The EVE Doppler Sensitivity and Flare Observations

The Extreme-ultraviolet Variability Experiment (EVE; see Woods et al., 2009) obtains continuous EUV spectra of the Sun viewed as a star. Its primary objective is the characterization of solar spectral irradiance, but its sensitivity and stability make it extremely interesting for observations of variability on time scales down to the limit imposed by its basic 10 s sample interval. In this paper we characterize the Doppler sensitivity of the EVE data. We find that the 30.4 nm line of He ii has a random Doppler error below 0.001 nm (1 pm, better than 10 km s⁻¹ as a redshift), with ample stability to detect the orbital motion of its satellite, the Solar Dynamics Observatory (SDO). Solar flares also displace the spectrum, both because of Doppler shifts and because of EVE’s optical layout, which (as with a slitless spectrograph) confuses position and wavelength. As a flare develops, the centroid of the line displays variations that reflect Doppler shifts and therefore flare dynamics. For the impulsive phase of the flare SOL2010-06-12, we find the line centroid to have a redshift of 16.8 ± 5.9 km s⁻¹ relative to that of the flare gradual phase (statistical errors only). We find also that high-temperature lines, such as Fe xxiv 19.2 nm, have well-determined Doppler components for major flares, with decreasing apparent blueshifts as expected from chromospheric evaporation flows.     

Use of a sensitive analytical method and the silt-clay (< 53 μm) fraction of stream sediments in exploration for gold in northern Thailand

Heavy mineral concentrates (SG 3.3) from the Huai Hin Laep, a tributary of the Huai Kho Lo River in northern Thailand, contain strongly anomalous concentrations of gold. In contrast, the gold content of the associated < 149 μm and <53 μm fractions of the sediment is generally less than the 5 ppb detection limit obtained by a conventional fire assay-atomic absorption spectrometry method. To test for the presence of a gold anomaly at concentrations < 5 ppb, we have used an aqua-regia digestion followed by an Amberlite XAD-8 column preconcentration technique that, when used with a spectrometer that enables full display of the analytical spectrum to optimize baseline analysis, gives a detection limit of 0.1 ppb Au.Gold content of the < 53 μm sediment fraction ranges from 1.0 to 3.1 ppb compared to concentrations that typically range from 1000 to more than 100,000 ppb in the heavy mineral concentrates. However, despite gold concentrations in the sediment being several orders of magnitude lower than those in the heavy mineral concentrates, the downstream dispersion patterns are similar, with gold concentrations increasing at high energy sites and downstream away from the assumed source. These results identify the presence of a greatly diluted gold anomaly in the < 53 μm fraction of the sediments and suggest that transport and deposition of this fine grained gold is controlled by the same sedimentological factors that control the behavior of gold in the sand-size range, between 53 μm and 425 μm. Most important from an exploration standpoint, is that by using a sufficiently sensitive analytical method, meaningful gold dispersion patterns can be recognized at concentrations below 5 ppb.     

AsteroFLAG: First results from hare‐and‐hounds Exercise #1

We report on initial results from the first phase of Exercise #1 of the asteroFLAG hare and hounds. The asteroFLAG group is helping to prepare for the asteroseismology component of NASA's Kepler mission, and the first phase of Exercise #1 is concerned with testing extraction of estimates of the large and small frequency spacings of the low‐degree p modes from Kepler‐like artificial data. These seismic frequency spacings will provide key input for complementing the exoplanet search data. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)