论文标题
装饰的自旋链系统中的复杂磁性订单RB $ _2 $ MN $ _3 $（MOO $ _4 $）$ _ 3 $（OH）$ _ 2 $
Complex Magnetic Order in a Decorated Spin Chain System Rb$_2$Mn$_3$(MoO$_4$)$_3$(OH)$_2$
论文作者
论文摘要
RB $ _2 $ _2 $ _3 $（MOO $ _4 $）$ _ 3 $ _ 3 $（oh）$ _ 2 $（太空群$ PNMA $）的宏观磁性和显微镜磁性结构通过磁化，热容量和单晶中性衍射测量测量来研究。该化合物的晶体结构包含债券的[mn $ _3 $ o $ _ {11} $] $^{\ infty} $链条沿$ b $轴沿$ b $轴形成，由等速膜三角形组成，占据了两个固定网站上两个非晶格（Mn1 sere of Base and base and base and base and base and base and base and base and base and base and base and base and base and base and Mn2 site in core and base and base and Mn2。这些链仅通过非磁性氧彼此薄弱。鱿鱼磁力测定法和中子衍射实验均显示了两个连续的磁过渡随温度的函数。在冷却时，它从顺磁相转变为4.5 〜k以下的不一致相，磁波向量接近$ {\ bf k} _ {1} =（0，〜0.46，〜0）$。 $ {\ bf k} _ {2} =（0，〜0，〜0）$出现另一个相称的抗磁性有序分量，形成了3.5〜K以下的复杂磁性结构，具有两个不同恒星的两个不同的传播向量。在进一步冷却时，不相称的波形经历了低于2.3〜k的锁定过渡。实验结果表明，磁性超空间组为$ pnma.1'（0b0）s0ss $，用于单个-U {\ bf k} $不兑换阶段，是2- $ {\ bf k} $磁性阶段的2- $ pn'ma（0b0）00s $。我们提出了一个简化的磁性结构模型，考虑了主要有序的贡献，其中相应的$ {\ bf k} _ {2} $定义了mn1磁矩的$ c $ - 轴成分的顺序，而不遵守$ {\ bf k} _ {1} $ comments $ n of the $ ab ab ab ab ab ab ab ab ab ab ab ab。椭圆形的循环
Macroscopic magnetic properties and microscopic magnetic structure of Rb$_2$Mn$_3$(MoO$_4$)$_3$(OH)$_2$ (space group $Pnma$) are investigated by magnetization, heat capacity and single-crystal neutron diffraction measurements. The compound's crystal structure contains bond-alternating [Mn$_3$O$_{11}$]$^{\infty}$ chains along the $b$-axis, formed by isosceles triangles of Mn ions occupying two crystallographically nonequivalent sites (Mn1 site on the base and Mn2 site on the vertex). These chains are only weakly linked to each other by nonmagnetic oxyanions. Both SQUID magnetometry and neutron diffraction experiments show two successive magnetic transitions as a function of temperature. On cooling, it transitions from a paramagnetic phase into an incommensurate phase below 4.5~K with a magnetic wavevector near ${\bf k}_{1} = (0,~0.46,~0)$. An additional commensurate antiferromagnetically ordered component arises with ${\bf k}_{2} = (0,~0,~0)$, forming a complex magnetic structure below 3.5~K with two different propagation vectors of different stars. On further cooling, the incommensurate wavevector undergoes a lock-in transition below 2.3~K. The experimental results suggest that the magnetic superspace group is $Pnma.1'(0b0)s0ss$ for the single-${\bf k}$ incommensurate phase and is $Pn'ma(0b0)00s$ for the 2-${\bf k}$ magnetic phase. We propose a simplified magnetic structure model taking into account the major ordered contributions, where the commensurate ${\bf k}_{2}$ defines the ordering of the $c$-axis component of Mn1 magnetic moment, while the incommensurate ${\bf k}_{1}$ describes the ordering of the $ab$-plane components of both Mn1 and Mn2 moments into elliptical cycloids
