Ni50.5Mn24.5G25单晶的预马氏体相变特性

通过交流磁化率、电阻、有无磁场下的预相变应变、磁致伸缩和磁化强度测量，系统研究了近正配分比Ni505Mn245Ga25单晶的预马氏体相变特性.在自由样品中观察到预马氏体相变应变.在预相变点，沿[010]方向施加大小约为80kA/m的磁场，在晶体母相的[001]方向上获得了高达505ppm的磁致伸缩，该值是相同条件下晶体母相磁致伸缩量的5倍多.同时，报道了不同方向磁场对预相变应变干预的结果.利用软模凝结的概念和依据单晶生长的特点，分析了预相变应变产生的机理.而磁场干预预相变应变的机理是磁场增大的磁弹耦合导致的晶格形变与材料内禀形变的竞争.利用磁性测量结果证实和解释了预相变过程中[001]和[010]轴方向间进一步增大的各向异性.进而对磁场沿[001]和[010]两个晶体学方向所导致的应变特性的差别，包括最大磁致伸缩、饱和预相变应变、饱和场等，进行了分析和讨论. 关键词： 预马氏体相变 应变 磁致伸缩 磁弹耦合     

单晶Ni52Mn24Ga24中马氏体变体择优取向的物理表征

利用各种实验手段对M52Mn24Ga24单晶中马氏体变体的择优取向进行了表征.针对金相观察、磁场干预的相变应变、磁感生应变等实验结果,分析了马氏体相变过程变体自发择优取向和磁诱导择优取向的机理.根据不同方向磁场干预相变应变的结果,计算了Ni52Mn24Ga24单晶中等效取向内应力的大小约为2.45 MPa.从变体择优取向造成的有效弹性和磁畴分布两个方面,对单晶样品在[001]和[010]两个等价的晶体学方向上磁感生应变特性的差别,包括最大应变值、饱和场、滞后效应和起始磁场数值的参数,进行了分析和讨论.     

Fe81Ga19合金晶体生长取向与磁致伸缩性能

通过区熔定向凝固法,生长出[001]易磁化方向与晶体轴向之间存在不同取向差的Fe₈₁Ga₁₉合金单晶体和Fe₈₁Ga₁₉合金多晶体.极图测试结果显示,Fe₈₁Ga₁₉合金单晶体的[001]方向与轴向取向差分别为12°,5°和3°.采用电阻应变片法测定相应磁致伸缩应变,与外加磁场方向平行的轴向磁致伸缩应变分别为254×10^-6,271×10^{-6< 关键词： 磁致伸缩 81Ga₁₉合金')" href="#">Fe₈₁Ga₁₉合金 晶体取向}     

Ni53.2Mn22.6Ga24.2单晶的两步热弹性马氏体相变及其应力应变特性

对具有两步完全热弹性的Ni_53.2Mn_22.6Ga_24.2单晶的物性采用多种测量手段进行了表征,特别研究了不同温度下的应力-应变特性.研究表明,热诱发的中间马氏体相变应变远大于马氏体相变应变.在较低的形变温度下,沿单晶母相［001］方向的压应力诱发的是两步马氏体相变,材料表现出赝弹性;在较高的形变温度下,只能观察到一步马氏体相变,材料展现出完全超弹性特性.此外,利用热力学理论分别计算了诱发马氏体相变和中间马氏体相变的临界应力与形变温度的关系,与实验测量得到的结果相符. 关键词： 马氏体相变 形状记忆效应 应变 超弹性     

压应力对Fe0.81 Ga0.19单晶磁化和磁致伸缩的影响

研究了Fe_0.81Ga_0.19合金单晶沿[100]方向的磁机械效应和磁致伸缩效应.基于Stoner-Wohlfarth模型,通过数值计算获得了在压应力和外磁场联合作用下磁化强度的方向余弦.研究表明,随着压应力的增加,退磁态下合金中的磁各向异性会由三轴各向异性向双轴各向异性转变.这使得合金中 90° 畴的体积分数增加,导致磁致伸缩效应增大. 关键词： FeGa合金 磁机械效应 巨磁致伸缩效应     

哈斯勒合金Ni-Mn-Ga的马氏体相变和磁增强双向形状记忆效应

通过研究铁磁性金属间化合物Ni_2+xMn_1-xGa(x=-0.1,0,0.08,0.13,0.18,0.2)和Ni_2-xMn_1+x/2Ga_1+x/2(x=-0.1,0,0.04,0.06,0.1)两个系列多晶样品的交流磁化率随温度的变化行为,得到了化合物在不同组分下的马氏体相变温度TM和居里温度T_C.发现随着Ni成分的增加,前者的马氏体相变温度T_m增加,而居里温度T_C降低,后者的马氏体相变温度T_m和居里温度T_C均是先增大后减小.报道了T_m在室温附近的单晶样品Ni₅₂Mn₂₄Ga₂₄的磁场增强双向形状记忆效应.发现伴随着马氏体相变,样品在[001]方向可产生1.2%的收缩.如果在该方向施加1.2T的偏磁场可以使该应变值增大到4.0%.而垂直于[001]方向施加1.2T的偏磁场时,在[001]方向产生1.6%的膨胀.阐明了产生大应变的原因并非相界移动,而是单晶的杂散内应力小和外加磁场通过孪晶界移动使马氏体变体重组的共同结果. 关键词： 形状记忆效应 马氏体相变 2MnGa')" href="#">Ni₂MnGa     

热磁预处理对Ni-Mn-Ga单晶磁学和力学性能的影响

研究了预先热磁处理对Ni_503Mn_287Ga₂₁单晶的磁学和力学性能的影响.首先将样品加热到居里温度之上让其冷却,冷却方式分为两种：一种是施加一定大小的磁场从高于居里温度冷却至室温,另一种是在样品经历顺磁-铁磁相变后但还未发生奥氏体-马氏体相变前施加相同大小和方向的磁场并冷却至室温.室温时的拉伸-压缩实验结果表明单晶样品在经历前一种处理后,其可逆应变、磁化强度的变化 （ΔM）比后一种处理的相应值要小很多.在后一种热磁处理的样品中,顺磁-铁磁相变发生后形成了自发磁畴,但这种磁畴不具有择优取向.在顺磁-铁磁相变结束后施加磁场,容易导致择优的马氏体准单畴出现,从而表现出大的可逆应变和ΔM.但对于前者,我们认为样品从居里温度降到室温过程中,其中的磁畴在相同的磁场作用下获得择优生长,形成大磁畴,导致磁诱导的强各向异性.这种择优取向的大磁畴在随后马氏体相变期间影响着马氏体的自发排列方式,不利于马氏体准单畴的出现,结果导致较小的可逆应变和ΔM. 关键词： 磁和力学锻炼 Ni-Mn-Ga单晶 铁磁和马氏体相变     

铁单质薄膜磁致伸缩行为与磁矩演化研究

磁致伸缩材料在传感器、位移器件等领域应用前景广阔,对此类材料的制备与实验已成为研究热点,但使用分子动力学方法模拟其磁致伸缩过程中内部磁矩的演化仍缺乏相关研究.本研究以磁致伸缩材料铁单质为研究对象,采用分子动力学方法建立单畴铁单质磁致伸缩模型.分析了铁单质薄膜磁致伸缩行为随初始磁矩的变化,以及在磁场作用下微观原子磁矩的变化与宏观磁致伸缩之间的关系.结果表明:模型磁化构型的演化与磁致伸缩行为有着密切联系,随着外加磁场强度增大,原子磁矩与外加磁场方向相同的区域面积逐渐增大,宏观表现为模型的磁致伸缩随磁场强度增大而伸长,并最终达到饱和,而边界处的原子磁矩是模型是否达到饱和磁致伸缩的关键.     

Ni52Mn24Ga24单晶中取向内应力的热动力学计算

测量了Ni52Mn24Ga24单晶样品在磁场加载和未加载情况下马氏体相变时的相变应变.分析结果表明:用提拉法生长单晶时在晶体内部引入了单一取向的内应力,该取向内应力可诱导马氏体变体择优取向,从而导致马氏体相变时产生大的相变应变.从理论上计算了该内应力的大小.另外,对样品在马氏体态单纯磁诱导应变的热动力学研究,表明取向内应力在马氏体态依然存在.     

Ni52Mn24Ga24单晶中取向内应力的热动力学计算

测量了Ni₅₂Mn₂₄Ga₂₄单晶样品在磁场加载和未加载情 况下马氏体相变时的相变应变.分析结果表明：用提拉法生长单晶时在晶体内部引入了单一取向的内应力，该取向内应力可诱导马氏体变体择优取向，从而导致马氏体相变时产生大的相变应变.从理论上计算了该内应力的大小.另外，对样品在马氏体态单纯磁诱导应变的热动力学研究，表明取向内应力在马氏体态依然存在. 关键词： 马氏体相变 磁感生应变 内应力     

关于"太阳在银河系中所受引力与到银心距离r的关系"的讨论

讨论了银道面内的引力场强分布和太阳在银河系中所受引力与到银心距离r的关系，指出引力场强g并不是与r的平方成反比，这是由于银河系的大小和形状不能忽略造成的．强调了万有引力定律的适用条件．     

On the predictability of the positions of the convergence zones in the ocean

The disagreement between the experimental and calculated positions of the first convergence zone are known from many publications. The most probable cause for such a disagreement, namely, the incorrect specification of the input data for the calculations, is considered. The lack of simultaneity between the hydrological surveys of the region and the acoustic experiments is emphasized. The experimental data obtained by the author in five ocean regions are presented. These data characterize the diurnal variability of the distance from the source to the nearest boundary of the convergence zone. The relations proposed by different researchers for calculating the sound speed from the temperature, salinity, and hydrostatic pressure are analyzed. It is shown that these relations lead to a substantial difference in the estimated depth dependence of the hydrostatic gradient of the sound speed. The position of the first convergence zone is calculated for the propagation conditions determined by vertical temperature and salinity profiles with the subsequent recalculation of these profiles into sound speed profiles by using eight different formulas known from the literature. It is shown that different formulas lead to different values of the distance to the first zone; this difference is substantially greater than that between the calculations and experiment. The necessity of improving the recalculation relations in view of the experimental data on sound propagation in natural oceanic waveguides, including the data on the actual positions of the convergence zones, is emphasized.     

On the calculation of the bremsstrahlung in the region of the plasma frequency

On the basis of the classical theory of radiation produced in incomplete Coulomb interaction, a formula is derived for the coefficient of the bremsstrahlung of fully ionized plasma. In the region of rectilinear approximation a comparison is made with the results of the quantum formula derived from the Born approximation. Furthermore, the influence of dispersion upon the emission coefficient is taken into account; some relations for the region of dispersion are given.     

Dependence of the Intensity of the Spectral Lines and the Composition of the Sample and the Plasma Parameters of the Unipolar Arc

The investigation was made of the dependence of the intensity of Tl, Ga, Mo, Mg, Mn, Sn, Bi, Ni, Zn, Pt and Au spectral lines and the plasma parameters (temperature T, electron concentration n_e, degree of 6 ionnization α) from concentration of lithium additive.     

Extracting the wavefunction of the LSP at the LHC

We consider associated production of squarks and gluinos with the lightest supersymmetric particle (LSP), or states nearly degenerate in mass with it. Though sub-dominant to pair production of color SU(3)-charged superpartners, these processes are directly sensitive to the wavefunction composition of the lightest neutralinos. Exploiting event-shape variables - including some introduced here for the first time - we are able to identify the composition of the LSP by selecting events involving a single high-pT jet recoiling against missing transverse energy. We illustrate the proposed technique on a set of benchmark cases and propose methods for applying these results in more realistic experimental environments.     

Set the controls for the heart of the Sun

In this paper we describe experiments conducted with high-power lasers that are attempting to replicate, for a very short time and in miniature, conditions found in the Sun. Experiments to date have reached conditions in the outer part of the Sun. To reach the Sun's centre requires compression of material to very much greater than solid density and heating to over ten million degrees. To achieve this, a new class of experiments and a new generation of high-power lasers are required.     

On the Question of the Source of the Apokamp

Technical Physics - The object of this work is the apokamp—a new type of plasma jet, which is formed from a bright offshoot emerging at the bending point of a channel of a high-voltage...