SiO in G34.26: Outflows and shocks in a high mass star forming region

We have looked for SiO emission as evidence of shocks in the high mass star formation region G34.26+0.15. JCMT, VLA and FCRAO observations show that SiO emission is widespread across the region. The SiO emission highlights a massive, collimated out ow and other regions where stellar winds are interacting with molecular clumps. As in other star forming regions, there is also SiO at ambient velocities which is related to the out ow activity. No strong SiO abundance enhancement was measured in either the out ow or the low velocity gas, though abundances up to 10(-8) are possible if the SiO is locally enhanced in clumps and optically thick. SiO emission is not detected from the hot core itself, indicating either that SiO is not strongly enhanced in the hot core or that column densities in the region where grain mantle evaporation has taken place are low. In line of sight spiral arm clouds, we measure a SiO abundance of 0.4-2 x 10(-10), consistent with previous estimates for quiescent clouds.

A 330-360 GHz spectral survey of G34.3+0.15 - III. The outer halo

We have undertaken a 330-360 GHz molecular line survey of the halo gas surrounding the hot core associated with G34.26+0.15. In contrast to our molecular line survey of the hot core itself, where 338 lines from at least 38 species were detected, only 18 lines from 9 species were detected in the halo. The lines are mainly single transitions of simple di atomic and triatomic molecules. Lower limits to their column densities have been evaluated by an LTE method. In the case of methanol, where four transitions were detected, the rotation temperature and column density have been evaluated by the rotation diagram technique. We have modified the previous depth-dependent chemical model developed in Paper II to calculate the column densities observed along a general line of sight drawn through the model cloud. The model is also extended to produce beam-averaged column densities for better comparison with those observed. We compare the model column densities with those observed and make recommendations for future depth-dependent chemical modelling of hot cores.

A 330-360 GHz spectral survey of G34.3+0.15 .2. Chemical modelling

We describe a detailed depth-and time-dependent model of the molecular cloud associated with the ultracompact H II region G 34.3+0.15. Previous work on observations of NH3 and CS indicates that the molecular cloud has three distinct physical components:- an ultracompact hot core, a compact hot core and an extended halo. We have used the physical parameters derived from these observations as input to our detailed chemical kinetic modelling. The results of the model calculations are discussed with reference to the different chemistries occuring in each component and are compared with abundances derived from our recent spectral line survey of G 34.3+0.15 (Paper I).

THE DETECTION OF HOT ETHANOL IN G34.3+0.15

Hot molecular cores in star-forming regions are known to have gas-phase chemical compositions determined by the evaporation of material from the icy mantles of interstellar grains, followed by subsequent reactions in the gas phase. Current models suggest that the evaporated material is rich in hydrogenated species, such as water, methane and methanol. In this paper, we report the detection of 14 rotational transitions of ethanol in the submillimetre spectrum of the molecular cloud associated with the ultra-compact H II region G34.3+0.15. We derive a rotation temperature of 125 K and a beam-averaged column density of 2.0x10(15) cm(-2), corresponding to a fractional abundance on the order of 4x10(-9). This large abundance, which is a lower limit due to the likelihood of beam dilution, cannot be made by purely gas-phase processes, and we conclude that the ethanol must be formed efficiently in the grain surface chemistry. Since it has been argued previously that methanol is formed via surface chemistry, it appears that alcohol formation may be a natural by-product of surface reactions.

Desempenho de genótipos de girassol no cerrado do leste Maranhense, ano agrícola 2013/2014.

RESUMO: No ano agrícola 2013/2014, foram conduzidos três ensaios de avaliação de genótipos de girassol, sendo dois no município de Mata Roma e um em Magalhães de Almeida, com o objetivo de identificar materiais promissores para produção de grãos e óleo. O espaçamento utilizado foi de 0,70 m entre linhas com plantas distanciadas de 0,30 m. A adubação de fundação constou de 200 kg ha-1 da fórmula 05-30-15 + micronutrientes e cobertura aos 30 dias após semeadura, usando-se 30 kg ha-1 de N e 30 kg ha-1 de K2O. Em Mata Roma, a produtividade de grãos no ensaio final 01 variou de 1.866 kg ha-1 a 2.567 kg ha-1, obtida nos genótipos Embrapa 122 e BRS G34, respectivamente, ficando a média geral do ensaio em 2.095 kg ha-1. No ensaio final 02 a produtividade de grãos variou de 1.705 kg ha-1 a 2.036 kg ha -1 para os genótipos Helio 250 e MG 360, REspectivamente, com média geral de 1.834 kg ha-1. Em Magalhães de Almeida a produtividade de grãos obtida no ensaio final constou de 1.600 kg ha-1 no genótipo Helio 251, 2.110 kg ha-1 no CF 101 e média Geral do ensaio de 1.908 kg ha -1. Os maiores teores de óleo obtidos nos três ensaios foram 40,1%, 40,6%, 40,9% e 41,4%, respectivamente, nos genótipos CF 101, Paraíso 20, BRS G41 e MG 360. ABSTRACT: In the agricultural year 2013/2014, three sunflowers genotypes tests were conducted in the state of Maranhão: two in the county of Mata Roma and one in Magalhães de Almeida, in order to identify promising materials for the production of grain and oil. The spacing used was 0.70 m between rows with plants spaced of 0.30 m. The foundation of fertilization consisted of 200 kg ha-1 formula 05-30-15 + micro-nutrient and coverage on 30 days after sowing, using 30 kg ha-1 of N and 30 kg ha-1 of K2O. In Mata Roma, grain yield in the final test 01 ranged from 1,866 kg ha-1 to 2,567 kg ha-1, obtained at Embrapa 122 and BRS G34 genotypes, respectively, getting the overall average of the test in 2,095 kg ha-1. In the final test 02, the grain yield ranged from 1,705 kg ha-1 to 2,036 kg ha-1 for Helio 250 and MG 360 genotypes, respectively, with overall average of 1,834 kg ha-1. In Magalhães de Almeida the grain yield obtained in the final test consisted of 1,600 kg ha-1 in the genotype Helio 251, 2,110 kg ha-1 in the CF 101 and overall average test of 1,908 kg ha-1. The highest oil content obtained in the three tests were 40.1%, 40.6%, 40.9% and 41.4%, respectively, in the 101 CF genotypes, Heaven 20, BRS G41 and MG 360.

Mergers and Acquisitions in Vietnam’s Emerging Market Economy, 1990-2009

This paper is the first major and thorough study on the M&A activities in Vietnam’s emerging market economy, covering almost entirely the M&A history after the launch of Doi Moi. The surge in these activities since mid-2000s by no means incidentally coincides with the jump in FDI and FPI inflows into the nation. M&A industry in Vietnam has its socio-cultural traits that could help explain economic happenings, with anomalies and transitional characteristics, far better than even the most complete set of empirical data. Proceeds from sales of existing assets and firms have mainly flowed into the highly speculative industries of securities, banking, non-bank financials, portfolio investments and real estates. The impacts of M&A on Vietnam’s long-term prosperity are, thus, highly questionable. An observable high degree of volatility in the M&A processes would likely blow outthe high ex ante expectations by many speculators, when ex post realizations finally arrive. The effect of the past M&A evolution in Vietnam has been indecisively positive or negative, with significant presence of rent-seeking and likelihood of causing destructive entrepreneurship. From a socio-economic and cultural view, the degree of positive impacts it may result in for domestic entrepreneurship will perhaps be the single most important indicator.

The Physical and Chemical Structure of Hot Molecular Cores

We have made self-consistent models of the density and temperature profiles of the gas and dust surrounding embedded luminous objects using a detailed radiative transfer model together with observations of the spectral energy distribution of hot molecular cores. Using these profiles we have investigated the hot core chemistry which results when grain mantles are evaporated, taking into account the different binding energies of the mantle molecules, as well a model in which we assume that all molecules are embedded in water ice and have a common binding energy. We find that most of the resulting column densities are consistent with those observed toward the hot core G34.3+0.15 at a time around 10^4 years after central luminous star formation. We have also investigated the dependence of the chemical structure on the density profile which suggests an observational possibility of constraining density profiles from determination of the source sizes of line emission from desorbed molecules.

A survey of molecular line emission towards ultracompact HII regions

We have used the JCMT to survey molecular line emission towards 14 ultracompact HII regions (G5.89, G9.62, G10.30, G10.47, G12.21, G13.87, G29.96, G31.41, G34.26, G43.89, G45.12, G45.45, G45.47, and G75.78). For each source, we observed up to ten 1 GHz bands between 200 and 350 GHz, covering lines of more than 30 species including multiple transitions of CO isotopes, CH3OH, CH3CCH, CH3CN and HCOOCH3, and sulphuretted molecules. The number of transitions detected varied by a factor of 20 between sources; which were chosen following observations of high-excitation ammonia (Cesaroni et al. 1994a) and methyl cyanide (Olmi et al. 1993). In half our sample (the line-poor sources), only (CO)-O-17: (CO)-O-18, SO, (CS)-S-34 and CH3OH were detected. In the line-rich sources, we detected over 150 lines, including high excitation lines of CH3CN, HCOOCH3; C2H5CN, CH3OH, and CH3CCH. We have calculated the physical conditions of the molecular gas. To reproduce the emission from the line-rich sources requires both a hot, dense compact core and an ambient cloud consisting of less dense, cooler gas. The hot cores, which are less than 0.1 pc in size; reach densities of at least 10(8) cm(-3) and temperatures of more than 80 K. The line-poor sources can be modelled without a hot core by a 20-30 K, 10(5) cm(-3) cloud. We find no correlation between the size of the HII region and the current physical conditions in the molecular environment. A comparison with chemical models (Millar et al. 1997) confirms that grain surface chemistry is important in hot cores.

Trade Liberalization and the Profitability of Domestic Mergers.

It is often thought that a tariff reduction, by opening up the domestic market to foreign firms, should lessen the need for a policy aimed at discouraging domestic mergers. This implicitly assumes that the tariff in question is sufficiently high to prevent foreign firms from selling in the domestic market. However, not all tariffs are prohibitive, so that foreign firms may be present in the domestic market before it is abolished. Furthermore, even if the tariff is prohibitive, a merger of domestic firms may render it nonprohibitive, thus inviting foreign firms to penetrate the domestic market. In this paper, we show, using a simple example, that in the latter two cases, abolishing the tariff may in fact make the domestic merger more profitable. Hence, trade liberalization will not necessarily reduce the profitability of domestic mergers.

Suplementação com levedura de Crômio eleva a concentração sérica de Crômio em bovinos

This study evaluated the effect of daily chromium supplementation at growing doses on serum Cr levels in cattle. Sixty Nellore heifers 2 to 5 years old were randomly assigned to one of four groups (15 heifers/group) fed non-fertilized Brachiaria decumbens pasture. In the control group (Gc), the heifers received a mineral mixture without Cr. In the other groups, heifers received 0.59, 1.19 or 2.38 mg Cr+3/animal/day, groups G8,5, G17 and G34, respectively. Blood samples were collected on days 0, 30 and 60. Serum concentration of chromium was determined by graphite furnace atomic absorption spectrophotometer. The chromium source used was the chromium yeast. The results do not support any significant difference (p>0.05) among serum chromium levels of heifers in groups Gc, G8,5, G17 and G34 at a same observation day. Only effect of supplementation time was detected in group G34. In this group there was significant increase (p<0,05) in the concentration serum chromium 60 days after the beginning of the experiment. Concluded Cr yeast can be used as the source of this mineral element for animals and supplementation with 2.38 mg/ cattle/day was the dose that most increased the serum concentration of Cr in Nellore cattle during the experimental period.

Das Strafverfahren gegen die märkischen Juden im Jahre 1510

Friedrich Holtze