科尔沁沙地78种植物繁殖体重量和形状比较

研究了科尔沁沙地 78种植物的繁殖体 (2 3种为种子 ,5 5种为果实 )重量和形状 ,其重量差别很大 ,最小的单粒重不足 0 .1mg,最大的超过 130 mg;形状差异也很大 ,最小的方差不足 0 .0 3,最大的超过 0 .18。综合本研究和以前研究的全部 14 0种植物的研究结果 ,进行了分析。结果表明 :1计有 2 4种植物繁殖体单粒重小于 1mg并接近圆球形 (方差小于 0 .0 9) ,它们可能具有持久种子库 ;2 1年生植物 (平均方差为 0 .0 70 )与 2年生植物 (平均方差为 0 .12 9)间的形状差异显著 (P<0 .0 5 ) ,2年生植物的繁殖体更加扁、长 ;1年生植物也与多年生草本植物 (平均方差为 0 .10 9)之间形状差异显著 (P<0 .0 5 ) ,多年生草本植物的繁殖体更加扁、长 ;3有 5 5 %的豆科植物、70 %的藜科植物繁殖体接近圆球形 (方差 <0 .0 6 ) ,所有的菊科、萝摩科植物繁殖体都很扁、长 (方差 >0 .0 6 )。豆科植物显著比菊科、禾本科、藜科植物繁殖体的重量大 (P<0 .0 5 ) ;4繁殖体附属物在植物的传播和定居方面具有重要的作用 :6种萝摩科植物和 3种杨柳科植物具有绢毛 ,6 0 %的菊科植物具有冠毛 ,6种植物有翅 ,8种植物有宿存花柱或宿存花萼 ,这些植物可能易于被风传播 ;5 4 %的禾本科植物具芒 ,减小了传播可能 ;苍耳、雾冰藜、鹤虱、蒺藜、

Cloning and expression of glucose regulated protein 78 (GRP78) in Fenneropenaeus chinensis

GRP78 (78 kDa glucose-regulated protein), also known as BiP (immunoglobulin heavy-chain-binding protein), is an essential regulator of endoplasmic reticulum (ER) homeostasis because of its multiple functions in protein folding, ER calcium binding, and controlling of the activation of transmembrane ER stress sensors. In this report, we cloned the full length cDNA of GRP78 (FcGRP78) from Chinese shrimp Fenneropenaeus chinensis. This cDNA revealed a 2,325 bp with 1,968 bp open reading frame encoding 655 amino acids. This is the first reported GRP78 gene in Crustacea. The deduced amino acid sequence of FcGRP78 shared high identity with previously reported insect GRP78s: 86, 87 and 85% identity with GRP78s of Drosophila melanogaster, Aedes aegypti and Bombyx mori, respectively. Northern blot analysis shows that FcGRP78 is ubiquitously expressed in tissues of shrimp. Heat shock at 35A degrees C significantly enhanced the expression of FcGRP78 at the first hour, reached the maximum at 4 h post heat shock, dropped after that and resumed to the normal level until 48 h of post recovery at 25A degrees C. Additionally, differential expression of FcGRP78 was detected in haemocytes, hepatopancreas and lymphoid organ when shrimp were challenged by white spot syndrome virus (WSSV). We inferred that FcGRP78 may play important roles in chaperoning, protein folding and immune function of shrimp.

Measurements of the heat capacity of an azeotropic mixture of water and n-butanol from 78 to 320 K

Molar heat capacities of n-butanol and the azeotropic mixture in the binary system [water (x=0.716) plus n-butanol (x=0.284)] were measured with an adiabatic calorimeter in a temperature range from 78 to 320 K. The functions of the heat capacity with respect to thermodynamic temperature were established for the azeotropic mixture. A glass transition was observed at (111.9 +/- 1.1) K. The phase transitions took place at (179.26 +/- 0.77) and (269.69 +/- 0.14) K corresponding to the solid-liquid phase transitions of. n-butanol and water, respectively. The phase-transition enthalpy and entropy of water were calculated. A thermodynamic function of excess molar heat capacity with respect to temperature was established, which took account of physical mixing, destructions of self-association and cross-association for n-butanol and water, respectively. The thermodynamic functions and the excess thermodynamic ones of the binary systems relative to 298.15 K were derived based on the relationships of the thermodynamic functions and the function of the measured heat capacity and the calculated excess heat capacity with respect to temperature.

Chemical composition of B-type supergiants in the OB 8, OB 10, OB 48, OB 78 associations of M 31

Absolute and differential chemical abundances are presented for the largest group of massive stars in M31 studied to date. These results were derived from intermediate resolution spectra of seven B-type supergiants, lying within four OB associations covering a galactocentric distance of 5-12 kpc. The results are mainly based on an LTE analysis, and we additionally present a full non-LTE, unified model atmosphere analysis of one star (OB 78-277) to demonstrate the reliability of the differential LTE technique. A comparison of the stellar oxygen abundance with that of previous nebular results shows that there is an off set of between similar to0.15-0.4 dex between the two methods which is critically dependent on the empirical calibration adopted for the R 23 parameter with [O/H]. However within the typical errors of the stellar and nebular analyses (and given the strength of dependence of the nebular results on the calibration used) the oxygen abundances determined in each method are fairly consistent. We determine the radial oxygen abundance gradient from these stars, and do not detect any systematic gradient across this galactocentric range. We find that the inner regions of M31 are not, as previously thought, very "metal rich". Our abundances of C, N, O, Mg, Si, Al, S and Fe in the M31 supergiants are very similar to those of massive stars in the solar neighbourhood.