Studies with 60Co-Radiated Guar (Cyamopsis Tetragonoloba) (L.) Taub

Author Institution: Academic Faculty of Genetics, The Ohio State University, Columbus, OhioDry seeds of G-II (bushy, fodder type) and G-IV (erect, pod type) varieties of Punjab guar {Cyamopsis tetragonoloba) were radiated with gamma rays using 60Co as source of radiation. The doses applied were 5,000, 10,000, 20,000, and 30,000 r. The radiation speeded up germination, increased the rate of root growth, and expanded the range of plant height and stem girth in the generation from the radiated seeds (Ri). Other morphological variants in Ri were: Chlorophyll defects, small-leaved and small-poded types, unusually tall and unusually small plants, and chimaeras for pod and leaf size. In R2 none of the above characters excepting chlorophyll defects appeared, thus establishing that non-genetic changes were responsible for other variations. In R2 and R3, however, segregation was observed for plant height and branching from both G-II and G-IV. In no case were the number of genes involved determined

Research Notes: University of Nevada

Glycine max (L.) Merrill (soybean) is said to have at least 18 loci responsible for the development of chlorophyl (Bernard and Cremeens, 1970). One of these, y11, discovered by Weber and Weiss (1959), is characterized by the development of golden yellow color of the leaves and stem in homozygous (y11 y11 ) combination. The heterozygous plants are light green and differ from the y11y11 homozygotes which have normal, dark green color

Star formation activity in the southern Galactic HII region G351.63-1.25

The southern Galactic high mass star-forming region, G351.6-1.3, is a HII region-molecular cloud complex with a luminosity of 2.0 x 10^5 L_sun, located at a distance of 2.4 kpc. In this paper, we focus on the investigation of the associated HII region, embedded cluster and the interstellar medium in the vicinity of G351.6-1.3. We address the identification of exciting source(s) as well as the census of stellar populations. The ionised gas distribution has been mapped using the Giant Metrewave Radio Telescope (GMRT), India at three continuum frequencies: 1280, 610 and 325 MHz. The HII region shows an elongated morphology and the 1280 MHz map comprises six resolved high density regions encompassed by diffuse emission spanning 1.4 pc x 1.0 pc. The zero age main-sequence (ZAMS) spectral type of the brightest radio core is O7.5. We have carried out near-infrared observations in the JHKs bands using the SIRIUS instrument on the 1.4 m Infrared Survey Facility (IRSF) telescope. The near-infrared images reveal the presence of a cluster embedded in nebulous fan-shaped emission. The log-normal slope of the K-band luminosity function of the embedded cluster is found to be 0.27 +- 0.03 and the fraction of the near-infrared excess stars is estimated to be 43%. These indicate that the age of the cluster is consistent with 1 Myr. The champagne flow model from a flat, thin molecular cloud is used to explain the morphology of radio emission with respect to the millimetre cloud and infrared brightness.Comment: 18 pages, 8 figures, To be published in MNRA

Radio and infrared study of the star forming region IRAS 20286+4105

A multi-wavelength investigation of the star forming complex IRAS 20286+4105, located in the Cygnus-X region, is presented here. Near-infrared K-band data is used to revisit the cluster / stellar group identified in previous studies. The radio continuum observations, at 610 and 1280 MHz show the presence of a HII region possibly powered by a star of spectral type B0 - B0.5. The cometary morphology of the ionized region is explained by invoking the bow-shock model where the likely association with a nearby supernova remnant is also explored. A compact radio knot with non-thermal spectral index is detected towards the centre of the cloud. Mid-infrared data from the Spitzer Legacy Survey of the Cygnus-X region show the presence of six Class I YSOs inside the cloud. Thermal dust emission in this complex is modelled using Herschel far-infrared data to generate dust temperature and column density maps. Herschel images also show the presence of two clumps in this region, the masses of which are estimated to be {\sim} 175 M{\sun} and 30 M{\sun}. The mass-radius relation and the surface density of the clumps do not qualify them as massive star forming sites. An overall picture of a runaway star ionizing the cloud and a triggered population of intermediate-mass, Class I sources located toward the cloud centre emerges from this multiwavelength study. Variation in the dust emissivity spectral index is shown to exist in this region and is seen to have an inverse relation with the dust temperature.Comment: 20 pages, 16 figures, accepted for publication in MNRA