Extreme ultraviolet emission lines of Ca XV in solar and laboratory spectra

New R-matrix calculations of electron impact excitation rates in Ca XV are used to derive theoretical electron density diagnostic emission line intensity ratios involving 2s(2)2p(2)- 2s2p(3) transitions, specifically R-1 = I(208.70 Angstrom)/I(200.98 Angstrom), R-2 = I(181.91 Angstrom)/I(200.98 Angstrom), and R-3 = I(215.38 Angstrom)/I(200.98 Angstrom), for a range of electron temperatures (T-e = 10(6.4)-10(6.8) K) and densities (Ne = 10(9)-10(13) cm(-3)) appropriate to solar coronal plasmas. Electron densities deduced from the observed values of R-1, R-2, and R-3 for several solar flares, measured from spectra obtained with the Naval Research Laboratory's S082A spectrograph on board Skylab, are found to be consistent. In addition, the derived electron densities are in excellent agreement with those determined from line ratios in Ca XVI, which is formed at a similar electron temperature to Ca XV. These results provide some experimental verification for the accuracy of the line ratio calculations, and hence the atomic data on which they are based. A set of eight theoretical Ca XV line ratios involving 2s(2)2p(2)-2s2p(3) transitions in the wavelength range similar to140-216 Angstrom are also found to be in good agreement with those measured from spectra of the TEXT tokamak plasma, for which the electron temperature and density have been independently determined. This provides additional support for the accuracy of the theoretical line ratios and atomic data.

Accounts of debates in the House of Commons, March– April 1731, supplementary to the diary of the first earl of Egmont

John Perceval (1685–1748), 1st Viscount Perceval and (from 1733) 1st Earl of Egmont, was an assiduous recorder of his own life and times. His diaries, published by the Historical Manuscripts Commission from manuscripts in the British Library, are the best source for parliamentary debates at Westminster in the 1730s. For the years 1730-1733, when Perceval sat in the Commons (as an Irish peer) they are remarkably full. His practice seems to have been to prepare two versions (presumably on the basis of notes taken in the House), the first attributing speeches to individuals, and the second, entered up in the diary, which listed speakers and summarized all arguments on each side. His letterbooks for 1731 contain accounts of five debates that embody his first editing process, with speeches attributed to individuals. They were sent to an Irish correspondent, Marmaduke Coghill, and largely omitted from the diary because Perceval had already transcribed them elsewhere. They are new to historians and cast light on two main issues: the unsuccessful attempts by Perceval and the ‘Irish lobby’ to persuade the British parliament to settle the Irish woollen trade, a question bedevilling Anglo-Irish relations in this period; and an attempt by the opposition to stir up anger against perceived Spanish aggression against Gibraltar. One of the most interesting features is the insight afforded into the Commons performances of Sir Robert Walpole: his management of debates, his own style of speaking, and his sharp exchanges with opponents like William Pulteney.

INFLUENCE OF CORE POLARIZATION ON THE ELECTRON-AFFINITY OF CA

We have developed a method, based on the use of B-spline basis sets and model potentials, for determining properties of systems with two or three electrons outside a polarizable closed-shell core. It is applied to the calculation of the electron affinity of Ca and the resulting value of 17.7 meV is in excellent agreement with the most recent experiments. It is found that the dielectronic core-valence interaction reduces the electron affinity by 39.5 meV.

Electron excitation of Ca XVII

Electron-excitation collision strengths have been calculated for transitions between the ten lowest levels of Ca XVII (2sS, 2s2p P, 2s2p P, 2pP 2p D, 2pS ). At high impact energies, where all the channels are open, the calculation was carried out in the LS-coupling approximation by means of the R-matrix method. Transitions between the fine structure levels were then determined by application of a unitary transformation to the LS-coupled K-matrices. At low impact energies, where some of the channels may be closed, an extension of the R-matrix method was employed to take account of relativistic effects directly in the scattering equations. In general, results are in good agreement with recent distorted-wave calculations. Electron-excitation rates are given for a range of electron temperatures.

A Zoologist with a Taste for the Past: The Earl of Cranbrook’s Contribution to Zooarchaeological Research in Southeast Asia

The Earl of Cranbrook (V) (then Lord Medway) was fi rst introduced to archaeological research in 1958 when he participated in excavations at the Niah Caves, Sarawak Borneo. In that same year he published a paper entitled ‘Food bone in Niah Cave excavations (-1958)’ in the Sarawak Museum Journal. Unbeknownst to him at the time, his individual and intuitive research was on a par with, if not methodologically ahead of, burgeoning studies in the fi eld of zooarchaeology that were taking place at leading academic institutions in Europe and the United States. This paper recounts and lauds the signifi cant contributions the Earl of Cranbrook has made to the establishment and furtherance of a discipline over more than 50 years. 

Select Document: Sir George Radcliffe’s “Original of Government” (1639) and Absolutist Political Theory in Stuart Ireland

A seventeenth-century manuscript miscellany, which once belonged to Archbishop James Ussher of Armagh, contains a short treatise on the origins of government by Sir George Radcliffe. Radcliffe was legal assistant to Sir Thomas Wentworth, lord deputy of Ireland (from January 1640 earl of Strafford and lord lieutenant). The treatise insisted on the divine origin of all human political power and implied that the best form of government was absolute monarchy, in which the monarch was free of all human law and subject to divine restraint alone. It will be suggested below that the composition of this treatise can be dated to the summer of 1639. This introduction will offer an outline of Radcliffe’s education and political career, explain the genesis of his treatise on government, point out some pertinent aspects of its argument, and finally assess the document’s significance.

Carbachol triggers RyR-dependent Ca(2+) release via activation of IP(3) receptors in isolated rat gastric myocytes.

Possible interactions between different intracellular Ca(2+) release channels were studied in isolated rat gastric myocytes using agonist-evoked Ca(2+) signals. Spontaneous, local Ca(2+) transients were observed in fluo-4-loaded cells with linescan confocal imaging. These were blocked by ryanodine (100 microM) but not by the inositol 1,4,5-trisphosphate receptor (IP(3)R) blocker, 2-aminoethoxydiphenyl borate (100 microM), identifying them as Ca(2+) sparks. Caffeine (10 mM) and carbachol (10 microM) initiated Ca(2+) release at sites which co-localized with each other and with any Ca(2+) spark sites. In fura-2-loaded cells extracellular 2-aminoethoxydiphenyl borate and intracellular heparin (5 mg ml(-1)) both inhibited the global cytoplasmic [Ca(2+)] transient evoked by carbachol, confirming that it was IP(3)R-dependent. 2-Aminoethoxydiphenyl borate and heparin also increased the response to caffeine. This probably reflected an increased Ca(2+) store content since 2-aminoethoxydiphenyl borate more than doubled the amplitude of transients evoked by ionomycin. Ryanodine completely abolished carbachol and caffeine responses but only reduced ionomycin transients by 30 %, suggesting that blockade of carbachol transients by ryanodine was not simply due to store depletion. Double labelling of IP(3)Rs and RyRs demonstrated extensive overlap in their distribution. These results suggest that carbachol stimulates Ca(2+) release through co-operation between IP(3)Rs and RyRs, and implicate IP(3)Rs in the regulation of Ca(2+) store content.

Grazing under experimental hypercapnia and elevated temperature does not affect the radula of a chiton (Mollusca, Polyplacophora, Lepidopleurida)

Chitons (class Polyplacophora) are benthic grazing molluscs with an eight-part aragonitic shell armature. The radula, a serial tooth ribbon that extends internally more than half the length of the body, is mineralised on the active feeding teeth with iron magnetite apparently as an adaptation to constant grazing on rocky substrates. As the anterior feeding teeth are eroded they are shed and replaced with a new row. The efficient mineralisation and function of the radula could hypothetically be affected by changing oceans in two ways: changes in seawater chemistry (pH and pCO(2)) may impact the biomineralisation pathway, potentially leading to a weaker or altered density of the feeding teeth; rising temperatures could increase activity levels in these ectothermic animals, and higher feeding rates could increase wear on the feeding teeth beyond the animals' ability to synthesise, mineralise, and replace radular rows. We therefore examined the effects of pH and temperature on growth and integrity in the radula of the chiton Leptochiton asellus. Our experiment implemented three temperature (similar to 10, 15, 20 degrees C) and two pCO(2) treatments (similar to 400 mu atm, pH 8.0; similar to 2000 mu atm, pH 7.5) for six treatment groups. Animals (n = 50) were acclimated to the treatment conditions for a period of 4 weeks. This is sufficient time for growth of ca. 7-9 new tooth rows or 20% turnover of the mineralised portion. There was no significant difference in the number of new (non-mineralised) teeth or total tooth row count in any treatment. Examination of the radulae via SEM revealed no differences in microwear or breakage on the feeding cusps correlating to treatment groups. The shell valves also showed no signs of dissolution. As a lineage, chitons have survived repeated shifts in Earth's climate through geological time, and at least their radulae may be robust to future perturbations.

The large- and small-scale Ca IIK structure of the Milky Way from observations of Galactic and Magellanic sightlines

Aims. The large and small-scale (pc) structure of the Galactic interstellar medium can be investigated by utilising spectra of early-type stellar probes of known distances in the same region of the sky. This paper determines the variation in line strength of Ca ii at 3933.661 Å as a function of probe separation for a large sample of stars, including a number of sightlines in the Magellanic Clouds. 

Methods. FLAMES-GIRAFFE data taken with the Very Large Telescope towards early-type stars in 3 Galactic and 4 Magellanic open clusters in Ca ii are used to obtain the velocity, equivalent width, column density, and line width of interstellar Galactic calcium for a total of 657 stars, of which 443 are Magellanic Cloud sightlines. In each cluster there are between 43 and 111 stars observed. Additionally, FEROS and UVES Ca ii K and Na i D spectra of 21 Galactic and 154 Magellanic early-type stars are presented and combined with data from the literature to study the calcium column density - parallax relationship. 

Results. For the four Magellanic clusters studied with FLAMES, the strength of the Galactic interstellar Ca ii K equivalent width on transverse scales from ∼0.05-9 pc is found to vary by factors of ∼1.8-3.0, corresponding to column density variations of ∼0.3-0.5 dex in the optically-thin approximation. Using FLAMES, FEROS, and UVES archive spectra, the minimum and maximum reduced equivalent widths for Milky Way gas are found to lie in the range ∼35-125 mÅ and ∼30-160 mÅ for Ca ii K and Na i D, respectively. The range is consistent with a previously published simple model of the interstellar medium consisting of spherical cloudlets of filling factor ∼0.3, although other geometries are not ruled out. Finally, the derived functional form for parallax (π) and Ca ii column density (N_CaII) is found to be π(mas) = 1 / (2.39 × 10^-13 × N_CaII (cm^-2) + 0.11). Our derived parallax is ∼25 per cent lower than predicted by Megier et al. (2009, A&A, 507, 833) at a distance of ∼100 pc and ∼15 percent lower at a distance of ∼200 pc, reflecting inhomogeneity in the Ca ii distribution in the different sightlines studied.

CaII K interstellar observations towards early-type disc and halo stars

We present high-resolution (R = lambda/Deltalambda similar to 40 000) Ca II K interstellar observations (lambda(air) = 3933.66Angstrom) towards 88 mainly B-type stars, of which 74 are taken from the Edinburgh-Cape or Palomar-Green surveys, and 81 have > 25degrees. The majority of the data come from previously existing spectroscopy, although also included are 18 new observations of stars with echelle spectra taken with UVES on the Very Large Telescope UT2 (Kueyen). Some 49 of the sample stars have distance estimates above the Galactic plane (z) greater than or equal to 1 kpc, and are thus good probes of the halo interstellar medium. Of the 362 interstellar Ca K components that we detect, 75 (21 per cent) have absolute values of their LSR velocity values exceeding 40 km s(-1). In terms of the deviation velocity for the sightlines with distance estimates, 46/273 (17 per cent) of components have velocity values exceeding those predicted by standard Galactic rotation by more than 40 km s(-1). Combining this data set with previous observations, we find that the median value of the reduced equivalent width (REW) of stars with z greater than or equal to 1 kpc (EW x sin ) is similar to 115 mAngstrom (n = 80), similar to that observed in extragalactic sightlines by Bowen. Using data of all z distances, the REW at infinity is found to be similar to 130 mAngstrom, with the scaleheight (1) of the Ca II K column density distribution being;z 800 pc (n = 196) and reduced column density at infinity of log[N(Ca II K) cm(-2)] similar to 12.24. This implies that similar to30 per cent of Ca II K absorption occurs at distances exceeding similar to1 kpc. For nine sightlines, with distance exceeding 1 kpc and with a companion object within 5degrees, we find that all but two have values of Ca II reduced equivalent width the same to within similar to20 per cent, when the REW of the nearest object is extrapolated to the distance of the further of the pair, and assuming 1 = 800 pc. For 29 of our sightlines with z greater than or equal to 1 kpc and a H I detection from the Leiden-Dwingeloo survey (beamsize of 0.5degrees), we find log(N(Ca II K)IN(H I)) ranging from -7.4 to - 8.4. Values of the Ca II K abundance relative to neutral hydrogen (log[N(Ca II K) cm(-2)] - log[N(H I) cm(-2)]) are found to be more than similar to0.5 dex higher in stars with distances exceeding approximate to100 pc, when compared with the (log[N(Ca II K) cm(-2)] -log[N(H-tot) cm(-2)]) values found in nearby sightlines such as those in Wakker & Mathis (2000). Finally, stellar Ca II K equivalent widths of the sample are determined for 26 objects.