T. K. Das

Distribution of sunspots according to their magnetic fluxes

The occurrence frequency distribution of sunspots in different magnetic flux values has been examined. The number of sunspots decreases as φ-1.9 for sunspots with magnetic flux greater than 3 × 1021 Maxwell, where φ is the said flux of a sunspot.

A comparative study of Hα-flares of different visual features in relation to radio bursts and sunspots

Solar Hα-flares now reported with their distinctive visual features have been statistically examined for a period of about eight years in relation to their different characteristics, flare-burst and flare-sunspot association. Important results obtained are: (i) Integrated intensity changes from the highest to the lowest values in the order F, H, E, and D flare type, whereas, impulsiveness in the order H, F, E, and D type, (ii) Flare-burst association is frequency dependent and is highest and lowest for H and D types respectively in almost all the frequencies, (iii) Most of the flares of D, E, and F types are associated with sunspots of βp, αp, and δ configurations having field strength 1500–2500 G, while that of H type with βp and β configurations having field strength 1000–2000 G.

Closed eruption of impacted mandibular canine

Abstract An impacted tooth is defined as partially or completely unerupted tooth which lies against adjacent tooth, overlying soft tissues or bone so that its further eruption is unlikely. One of the rare or infrequent tooth that is impacted in the oral cavity is mandibular canine. The current case report demonstrates a simple way to treat an impacted right mandibular canine using lingual arch made up of 19 gauge round stainless steel arch wire with soldered spring (19 × 25″ stainless steel). Closed eruption technique with a Beggs bracket bonded on the labial surface of impacted canine was chosen as it facilitates the preservation of the attached gingiva around the newly erupted tooth.

The role of photospheric magnetic field in the development of solar flares

A statistical investigation has been made about the flare-process in relation to the photospheric magnetic field and configuration. It is understood from the analysis that the flare energy bears a linear relationship with the rate of change of flux of the longitudinal component of photospheric magnetic field.