Ammonia volatilized from aboveground parts of winter wheat was collected with an enclosuregrowth chamber and measured from jointing to maturing stage. The results showed that ammonia releasedfrom unfertilized plants grown in high and low fertility soils remained at low rates of 2.3 and 0.9 μg NH3 40plant-1 h-1 respectively at late filling stage. However, fertilized plants rapidly increased the rates to 43.4 and52.2 μg NH3 40 plant-1 h-1 in the high and low fertility soils, respectively, at the same period. The released a-mount was different in different parts of plants. At filling stage, lower senescing stems and leaves volatilizedmore ammonia than upper parts, i.e. , ears and flag leaves that grew normally, with an average of 1.4 and0.7 μg NH3 20 plant-1 h-1 respectively, strongly suggesting that it was the senile organs that released largeamounts of ammonia. At the grain filling stage, shortage of water supply (drought stress) reduced ammoniavolatilization. The average rate of ammonia released under water stress was 0.9 μg NH3 40 plant-1 h-1 , but 1.2μg NH3 40 plant-1 h-1 with moderate water supply. Application of N together with P fertilizer resulted in ahigher ammonia volatilization than N fertilization alone at the maturing stage. The average rate released was135.3 μg NH3 40 plant-1 h-1 when 0.4 g N and 0.13 g P had been added to per kg soil, while 33.7 μg when0.4 g N added alone. Ammonia volatilization from plants was closely related with plant biomass and N up-take; P fertilization increased plant biomass and N uptake and therefore increased its release.
WANG Zhao-hui and LI Sheng-xiuCollege of Resources and Environmental Sciences, Northwestern Science and Technology University of Agricultureand Forestry, Yangling 712100, P. R. China
The thermal history of cosmic gas in the dark ages remains largely unknown.It is important to quantify the impact of relevant physics on the IGM temperature between z=10 and z^30,in order to interpret recent and oncoming observations,including results reported by EDGES.We revisit the gas heating due to structure formation shocks in this era,using a set of fixed grid cosmological hydrodynamical simulations performed by three different codes.In all our simulations,the cosmic gas is predicted to be in multiphase state since z>30.The gas surrounding high density peaks gradually develops a relation more sharp than T∝ρ2/3,approximately T∝ρ2,from z=30 to z=11,might be due to shock heating.Meanwhile,the gas in void region tends to have a large local Mach number,and their thermal state varies significantly from code to code.In the redshift range 11-20,the mass fraction of gas shock heated above the CMB temperature in our simulations is larger than previous semi-analytical results by a factor of 2 to 8.At z=15,the fraction varies from^19%to 52%among different codes.Between z=11 and z=20,the gas temperature<1/TK>M-1 is predicted to be^10-20 K by two codes,much higher than the adiabatic cooling model and some previous works.However,in our simulations performed by RAMSES,<1/TK>M-1is predicted to be even below the temperature required to explain result of the EDGES.Given the fact that different codes give different predictions,currently,it seems a challenge to make solid prediction on the temperature of gas at z^17 in simulations.
