PROBOSIS LATERALIS

Proboscis lateralis is an embryological inconsistency which is identified with the middle facial cleft. This outcomes in fragmented arrangement of one side of nose. This underdeveloped nose structure is situated close to the nose but off the midline. It seems like a cylinder and is appended at the undeveloped combination line anytime between the foremost maxillary interaction and the frontonasal cycle. This issue ought to be tended to at an early age and with stage shrewd methodology as this proboscis itself is a valuable design for remaking. We report an instance of proboscis lateralis in a 1-year-old female patient.

The manifestation of the main quantitative characteristics in the populations of second-generation beans and their parent forms

The aim of the research was to study the nature of variability of the main quantitative traits in hybrid populations of the second generation Phaseolus vulgaris L. within the framework of the task 13.00.01.28. F “To study the nature of the inheritance of quantitative traits in hybrids of create a starting material with improved flavoring properties.As a result of the studies carried out, it was found that regardless of the duration of the growing season of the parent components of the crossing, in the hybrid populations of the second generation, the limits of variability for this indicator went beyond the limits of the variability of the parent forms. The average values of the duration of the growing season in hybrids were intermediate between the indicators of the corresponding parent forms. The coefficients of variation in the parent forms were insignificant (1.1 – 1.4%); in hybrid populations they were low – from 4.9% (Line 744-14 / Ukrainka) to 9.2% (Line 741-14 / Suita).In terms of plant height, the limits of variability of hybrid offspring F2 went beyond the limits of variability of the parent components. The average values of the trait in hybrid populations significantly exceeded the corresponding indicators of the parent forms. The degree of variability in plant height of hybrid populations was significant in the combination Line 872-14 / Podolyanka-1 (the parent components differ in the type of plant growth) and was equal to 20.6% versus 3.5% and 4.9% for the corresponding parent forms. In other hybrid populations, the coefficient of variation was average (Ukrainka / Suita-16.5%; Line 741-14 / Suita – 13.5%; Line 744-14 / Ukrainka -10.1%) The degree of variability of the corresponding parental forms was in the range from 2.8% to 3.1%.The widest range of variability was observed according to the characteristics of the mass of seeds from the plant, the number of seeds from the plant, the number of beans from the plant. The degree of variability of the seed mass from the plant in hybrid populations ranged from 30.3% to 39.1% (in the parent forms from 9.1% to 21.7%); the number of seeds from the plant from 22.3% to 40.7% (in the parent forms from 9.8% to 20.1%); the number of beans from the plant from 28.1% to 38.3% (in the parent forms from 4.7% to 16.2%). The degree of variation of the studied traits in hybrid populations was 2–3 times higher than in the parent forms.By the weight of 100 seeds in the offspring of the second generation, the range of variation was much wider than this indicator in the parent forms. The degree of variability on this trait was average for hybrid populations (from 10.6% to 13.4%), and insignificant for parental forms (from 3.7% to 6.6%).It is possible that the most valuable in terms of breeding may be the hybrid combination Line 872-14/Podolyanka, from the widest range of variability in the studied traits in the second generation population.

Identifications of Some Highly-Ionized Iron and Nickel Lines in the 200–400 Å Region of the Solar Spectrum

A number of previously unclassified multiplets of FeXIV, XIII, XII, and XI produced by transitions of the type 3s23pn–3s3pn+1 are identified in the XUV spectrum of the Sun. The iron lines account for most of the previously unidentified strong lines between 330 and 370 Å. Solar observations of especial value for the investigation of the 300–400 Å region were the slitless spectroheliograms of September 22, 1968 (Purcell and Tousey, 1969) and November 4, 1969 (Tousey, 1971) – on which the image of a flare was recorded.Other solar identifications in the same spectral region include the resonance lines of NiXVII and NiXVIII, and one 3p–3d multiplet of FeXIII. The solar blend at 417 Å involving the FeXV inter-combination line and SXIV is resolved.