The analysis of the Ca-K line spectra as a function of latitude and integrated over the visible disk obtained during the period of 1989–2011 at the Kodaikanal Solar Tower Telescope shows that the FWHM of the K1 distribution at different latitudes varies by negligible amount at about 60° latitude whereas it varies significantly at other latitudes. Findings, especially the fewer variations in mid-latitude belts as compared to polar regions and complex variation in the shift in the activity around 60° latitude belt, will have important implications on the modeling of solar dynamos. Further, we have generated a uniform set of digitized Ca-K line images by selecting images considering the intensity distribution of the images corrected for the instrumental vignetting for the data obtained at Kodaikanal during the 20th century. Then, we have determined the percentage of plage and network areas by using the intensity and area threshold values.

The present study was conducted to determine the elemental concentration and bacterial presence in the ocean on the two sides of Brøggerhalvøya, a peninsula in Svalbard. Sediments from 25 different locations were collected and subjected to elemental analysis using inductively coupled plasma mass spectrometry (ICPMS). In total, 21 elements were analysed. The elements in their decreasing order of concentrations on the Kongsfjorden side of Brøggerhalvøya were Fe> Mn> Ba > V > Zn > Sr > Rb > Cr > Li > Ni > As > Pb > Cu > Co > Cs >Ag > Be > U> Bi >Tl > Cd while that for Forlandsendet side of Brøggerhalvøya they were Fe > Ba >Mn > V> Sr > Zn > Rb > Cr > Li > Ni > Pb > Cu > As > Co > Cs > Be > U> Tl > Bi > Cd. On the other hand, at a coastal outcrop, elements in their decreasing order of concentration were Fe > Mn > Cr > Sr > Ba > Rb > Cr > Zn > V > Rb > Ni > Li > Co > Cu > As > Pb > Cs > Be > Cd > Tl > U > Bi. AMS dates confirmed the age of outcrop sediment to be 12,496 to 42,500 BP. The crustal enrichment factor calculated for all the elements with reference to Fe values, demonstrates that the elements have derived from a crustal source. Total bacterial counts ranged from 3.30 × 105 to 3.02 × 106 per gm soil sediment. Culturable bacterial counts in these sediments were between 2.00 × 102 to 2.09 × 105 CFU's per gm. Overall comparison showed high Fe and Mn concentrations around Brøggerhalvøya, due to the presence of specific bacteria which play key roles in metal cycling and carry out biogeochemical transformations.

The present study was conducted to measure the elemental concentration and bacterial deposition in the firn-cores at the Midre Lovénbreen glacier, Svalbard. Firn-cores up to 1m deep were collected and divided into three subsections. These were subjected to elemental analysis using inductively coupled plasma mass spectroscopy (ICPMS). In all 20 elements were analysed. The crustal enrichment factors calculated for these elements on the basis of Fe values, demonstrate that the elements have derived from both crustal and anthropogenic sources. For certain elements there also exists a possibility of input from sea salt spray. Total bacterial counts in these firn samples ranged from 1.03 × 105 to 3.67 × 105 per ml of meltwater. Culturability of these bacterial cells, in comparison to the total count was very low. At 4°C the maximum culturability was <1.4% of the total count while at 15°C it was still lower (~1%).

Supergranules are observed in the high photosphere as large convection eddies with horizontal diverging flows from the cell centre and subsiding flows at the cell borders.

The analysis of an eruptive prominence and disappearing quiescent filaments indicates that the prominence height on the limb increases after the filament develops a twist as seen in the Hα on the disc. The increase in prominence height, large change in the shear angle, and the appearance of filament as a U-shaped structure before the disappearance of the filament or prominence eruption can be explained by assuming that the middle portion of the filament rises above the solar surface with its edges anchored in the chromosphere. Further, the loop-like structure of the filament splits into two parts 2–3 days prior to its disappearance and the gap between the two increases with time. The increasing gap and simultaneous disappearance of both parts of the filament suggests that heating of the top of the loop-like structure begins about 2 days before its disappearance. The cause for this portion of the filament not being visible in Hα may be that it is heated to a high temperature.

High resolution spectra are being taken in ionized calcium K-line at different latitudes and integrated over the visible 180 degree longitude. These have been analysed to study the variability of the line parameters as a function of latitude. These spectra are being obtained on a regular basis and large data base will be used to study chromospheric rotation, differential rotation in chromosphere, activity and variability of K-line parameters as function of latitude and solar cycle phase. Further, an optical arrangement has been worked out to obtain the spectra along the latitudes of the solar image in the light integrated over longitudes. This involves the unidirectionally focusing of the image in N-S direction.

To study the evolution and decay of large convective cells known as supergranules, a solar telescope was set up at Maitri, Indian permanent station in Antarctica region during the local summer months (December 1989 through March 1990). A continuous sequence of calcium-K-line filtergrams for 106 hours with an interval of about 10 minute was obtained. The analysis of this data indicates that most probable life time of the calcium K network is about 20 hours. The life time depends upon the size of the cell and is larger for bigger cells. The data also show that cells (of given size) associated with remanent magnetic field regions live longer than those in the region free from magnetic field regions.

The sun as a star has been studied by many observers by monitoring the calcium K line profile. Skumanich et al (1984) proposed a three component model of the solar cycle variability of calcium K emission using extant contrast and fractional area parameters for (1) cell (2) network and (3) plage components. The computed line profile agreed well with the observed one at the solar minimum by taking the contribution of only cell and network features and using extant limb-darkening laws. The occurrence of plages during the growth of the solar cycle was found to be insufficient to account for the increase in K emission and therefore, they introduced an additional network component, ‘Active network’ in excess of the quiet sun value to explain the observed excess emission during the maximum phase.