mountings confirmed the precision of the grating boxes fabrication. Examination of the individual grating surface`s at micron resolution revealed the cause of anomalously wide line profiles to be scattering due to the crazing of the replica`s surface
Interstellar X-Ray Absorption Spectroscopy of Oxygen, Neon, and Iron with the Chandra LETGS Spectrum of X0614+091
We find resolved interstellar O K, Ne K, and Fe L absorption spectra in the Chandra X-Ray Observatory Low-Energy Transmission Grating Spectrometer (LETGS) spectrum of the low-mass X-ray binary X0614+091. We measure the column densities in O and Ne and find direct spectroscopic constraints on the chemical state of the interstellar O. These measurements probably probe a low-density line of sight through the Galaxy, and we discuss the results in the context of our knowledge of the properties of interstellar matter in regions between the spiral arms
Chandra Orion Ultradeep Project: Observations and Source Lists
We present a description of the data reduction methods and the derived
catalog of more than 1600 X-ray point sources from the exceptionally deep
January 2003 Chandra X-ray Observatory observation of the Orion Nebula Cluster
and embedded populations around OMC-1. The observation was obtained with
Chandra's Advanced CCD Imaging Spectrometer (ACIS) and has been nicknamed the
Chandra Orion Ultradeep Project (COUP). With an 838 ks exposure made over a
continuous period of 13.2 days, the COUP observation provides the most uniform
and comprehensive dataset on the X-ray emission of normal stars ever obtained
in the history of X-ray astronomy.Comment: 52 pages, 11 figures, 12 tables. Accepted for publication in ApJS,
special issue dedicated to Chandra Orion Ultradeep Project. A version with
high quality figures can be found at
http://www.astro.psu.edu/users/gkosta/COUP_Methodology.pd