低本底α、β测量仪效率校准研究

简述了低本底α、β测量仪效率校准的基本原理,研究了自吸收和面积与探测效率的关系,评定了效率校准中的不确定度,并分析了效率在α、β样品测量中的应用。     

环糊精包结分离制备高纯度辛基二茂铁同分异构体

以辛基二茂铁工业品与本实验室前期分离得到的三种一元辛基二茂铁混合制剂(C8-Fc)为原料,以β-环糊精包结硅胶得到包结分离柱Immo-CD-1,确定了包结分离制备高纯度辛基二茂铁同分异构体的原料;在此基础上,利用正交实验的方法,确定了包结分离的主要影响因素与最佳条件,发现水分含量对于分离效果的影响最为显著,经Immo-CD-1柱分离得到纯度为97.2%的(4-辛基)-二茂铁、纯度大于96%的(3-辛基)-二茂铁以及(2-辛基)-二茂铁和(3-辛基)-二茂铁的混合物;利用类似的方法,以羟丙基-β-环糊精为主体材料制备包结分离柱Immo-CD-2,并对上述所得到的(2-辛基)-二茂铁和(3-辛基)-二茂铁混合物进行包结分离,经优化分离后,得到纯度大于95%的(2-辛基)-二茂铁。     

Dy对EB-PVDβ-NiAl涂层高温瞬态氧化行为的影响(英文)

β-NiAl是一种有前景的应用于1150°C以上的抗氧化涂层材料。本文利用电子束物理气相沉积(EB-PVD)方法制备了0~0.5at%Dy含量的β-NiAl涂层,研究了涂层的瞬态氧化行为。1200°C时,在0.05at%Dy掺杂的涂层中只观察到了稳态α-Al2O3相,而在0.5at%Dy掺杂的涂层中,1h氧化过程中,发生了θ-Al2O3到α-Al2O3的相变。1100°C时,在最初的15min所有涂层均发生了θ-α相变。0.05at%Dy掺杂的涂层在45min的时候相变已经完成,这比0.5at%Dy掺杂涂层要早得多。过量Dy的掺杂能够延缓θ-α相变。未掺杂和过量掺杂涂层在20h氧化之后仍存在针状相θ-Al2O3,而0.05at%Dy掺杂的涂层中则为经典的颗粒状α-Al2O3形貌。     

Stellar β-decay rates of iron isotopes and its implications in astrophysics

β-Decay and positron decay are believed to play a consequential role during the late phases of stellar evolution of a massive star culminating in a supernova explosion. The β-decay contributes in maintaining a respectable lepton-to-baryon ratio, Y_e, of the core prior to collapse which results in a larger shock energy to produce the explosion. The positron decay acts in the opposite direction and tends to decrease the ratio. The structure of the presupernova star is altered both by the changes in Y_e and the entropy of the core material. Recently the microscopic calculation of weak interaction mediated rates on key isotopes of iron was introduced using the proton–neutron quasiparticle random phase approximation (pn-QRPA) theory with improved model parameters. Here I discuss in detail the improved calculation of β^±-decay rates for iron isotopes (^54,55,56Fe) in stellar environment. The pn-QRPA theory allows a microscopic “state-by-state” calculation of stellar rates as explained later in text. Excited state Gamow–Teller distributions are much different from ground state and a microscopic calculation of decay rates from these excited states greatly increases the reliability of the total decay rate calculation specially during the late stages of stellar evolution. The reported decay rates are also compared with earlier calculations. The positron decay rates are in reasonable agreement with the large-scale shell model calculation. The main finding of this work includes that the stellar β-decay rates of ^54,55,56Fe are around 3–5 orders of magnitude smaller than previously assumed and hence irrelevant for the determination of the evolution of Y_e during the presupernova phase of massive stars. The current work discourages the inclusion of ^55,56Fe in the list of key stellar β-decay nuclei as suggested by former simulation results.