Stratigraphy of Wood-derived Sterols in Sediments Historically Contaminatedby Pulp and Paper Mill Effluents

Sterols and their metabolites are recognized as hormonally active compounds in many earlier studies. Therefore, identification and quantification of selected phytosterols related to developments in pulping and wastewater treatment of pulp and paper industry were studied from sediment cores of two Finnish lakes. Indicating the period of maximal emissions, the highest total concentration of sterols, 1970 μg/g dry weight, was detected in the stratified sediment of central Lake Päijänne, dated to the mid-1970s (depth 12–15 cm). After notable changes in processes and effluent treatment, the amounts of sterols in effluents must have diminished, as shown by the sterol content in the sediment downstream from the mills. Therefore, the concentrations were about 10% of the historical maximum in the surface sediment (depth 0–3 cm) in both downstream sites investigated at Lake Päijänne. However, these concentrations were clearly over the natural background (10–50 μg/g) occurring in the subsamples of the pre-industrial phase (depth 36–44 cm) as well as in the reference site of southern Lake Saimaa, the second investigated lake. At a nearby site of a pulp and paper mill in southern Lake Saimaa, sterols were most abundant (1760 μg/g dry weight) in the sediment layer 0–5 cm despite the improved process control during last few decades. This study showed the abundance of ecotoxicologically harmful compounds in downstream sediment sites of pulp and paper industry.     

Automated Identification of Coronal Holes from Synoptic EUV Maps

Coronal holes (CHs) are regions of open magnetic field lines in the solar corona and the source of the fast solar wind. Understanding the evolution of coronal holes is critical for solar magnetism as well as for accurate space weather forecasts. We study the extreme ultraviolet (EUV) synoptic maps at three wavelengths (195 Å/193 Å, 171 Å and 304 Å) measured by the Solar and Heliospheric Observatory/Extreme Ultraviolet Imaging Telescope (SOHO/EIT) and the Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) instruments. The two datasets are first homogenized by scaling the SDO/AIA data to the SOHO/EIT level by means of histogram equalization. We then develop a novel automated method to identify CHs from these homogenized maps by determining the intensity threshold of CH regions separately for each synoptic map. This is done by identifying the best location and size of an image segment, which optimally contains portions of coronal holes and the surrounding quiet Sun allowing us to detect the momentary intensity threshold. Our method is thus able to adjust itself to the changing scale size of coronal holes and to temporally varying intensities. To make full use of the information in the three wavelengths we construct a composite CH distribution, which is more robust than distributions based on one wavelength. Using the composite CH dataset we discuss the temporal evolution of CHs during the Solar Cycles 23 and 24.     

Tilt of Sunspot Bipoles in Solar Cycles 15 to 24

We use recently digitized sunspot drawings from Mount Wilson Observatory to investigate the latitudinal dependence of tilt angles of active regions and its change with solar cycle. The drawings cover the period from 1917 to present and contain information as regards polarity and strength of magnetic field in sunspots. We identified clusters of sunspots of same polarity, and used these clusters to form “bipole pairs”. The orientation of these bipole pairs was used to measure their tilts. We find that the latitudinal profile of tilts does not monotonically increase with latitude as most previous studies assumed, but instead, it shows a clear maximum at about 25?–?30 degree latitudes. Functional dependence of tilt (\(\gamma\)) on latitude (\(\varphi\)) was found to be \(\gamma= (0.20\pm0.08) \sin(2.80 \varphi) + (-0.00\pm0.06)\). We also find that latitudinal dependence of tilts varies from one solar cycle to another, but larger tilts do not seem to result in stronger solar cycles. Finally, we find the presence of a systematic offset in tilt of active regions (non-zero tilts at the equator), with odd cycles exhibiting negative offset and even cycles showing the positive offset.