Half-quantum vortex and d-soliton in Sr$_2$RuO$_4$

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Quantum spin liquid emerging in 2D correlated Dirac fermions

Quantum spin liquid emerging in 2D correlated  Dirac fermions
At sufficiently low temperatures, condensed-matter systems tend to develop order. A notable exception to this behaviour is the case of quantum spin liquids, in which quantum fluctuations prevent a transition to an ordered state down to the lowest temperatures. There have now been tentative observations of such states in some two-dimensional organic compounds, yet quantum spin liquids remain elusive in microscopic two-dimensional models that are relevant to experiments. Here we show, by means of large-scale quantum Monte Carlo simulations of correlated fermions on a honeycomb lattice (a structure realized in, for example, graphene), that a quantum spin liquid emerges between the state described by massless Dirac fermions and an antiferromagnetically ordered Mott insulator. This unexpected quantum-disordered state is found to be a short-range resonating valence-bond liquid, akin to the one proposed for high-temperature superconductors: the possibility of unconventional superconductivity through doping therefore arises in our system. We foresee the experimental realization of this model system using ultra-cold atoms, or group IV elements arranged in honeycomb lattices.

SQUID(超导量子干涉仪)

SQUID(超导量子干涉仪)
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j jc sin(2 1
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Superconductiong flux transformers
Magnetometer
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Principles and applications of SQUID J.Clarke
SSM(扫描超导量子干涉显微镜)
Phys. Rev. Lett. 12, 159 - 160 (1964) R. C. Jaklevic et al.
• 60年代下半叶,制造简陋的dc SQUID开始为低温物理学家用于测量。 • 60年代末开始出现RF SQUID。 • 相当长的时间内,dc SQUID被摒弃,直到1974年出现灵敏性高于 RFSQUID的仪器。 • 1987年Koch和Nakane首先制造出了高温dc-SQUID。 Appl. Phys. Lett. 51(3). 20 July
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20 1015 Wb 因而对外加场的微小变化都很灵敏

量子力学英语词汇

量子力学英语词汇

1、microscopic world 微观世界2、macroscopic world 宏观世界3、quantum theory 量子[理]论4、quantum mechanics 量子力学5、wave mechanics 波动力学6、matrix mechanics 矩阵力学7、Planck constant 普朗克常数8、wave-particle duality 波粒二象性9、state 态10、state function 态函数11、state vector 态矢量12、superposition principle of state 态叠加原理13、orthogonal states 正交态14、antisymmetrical state 正交定理15、stationary state 对称态16、antisymmetrical state 反对称态17、stationary state 定态18、ground state 基态19、excited state 受激态20、binding state 束缚态21、unbound state 非束缚态22、degenerate state 简并态23、degenerate system 简并系24、non-deenerate state 非简并态25、non-degenerate system 非简并系26、de Broglie wave 德布罗意波27、wave function 波函数28、time-dependent wave function 含时波函数29、wave packet 波包30、probability 几率31、probability amplitude 几率幅32、probability density 几率密度33、quantum ensemble 量子系综34、wave equation 波动方程35、Schrodinger equation 薛定谔方程36、Potential well 势阱37、Potential barrien 势垒38、potential barrier penetration 势垒贯穿39、tunnel effect 隧道效应40、linear harmonic oscillator 线性谐振子41、zero proint energy 零点能42、central field 辏力场43、Coulomb field 库仑场44、δ-function δ-函数45、operator 算符46、commuting operators 对易算符47、anticommuting operators 反对易算符48、complex conjugate operator 复共轭算符49、Hermitian conjugate operator 厄米共轭算符50、Hermitian operator 厄米算符51、momentum operator 动量算符52、energy operator 能量算符53、Hamiltonian operator 哈密顿算符54、angular momentum operator 角动量算符55、spin operator 自旋算符56、eigen value 本征值57、secular equation 久期方程58、observable 可观察量59、orthogonality 正交性60、completeness 完全性61、closure property 封闭性62、normalization 归一化63、orthonormalized functions 正交归一化函数64、quantum number 量子数65、principal quantum number 主量子数66、radial quantum number 径向量子数67、angular quantum number 角量子数68、magnetic quantum number 磁量子数69、uncertainty relation 测不准关系70、principle of complementarity 并协原理71、quantum Poisson bracket 量子泊松括号72、representation 表象73、coordinate representation 坐标表象74、momentum representation 动量表象75、energy representation 能量表象76、Schrodinger representation 薛定谔表象77、Heisenberg representation 海森伯表象78、interaction representation 相互作用表象79、occupation number representation 粒子数表象80、Dirac symbol 狄拉克符号81、ket vector 右矢量82、bra vector 左矢量83、basis vector 基矢量84、basis ket 基右矢85、basis bra 基左矢86、orthogonal kets 正交右矢87、orthogonal bras 正交左矢88、symmetrical kets 对称右矢89、antisymmetrical kets 反对称右矢90、Hilbert space 希耳伯空间91、perturbation theory 微扰理论92、stationary perturbation theory 定态微扰论93、time-dependent perturbation theory 含时微扰论94、Wentzel-Kramers-Brillouin method W. K. B.近似法95、elastic scattering 弹性散射96、inelastic scattering 非弹性散射97、scattering cross-section 散射截面98、partial wave method 分波法99、Born approximation 玻恩近似法100、centre-of-mass coordinates 质心坐标系101、laboratory coordinates 实验室坐标系102、transition 跃迁103、dipole transition 偶极子跃迁104、selection rule 选择定则105、spin 自旋106、electron spin 电子自旋107、spin quantum number 自旋量子数108、spin wave function 自旋波函数109、coupling 耦合110、vector-coupling coefficient 矢量耦合系数111、many-particle system 多子体系112、exchange forece 交换力113、exchange energy 交换能114、Heitler-London approximation 海特勒-伦敦近似法115、Hartree-Fock equation 哈特里-福克方程116、self-consistent field 自洽场117、Thomas-Fermi equation 托马斯-费米方程118、second quantization 二次量子化119、identical particles 全同粒子120、Pauli matrices 泡利矩阵121、Pauli equation 泡利方程122、Pauli’s exclusion principle泡利不相容原理123、Relativistic wave equation 相对论性波动方程124、Klein-Gordon equation 克莱因-戈登方程125、Dirac equation 狄拉克方程126、Dirac hole theory 狄拉克空穴理论127、negative energy state 负能态128、negative probability 负几率129、microscopic causality 微观因果性本征矢量eigenvector本征态eigenstate本征值eigenvalue本征值方程eigenvalue equation本征子空间eigensubspace (可以理解为本征矢空间)变分法variatinial method标量scalar算符operator表象representation表象变换transformation of representation表象理论theory of representation波函数wave function波恩近似Born approximation玻色子boson费米子fermion不确定关系uncertainty relation狄拉克方程Dirac equation狄拉克记号Dirac symbol定态stationary state定态微扰法time-independent perturbation定态薛定谔方程time-independent Schro(此处上面有两点)dinger equation 动量表象momentum representation角动量表象angular mommentum representation占有数表象occupation number representation坐标(位置)表象position representation角动量算符angular mommentum operator角动量耦合coupling of angular mommentum对称性symmetry对易关系commutator厄米算符hermitian operator厄米多项式Hermite polynomial分量component光的发射emission of light光的吸收absorption of light受激发射excited emission自发发射spontaneous emission轨道角动量orbital angular momentum自旋角动量spin angular momentum轨道磁矩orbital magnetic moment归一化normalization哈密顿hamiltonion黑体辐射black body radiation康普顿散射Compton scattering基矢basis vector基态ground state基右矢basis ket ‘右矢’ket基左矢basis bra简并度degenerancy精细结构fine structure径向方程radial equation久期方程secular equation量子化quantization矩阵matrix模module模方square of module内积inner product逆算符inverse operator欧拉角Eular angles泡利矩阵Pauli matrix平均值expectation value (期望值)泡利不相容原理Pauli exclusion principle氢原子hydrogen atom球鞋函数spherical harmonics全同粒子identical particles塞曼效应Zeeman effect上升下降算符raising and lowering operator 消灭算符destruction operator产生算符creation operator矢量空间vector space守恒定律conservation law守恒量conservation quantity投影projection投影算符projection operator微扰法pertubation method希尔伯特空间Hilbert space线性算符linear operator线性无关linear independence谐振子harmonic oscillator选择定则selection rule幺正变换unitary transformation幺正算符unitary operator宇称parity跃迁transition运动方程equation of motion正交归一性orthonormalization正交性orthogonality转动rotation自旋磁矩spin magnetic monent(以上是量子力学中的主要英语词汇,有些未涉及到的可以自由组合。

第八届国际凝聚态理论与计算材料学会议

第八届国际凝聚态理论与计算材料学会议

大会将请专家对以下领域作专题性的特邀报告:
(1). 凝聚态物理的最新进展:
A. 自旋电子学
B. 纳米材料
C. 固体量子信息和计算
D. 玻色-爱因斯坦凝聚
E. 强关联电子系统
F. 高温超导
G. 量子霍尔效应
H. 磁学
I 表面和界面
J. 半导体物理
K. 低维凝聚态物理
L. 介观物理
M. 软凝聚态物质
N. 生物物理
structure Metallic Phases in Solid Germane (GeH4) under Pressure 锗烷在
压力下的金属相
11:45 -12:15
12:15 -13:00
午餐
张振宇 橡树岭国家实验室
柳百新
清华大学
林海青 香港中文大学 牛谦 美国德克萨斯大学
7 月 16 日
凝聚态理论专题邀请报告 I 主持人:谢心澄 地点:芙蓉厅
14:30 -14:55 14:55 -15:20 15:20 -15:45 15:45 -16:10 16:10 -16:35 16:35 -16:50
7 月 16 日
Manipulating Magnetization States of Nanostructures Two-spin decoherence in semiconductor quantum dots
稀磁半导体(Al,Cr)N 中的氮空位与高温铁磁性的第一原理研究
蒋青 刘邦贵
吉林大学 中科院物理所
15:20 -15:45 15:45 -16:10 16:10 -16:35
Theoretical and experimental studies of semiconductor dilute nitrides and devices

核能课件ppt英文

核能课件ppt英文
ห้องสมุดไป่ตู้
Advantages and Disadvantages of Nuclear Energy
Advantages
Nuclear energy is a sustainable source of energy that can provide a stable and related supply of electricity It does not emit greenhouse gases or air pollutants during operation, making it environmentally friendly Nuclear energy can also be used to produce medical isotopes and for other industrial applications
History of Nuclear Energy
The discovery of nuclear energy Began in the early 20th century with the discovery of radioactivity by Antoine Henri Becquerel in 1896
Nuclear Power Courseware PowerPoint English
• Introduction • Nuclear Physics • Nuclear Reactors • Safety and Security of Nuclear
Reactors • Future of Nuclear Energy
01 Introduction
Definition of Nuclear Energy

英文版原子物理课件

英文版原子物理课件
Shanxi University Atomic Physics
1.1 Introduction
The origins of atomic physics :quantum mechanics Bohr model of the H This introductory chapter surveys some of the early ideas: Spectrum of atomic H and Bohr Theory Einstein's treatment of interaction of atom with light the Zeeman effect Rutherford scattering And so on
Shanxi University Atomic Physics
1.2 Spectrum of atomic hydrogen_3
Wavenumbers may seem rather old-fashioned but they are very useful in atomic physics
the characteristic spectrum for atoms is composed of discrete lines that are the ‘fingerprint' of the element.
In 1888, the Swedish professor J. Rydberg found that the spectral lines in hydrogen obey the following mathematical formula:
Shanxi University Atomic Physics
Lyman series: n’ = 2; 3; 4; … n = 1. Balmer (n = 2), Paschen series: (n = 3), Brackett (n = 4) and Pfund (n = 5)

引力波观测原文PhysRevLett.116.061102

引力波观测原文PhysRevLett.116.061102

Observation of Gravitational Waves from a Binary Black Hole MergerB.P.Abbott et al.*(LIGO Scientific Collaboration and Virgo Collaboration)(Received21January2016;published11February2016)On September14,2015at09:50:45UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory simultaneously observed a transient gravitational-wave signal.The signal sweeps upwards in frequency from35to250Hz with a peak gravitational-wave strain of1.0×10−21.It matches the waveform predicted by general relativity for the inspiral and merger of a pair of black holes and the ringdown of the resulting single black hole.The signal was observed with a matched-filter signal-to-noise ratio of24and a false alarm rate estimated to be less than1event per203000years,equivalent to a significance greaterthan5.1σ.The source lies at a luminosity distance of410þ160−180Mpc corresponding to a redshift z¼0.09þ0.03−0.04.In the source frame,the initial black hole masses are36þ5−4M⊙and29þ4−4M⊙,and the final black hole mass is62þ4−4M⊙,with3.0þ0.5−0.5M⊙c2radiated in gravitational waves.All uncertainties define90%credible intervals.These observations demonstrate the existence of binary stellar-mass black hole systems.This is the first direct detection of gravitational waves and the first observation of a binary black hole merger.DOI:10.1103/PhysRevLett.116.061102I.INTRODUCTIONIn1916,the year after the final formulation of the field equations of general relativity,Albert Einstein predicted the existence of gravitational waves.He found that the linearized weak-field equations had wave solutions: transverse waves of spatial strain that travel at the speed of light,generated by time variations of the mass quadrupole moment of the source[1,2].Einstein understood that gravitational-wave amplitudes would be remarkably small;moreover,until the Chapel Hill conference in 1957there was significant debate about the physical reality of gravitational waves[3].Also in1916,Schwarzschild published a solution for the field equations[4]that was later understood to describe a black hole[5,6],and in1963Kerr generalized the solution to rotating black holes[7].Starting in the1970s theoretical work led to the understanding of black hole quasinormal modes[8–10],and in the1990s higher-order post-Newtonian calculations[11]preceded extensive analytical studies of relativistic two-body dynamics[12,13].These advances,together with numerical relativity breakthroughs in the past decade[14–16],have enabled modeling of binary black hole mergers and accurate predictions of their gravitational waveforms.While numerous black hole candidates have now been identified through electromag-netic observations[17–19],black hole mergers have not previously been observed.The discovery of the binary pulsar system PSR B1913þ16 by Hulse and Taylor[20]and subsequent observations of its energy loss by Taylor and Weisberg[21]demonstrated the existence of gravitational waves.This discovery, along with emerging astrophysical understanding[22], led to the recognition that direct observations of the amplitude and phase of gravitational waves would enable studies of additional relativistic systems and provide new tests of general relativity,especially in the dynamic strong-field regime.Experiments to detect gravitational waves began with Weber and his resonant mass detectors in the1960s[23], followed by an international network of cryogenic reso-nant detectors[24].Interferometric detectors were first suggested in the early1960s[25]and the1970s[26].A study of the noise and performance of such detectors[27], and further concepts to improve them[28],led to proposals for long-baseline broadband laser interferome-ters with the potential for significantly increased sensi-tivity[29–32].By the early2000s,a set of initial detectors was completed,including TAMA300in Japan,GEO600 in Germany,the Laser Interferometer Gravitational-Wave Observatory(LIGO)in the United States,and Virgo in binations of these detectors made joint obser-vations from2002through2011,setting upper limits on a variety of gravitational-wave sources while evolving into a global network.In2015,Advanced LIGO became the first of a significantly more sensitive network of advanced detectors to begin observations[33–36].A century after the fundamental predictions of Einstein and Schwarzschild,we report the first direct detection of gravitational waves and the first direct observation of a binary black hole system merging to form a single black hole.Our observations provide unique access to the*Full author list given at the end of the article.Published by the American Physical Society under the terms of the Creative Commons Attribution3.0License.Further distri-bution of this work must maintain attribution to the author(s)and the published article’s title,journal citation,and DOI.properties of space-time in the strong-field,high-velocity regime and confirm predictions of general relativity for the nonlinear dynamics of highly disturbed black holes.II.OBSERVATIONOn September14,2015at09:50:45UTC,the LIGO Hanford,W A,and Livingston,LA,observatories detected the coincident signal GW150914shown in Fig.1.The initial detection was made by low-latency searches for generic gravitational-wave transients[41]and was reported within three minutes of data acquisition[43].Subsequently, matched-filter analyses that use relativistic models of com-pact binary waveforms[44]recovered GW150914as the most significant event from each detector for the observa-tions reported here.Occurring within the10-msintersite FIG.1.The gravitational-wave event GW150914observed by the LIGO Hanford(H1,left column panels)and Livingston(L1,rightcolumn panels)detectors.Times are shown relative to September14,2015at09:50:45UTC.For visualization,all time series are filtered with a35–350Hz bandpass filter to suppress large fluctuations outside the detectors’most sensitive frequency band,and band-reject filters to remove the strong instrumental spectral lines seen in the Fig.3spectra.Top row,left:H1strain.Top row,right:L1strain.GW150914arrived first at L1and6.9þ0.5−0.4ms later at H1;for a visual comparison,the H1data are also shown,shifted in time by this amount and inverted(to account for the detectors’relative orientations).Second row:Gravitational-wave strain projected onto each detector in the35–350Hz band.Solid lines show a numerical relativity waveform for a system with parameters consistent with those recovered from GW150914[37,38]confirmed to99.9%by an independent calculation based on[15].Shaded areas show90%credible regions for two independent waveform reconstructions.One(dark gray)models the signal using binary black hole template waveforms [39].The other(light gray)does not use an astrophysical model,but instead calculates the strain signal as a linear combination of sine-Gaussian wavelets[40,41].These reconstructions have a94%overlap,as shown in[39].Third row:Residuals after subtracting the filtered numerical relativity waveform from the filtered detector time series.Bottom row:A time-frequency representation[42]of the strain data,showing the signal frequency increasing over time.propagation time,the events have a combined signal-to-noise ratio(SNR)of24[45].Only the LIGO detectors were observing at the time of GW150914.The Virgo detector was being upgraded, and GEO600,though not sufficiently sensitive to detect this event,was operating but not in observational mode.With only two detectors the source position is primarily determined by the relative arrival time and localized to an area of approximately600deg2(90% credible region)[39,46].The basic features of GW150914point to it being produced by the coalescence of two black holes—i.e., their orbital inspiral and merger,and subsequent final black hole ringdown.Over0.2s,the signal increases in frequency and amplitude in about8cycles from35to150Hz,where the amplitude reaches a maximum.The most plausible explanation for this evolution is the inspiral of two orbiting masses,m1and m2,due to gravitational-wave emission.At the lower frequencies,such evolution is characterized by the chirp mass[11]M¼ðm1m2Þ3=5121=5¼c3G596π−8=3f−11=3_f3=5;where f and_f are the observed frequency and its time derivative and G and c are the gravitational constant and speed of light.Estimating f and_f from the data in Fig.1, we obtain a chirp mass of M≃30M⊙,implying that the total mass M¼m1þm2is≳70M⊙in the detector frame. This bounds the sum of the Schwarzschild radii of thebinary components to2GM=c2≳210km.To reach an orbital frequency of75Hz(half the gravitational-wave frequency)the objects must have been very close and very compact;equal Newtonian point masses orbiting at this frequency would be only≃350km apart.A pair of neutron stars,while compact,would not have the required mass,while a black hole neutron star binary with the deduced chirp mass would have a very large total mass, and would thus merge at much lower frequency.This leaves black holes as the only known objects compact enough to reach an orbital frequency of75Hz without contact.Furthermore,the decay of the waveform after it peaks is consistent with the damped oscillations of a black hole relaxing to a final stationary Kerr configuration. Below,we present a general-relativistic analysis of GW150914;Fig.2shows the calculated waveform using the resulting source parameters.III.DETECTORSGravitational-wave astronomy exploits multiple,widely separated detectors to distinguish gravitational waves from local instrumental and environmental noise,to provide source sky localization,and to measure wave polarizations. The LIGO sites each operate a single Advanced LIGO detector[33],a modified Michelson interferometer(see Fig.3)that measures gravitational-wave strain as a differ-ence in length of its orthogonal arms.Each arm is formed by two mirrors,acting as test masses,separated by L x¼L y¼L¼4km.A passing gravitational wave effec-tively alters the arm lengths such that the measured difference isΔLðtÞ¼δL x−δL y¼hðtÞL,where h is the gravitational-wave strain amplitude projected onto the detector.This differential length variation alters the phase difference between the two light fields returning to the beam splitter,transmitting an optical signal proportional to the gravitational-wave strain to the output photodetector. To achieve sufficient sensitivity to measure gravitational waves,the detectors include several enhancements to the basic Michelson interferometer.First,each arm contains a resonant optical cavity,formed by its two test mass mirrors, that multiplies the effect of a gravitational wave on the light phase by a factor of300[48].Second,a partially trans-missive power-recycling mirror at the input provides addi-tional resonant buildup of the laser light in the interferometer as a whole[49,50]:20W of laser input is increased to700W incident on the beam splitter,which is further increased to 100kW circulating in each arm cavity.Third,a partially transmissive signal-recycling mirror at the outputoptimizes FIG. 2.Top:Estimated gravitational-wave strain amplitude from GW150914projected onto H1.This shows the full bandwidth of the waveforms,without the filtering used for Fig.1. The inset images show numerical relativity models of the black hole horizons as the black holes coalesce.Bottom:The Keplerian effective black hole separation in units of Schwarzschild radii (R S¼2GM=c2)and the effective relative velocity given by the post-Newtonian parameter v=c¼ðGMπf=c3Þ1=3,where f is the gravitational-wave frequency calculated with numerical relativity and M is the total mass(value from Table I).the gravitational-wave signal extraction by broadening the bandwidth of the arm cavities [51,52].The interferometer is illuminated with a 1064-nm wavelength Nd:Y AG laser,stabilized in amplitude,frequency,and beam geometry [53,54].The gravitational-wave signal is extracted at the output port using a homodyne readout [55].These interferometry techniques are designed to maxi-mize the conversion of strain to optical signal,thereby minimizing the impact of photon shot noise (the principal noise at high frequencies).High strain sensitivity also requires that the test masses have low displacement noise,which is achieved by isolating them from seismic noise (low frequencies)and designing them to have low thermal noise (intermediate frequencies).Each test mass is suspended as the final stage of a quadruple-pendulum system [56],supported by an active seismic isolation platform [57].These systems collectively provide more than 10orders of magnitude of isolation from ground motion for frequen-cies above 10Hz.Thermal noise is minimized by using low-mechanical-loss materials in the test masses and their suspensions:the test masses are 40-kg fused silica substrates with low-loss dielectric optical coatings [58,59],and are suspended with fused silica fibers from the stage above [60].To minimize additional noise sources,all components other than the laser source are mounted on vibration isolation stages in ultrahigh vacuum.To reduce optical phase fluctuations caused by Rayleigh scattering,the pressure in the 1.2-m diameter tubes containing the arm-cavity beams is maintained below 1μPa.Servo controls are used to hold the arm cavities on resonance [61]and maintain proper alignment of the optical components [62].The detector output is calibrated in strain by measuring its response to test mass motion induced by photon pressure from a modulated calibration laser beam [63].The calibration is established to an uncertainty (1σ)of less than 10%in amplitude and 10degrees in phase,and is continuously monitored with calibration laser excitations at selected frequencies.Two alternative methods are used to validate the absolute calibration,one referenced to the main laser wavelength and the other to a radio-frequencyoscillator(a)FIG.3.Simplified diagram of an Advanced LIGO detector (not to scale).A gravitational wave propagating orthogonally to the detector plane and linearly polarized parallel to the 4-km optical cavities will have the effect of lengthening one 4-km arm and shortening the other during one half-cycle of the wave;these length changes are reversed during the other half-cycle.The output photodetector records these differential cavity length variations.While a detector ’s directional response is maximal for this case,it is still significant for most other angles of incidence or polarizations (gravitational waves propagate freely through the Earth).Inset (a):Location and orientation of the LIGO detectors at Hanford,WA (H1)and Livingston,LA (L1).Inset (b):The instrument noise for each detector near the time of the signal detection;this is an amplitude spectral density,expressed in terms of equivalent gravitational-wave strain amplitude.The sensitivity is limited by photon shot noise at frequencies above 150Hz,and by a superposition of other noise sources at lower frequencies [47].Narrow-band features include calibration lines (33–38,330,and 1080Hz),vibrational modes of suspension fibers (500Hz and harmonics),and 60Hz electric power grid harmonics.[64].Additionally,the detector response to gravitational waves is tested by injecting simulated waveforms with the calibration laser.To monitor environmental disturbances and their influ-ence on the detectors,each observatory site is equipped with an array of sensors:seismometers,accelerometers, microphones,magnetometers,radio receivers,weather sensors,ac-power line monitors,and a cosmic-ray detector [65].Another∼105channels record the interferometer’s operating point and the state of the control systems.Data collection is synchronized to Global Positioning System (GPS)time to better than10μs[66].Timing accuracy is verified with an atomic clock and a secondary GPS receiver at each observatory site.In their most sensitive band,100–300Hz,the current LIGO detectors are3to5times more sensitive to strain than initial LIGO[67];at lower frequencies,the improvement is even greater,with more than ten times better sensitivity below60Hz.Because the detectors respond proportionally to gravitational-wave amplitude,at low redshift the volume of space to which they are sensitive increases as the cube of strain sensitivity.For binary black holes with masses similar to GW150914,the space-time volume surveyed by the observations reported here surpasses previous obser-vations by an order of magnitude[68].IV.DETECTOR VALIDATIONBoth detectors were in steady state operation for several hours around GW150914.All performance measures,in particular their average sensitivity and transient noise behavior,were typical of the full analysis period[69,70]. Exhaustive investigations of instrumental and environ-mental disturbances were performed,giving no evidence to suggest that GW150914could be an instrumental artifact [69].The detectors’susceptibility to environmental disturb-ances was quantified by measuring their response to spe-cially generated magnetic,radio-frequency,acoustic,and vibration excitations.These tests indicated that any external disturbance large enough to have caused the observed signal would have been clearly recorded by the array of environ-mental sensors.None of the environmental sensors recorded any disturbances that evolved in time and frequency like GW150914,and all environmental fluctuations during the second that contained GW150914were too small to account for more than6%of its strain amplitude.Special care was taken to search for long-range correlated disturbances that might produce nearly simultaneous signals at the two sites. No significant disturbances were found.The detector strain data exhibit non-Gaussian noise transients that arise from a variety of instrumental mecha-nisms.Many have distinct signatures,visible in auxiliary data channels that are not sensitive to gravitational waves; such instrumental transients are removed from our analyses [69].Any instrumental transients that remain in the data are accounted for in the estimated detector backgrounds described below.There is no evidence for instrumental transients that are temporally correlated between the two detectors.V.SEARCHESWe present the analysis of16days of coincident observations between the two LIGO detectors from September12to October20,2015.This is a subset of the data from Advanced LIGO’s first observational period that ended on January12,2016.GW150914is confidently detected by two different types of searches.One aims to recover signals from the coalescence of compact objects,using optimal matched filtering with waveforms predicted by general relativity. The other search targets a broad range of generic transient signals,with minimal assumptions about waveforms.These searches use independent methods,and their response to detector noise consists of different,uncorrelated,events. However,strong signals from binary black hole mergers are expected to be detected by both searches.Each search identifies candidate events that are detected at both observatories consistent with the intersite propa-gation time.Events are assigned a detection-statistic value that ranks their likelihood of being a gravitational-wave signal.The significance of a candidate event is determined by the search background—the rate at which detector noise produces events with a detection-statistic value equal to or higher than the candidate event.Estimating this back-ground is challenging for two reasons:the detector noise is nonstationary and non-Gaussian,so its properties must be empirically determined;and it is not possible to shield the detector from gravitational waves to directly measure a signal-free background.The specific procedure used to estimate the background is slightly different for the two searches,but both use a time-shift technique:the time stamps of one detector’s data are artificially shifted by an offset that is large compared to the intersite propagation time,and a new set of events is produced based on this time-shifted data set.For instrumental noise that is uncor-related between detectors this is an effective way to estimate the background.In this process a gravitational-wave signal in one detector may coincide with time-shifted noise transients in the other detector,thereby contributing to the background estimate.This leads to an overestimate of the noise background and therefore to a more conservative assessment of the significance of candidate events.The characteristics of non-Gaussian noise vary between different time-frequency regions.This means that the search backgrounds are not uniform across the space of signals being searched.To maximize sensitivity and provide a better estimate of event significance,the searches sort both their background estimates and their event candidates into differ-ent classes according to their time-frequency morphology. The significance of a candidate event is measured against the background of its class.To account for having searchedmultiple classes,this significance is decreased by a trials factor equal to the number of classes [71].A.Generic transient searchDesigned to operate without a specific waveform model,this search identifies coincident excess power in time-frequency representations of the detector strain data [43,72],for signal frequencies up to 1kHz and durations up to a few seconds.The search reconstructs signal waveforms consistent with a common gravitational-wave signal in both detectors using a multidetector maximum likelihood method.Each event is ranked according to the detection statistic ηc ¼ffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffi2E c =ð1þE n =E c Þp ,where E c is the dimensionless coherent signal energy obtained by cross-correlating the two reconstructed waveforms,and E n is the dimensionless residual noise energy after the reconstructed signal is subtracted from the data.The statistic ηc thus quantifies the SNR of the event and the consistency of the data between the two detectors.Based on their time-frequency morphology,the events are divided into three mutually exclusive search classes,as described in [41]:events with time-frequency morphology of known populations of noise transients (class C1),events with frequency that increases with time (class C3),and all remaining events (class C2).Detected with ηc ¼20.0,GW150914is the strongest event of the entire search.Consistent with its coalescence signal signature,it is found in the search class C3of events with increasing time-frequency evolution.Measured on a background equivalent to over 67400years of data and including a trials factor of 3to account for the search classes,its false alarm rate is lower than 1in 22500years.This corresponds to a probability <2×10−6of observing one or more noise events as strong as GW150914during the analysis time,equivalent to 4.6σ.The left panel of Fig.4shows the C3class results and background.The selection criteria that define the search class C3reduce the background by introducing a constraint on the signal morphology.In order to illustrate the significance of GW150914against a background of events with arbitrary shapes,we also show the results of a search that uses the same set of events as the one described above but without this constraint.Specifically,we use only two search classes:the C1class and the union of C2and C3classes (C 2þC 3).In this two-class search the GW150914event is found in the C 2þC 3class.The left panel of Fig.4shows the C 2þC 3class results and background.In the background of this class there are four events with ηc ≥32.1,yielding a false alarm rate for GW150914of 1in 8400years.This corresponds to a false alarm probability of 5×10−6equivalent to 4.4σ.FIG.4.Search results from the generic transient search (left)and the binary coalescence search (right).These histograms show the number of candidate events (orange markers)and the mean number of background events (black lines)in the search class where GW150914was found as a function of the search detection statistic and with a bin width of 0.2.The scales on the top give the significance of an event in Gaussian standard deviations based on the corresponding noise background.The significance of GW150914is greater than 5.1σand 4.6σfor the binary coalescence and the generic transient searches,respectively.Left:Along with the primary search (C3)we also show the results (blue markers)and background (green curve)for an alternative search that treats events independently of their frequency evolution (C 2þC 3).The classes C2and C3are defined in the text.Right:The tail in the black-line background of the binary coalescence search is due to random coincidences of GW150914in one detector with noise in the other detector.(This type of event is practically absent in the generic transient search background because they do not pass the time-frequency consistency requirements used in that search.)The purple curve is the background excluding those coincidences,which is used to assess the significance of the second strongest event.For robustness and validation,we also use other generic transient search algorithms[41].A different search[73]and a parameter estimation follow-up[74]detected GW150914 with consistent significance and signal parameters.B.Binary coalescence searchThis search targets gravitational-wave emission from binary systems with individual masses from1to99M⊙, total mass less than100M⊙,and dimensionless spins up to 0.99[44].To model systems with total mass larger than 4M⊙,we use the effective-one-body formalism[75],whichcombines results from the post-Newtonian approach [11,76]with results from black hole perturbation theory and numerical relativity.The waveform model[77,78] assumes that the spins of the merging objects are alignedwith the orbital angular momentum,but the resultingtemplates can,nonetheless,effectively recover systemswith misaligned spins in the parameter region ofGW150914[44].Approximately250000template wave-forms are used to cover this parameter space.The search calculates the matched-filter signal-to-noiseratioρðtÞfor each template in each detector and identifiesmaxima ofρðtÞwith respect to the time of arrival of the signal[79–81].For each maximum we calculate a chi-squared statisticχ2r to test whether the data in several differentfrequency bands are consistent with the matching template [82].Values ofχ2r near unity indicate that the signal is consistent with a coalescence.Ifχ2r is greater than unity,ρðtÞis reweighted asˆρ¼ρ=f½1þðχ2rÞ3 =2g1=6[83,84].The final step enforces coincidence between detectors by selectingevent pairs that occur within a15-ms window and come fromthe same template.The15-ms window is determined by the10-ms intersite propagation time plus5ms for uncertainty inarrival time of weak signals.We rank coincident events basedon the quadrature sumˆρc of theˆρfrom both detectors[45]. To produce background data for this search the SNR maxima of one detector are time shifted and a new set of coincident events is computed.Repeating this procedure ∼107times produces a noise background analysis time equivalent to608000years.To account for the search background noise varying acrossthe target signal space,candidate and background events aredivided into three search classes based on template length.The right panel of Fig.4shows the background for thesearch class of GW150914.The GW150914detection-statistic value ofˆρc¼23.6is larger than any background event,so only an upper bound can be placed on its false alarm rate.Across the three search classes this bound is1in 203000years.This translates to a false alarm probability <2×10−7,corresponding to5.1σ.A second,independent matched-filter analysis that uses adifferent method for estimating the significance of itsevents[85,86],also detected GW150914with identicalsignal parameters and consistent significance.When an event is confidently identified as a real gravitational-wave signal,as for GW150914,the back-ground used to determine the significance of other events is reestimated without the contribution of this event.This is the background distribution shown as a purple line in the right panel of Fig.4.Based on this,the second most significant event has a false alarm rate of1per2.3years and corresponding Poissonian false alarm probability of0.02. Waveform analysis of this event indicates that if it is astrophysical in origin it is also a binary black hole merger[44].VI.SOURCE DISCUSSIONThe matched-filter search is optimized for detecting signals,but it provides only approximate estimates of the source parameters.To refine them we use general relativity-based models[77,78,87,88],some of which include spin precession,and for each model perform a coherent Bayesian analysis to derive posterior distributions of the source parameters[89].The initial and final masses, final spin,distance,and redshift of the source are shown in Table I.The spin of the primary black hole is constrained to be<0.7(90%credible interval)indicating it is not maximally spinning,while the spin of the secondary is only weakly constrained.These source parameters are discussed in detail in[39].The parameter uncertainties include statistical errors and systematic errors from averaging the results of different waveform models.Using the fits to numerical simulations of binary black hole mergers in[92,93],we provide estimates of the mass and spin of the final black hole,the total energy radiated in gravitational waves,and the peak gravitational-wave luminosity[39].The estimated total energy radiated in gravitational waves is3.0þ0.5−0.5M⊙c2.The system reached apeak gravitational-wave luminosity of3.6þ0.5−0.4×1056erg=s,equivalent to200þ30−20M⊙c2=s.Several analyses have been performed to determine whether or not GW150914is consistent with a binary TABLE I.Source parameters for GW150914.We report median values with90%credible intervals that include statistical errors,and systematic errors from averaging the results of different waveform models.Masses are given in the source frame;to convert to the detector frame multiply by(1þz) [90].The source redshift assumes standard cosmology[91]. Primary black hole mass36þ5−4M⊙Secondary black hole mass29þ4−4M⊙Final black hole mass62þ4−4M⊙Final black hole spin0.67þ0.05−0.07 Luminosity distance410þ160−180MpcSource redshift z0.09þ0.03−0.04。

作者姓名:卢滇楠

作者姓名:卢滇楠

附件6作者姓名:卢滇楠论文题目:温敏型高分子辅助蛋白质体外折叠的实验和分子模拟研究作者简介:卢滇楠,男,1978年4月出生, 2000年9月师从清华大学化工系生物化工研究所刘铮教授,从事蛋白质体外折叠的分子模拟和实验研究,于2006年1月获博士学位。

博士论文成果以系列论文形式集中发表在相关研究领域的权威刊物上。

截至2007年发表与博士论文相关学术论文21篇,其中第一作者SCI论文9篇(有4篇IF>3),累计他引20次(SCI检索),EI收录论文14篇(含双收),国内专利1项。

中文摘要引言蛋白质体外折叠是重组蛋白质药物生产的关键技术,也是现代生物化工学科的前沿领域之一,大肠杆菌是重要的重组蛋白质宿主体系,截止2005年FDA批准的64种重组蛋白药物中有26种采用大肠杆菌作为宿主体系,目前正在研发中的4000多种蛋白质药物中有90%采用大肠杆菌为宿主表达体系。

但由于大肠杆菌表达系统缺乏后修饰体系使得其生产的目标蛋白质多以无生物学活性的聚集体——包涵体的形式存在,在后续生产过程中需要对其进行溶解,此时蛋白质呈无规伸展链状结构,然后通过调整溶液组成诱导蛋白质发生折叠形成具有预期生物学活性的高级结构,这个过程就称之为蛋白质折叠或者复性,由于该过程是在细胞外进行的,又称之为蛋白质体外折叠技术。

蛋白质体外折叠技术要解决的关键问题是避免蛋白质的错误折叠以及形成蛋白质聚集体。

目前本领域的研究以具体技术和产品折叠工艺居多,折叠过程研究方面则多依赖宏观的结构和性质分析如各类光谱学和生物活性测定等,在研究方法上存在折叠理论、分子模拟与实验研究结合不够的问题,这些都不利于折叠技术的发展和应用。

本研究以发展蛋白质新型体外折叠技术为目标,借鉴蛋白质体内折叠的分子伴侣机制,提出以智能高分子作为人工分子伴侣促进蛋白质折叠的新思路,即通过调控高分子与蛋白质分子的相互作用,1)诱导伸展态的变性蛋白质塌缩形成疏水核心以抑制蛋白质分子间疏水作用所导致的聚集,2)与折叠中间态形成多种可逆解离复合物,丰富蛋白质折叠的途径以提高折叠收率。

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a r X i v :c o n d -m a t /0005510v 1 [c o n d -m a t .s u p r -c o n ] 29 M a y 2000Half-quantum vortex and ˆd-soliton in Sr 2RuO 4Hae-Young Kee 1,Yong Baek Kim 2,and Kazumi Maki 31Department of Physics,University of California,Los Angeles,CA 900952Department of Physics,The Ohio State University,Columbus,OH 432103Department of Physics,University of Southern California,Los Angeles,CA 90089(February 1,2008)Assuming that the superconductivity in Sr 2RuO 4is described by a planar p-wave order parame-ter,we consider possible topological defects in Sr 2RuO 4.In particular,it is shown that both of the ˆd-soliton and half-quantum vortex can be created in the presence of the magnetic field parallel to the a -b plane.We discuss how one can detect the ˆd -soliton and half-quantum vortex experimentally.PACS numbers:74.20.-z,74.80.-g,74.25.-qIt has been suggested that the unconventional superconducting state of Sr 2RuO 4is described by the planar spin-triplet p -wave order parameter with broken time reversal symmetry in analogy to the 3He A-phase.As known fromthe example of superfluid 3He,one of the hallmarks of the triplet superconductivity is the presence of a manifold of topological defects.[1,2]Thus,we expect that the creation and detection of topological defects in Sr 2RuO 4(or spin-triplet superconductor)will provide further insights about the nature of the unconventional superconducting state of Sr 2RuO 4.In this sense,the study of the topological defects in the planar p -wave superconducting state with broken time reversal symmetry is of great interest.More specifically,it has been proposed [3,4]that the superconducting order parameter in this system is described by the planar p -wave form written as,∆αβ( k )= d ( k )·( σiσ2)αβ(1)withd ( k )=∆ˆd(ˆk 1±i ˆk 2),(2)where σµ(µ=1,2,3)are Pauli matrices and α,βrepresent spin ↑or ↓.Here ˆkj (j =1,2)represent the projection of the unit wave vector ˆk along two perpendicular directions ˆe 1and ˆe 2in two dimensional space.This order parameterdescribes the Cooper pair state with the zero spin projection on ˆd and with the unique projection of the pair orbitalangular momentum given by ˆl =ˆe 1׈e 2.In Sr 2RuO 4,due to the spin-orbit coupling,ˆd is forced to be parallel to ±ˆc and k is the quasi-particle momentum in the a -b plane.Indeed the spontaneous magnetization seen by muon spin relaxation experiment [5]and flat Knight shift seen by NMR [6]seem to be consistent with this picture.On the other hand,the origin of the spontaneous magnetization seen by muon spin relaxation experiment is somewhat mysterious since we do not expect such a magnetization in a homogeneous system.It is important to notice that the superconducting ground state described by the order parameter of Eq.2is doubly degenerate.We can designate these two ground states by the angular momentum l z =±1,where ˆl is parallel to the c -axis.Sigrist and Agterberg [7]proposed recently that there will be in general a domain wall between l z =1and l z =−1states,which we shall call ˆl -soliton [8]in analogy to the case of superfluid 3He-A.It is likely that such a soliton is magnetically active,so it may be an origin of the spontaneous magnetization seen in muon spin relaxation experiment [5].In particular,in a magnetic field H ||ˆc ,only one of these degenerate states is favored [9,10].Therefore,it is possible to control ˆl -solitons by a magnetic field parallel to the c -axis.[7]They also proposed that these ˆl -solitonswould provide very efficient barriers for the vortex motion and this effect is possibly related to the pinning of vortices observed in Sr 2RuO 4below T =30mK [11].However,in this experiment the magnetic field is applied in a directionperpendicular to the c -axis.As we will see later,so-called ˆd -solitons appear to be more appropriate than ˆl -solitons inthis configuration.Also,for the ˆl -solitons,it is rather difficult to estimate the soliton energy and to make a further quantitative prediction.The purpose of this paper is to propose an alternative model for the appearance of the spontaneous magnetizationand the mechanism of the pinning of vortices;ˆd-soliton and half-quantum vortex.The ˆd -soliton is a domain wall between ˆd ˆc and ˆd −ˆc as in superfluid 3He-A.We believe that ˆd is parallel and antiparallel to ˆc ,because they areforced to be parallel to the angular momentum ˆl (or −ˆl )due to the spin-orbit coupling characterized by an energyscale Ωd [12].Therefore,if we use Ωd as a parameter,we can calculate the energy and shape of the ˆd-soliton provided that Ωd ≪∆(T ),where ∆(T )is the superconducting gap.Unfortunately we do not know the precise value of Ωd ,but it may be about14πλ)2ln(λmc2ρs(T).When the magneticfield is parallel to the a-axis,in theanisotropic system like Sr2RuO4,λandξshould be reinterpreted asλ=√ξbξc.Hereλb,c andξb,care the magnetic penetration depth and coherence length in the b and c directions respectively.ˆd-soliton and a pair of half-quantum vorticesThere exists huge anisotropy in the in-plane and out-of-plane transport properties in Sr2RuO4.Thus Sr2RuO4may be regarded as an effectively two dimensional system.The large anisotropy or the effective two-dimensionality of the system forces the angular momentum of the Cooper pair to be parallel or antiparallel to the c-axis.In the p-wave superconducting state described by the order parameter described by Eq.1and Eq.2,theˆd vector is oriented along ±ˆl in the presence of the spin-orbit coupling.Here we consider the case that the angular momentumˆl is uniform in the entire system.We can assume,without loss of generality,thatˆl ˆc.We are interested in the deformation oftheˆd configuration from the uniform case;for example,ˆd ˆc.Any deviation from the uniform state would cost the energy associated with the spin-orbit coupling characterized by an energy scaleΩd[12].However,we will show that the so-calledˆd-soliton(a particular form of theˆd configuration)with a pair of half-quantum vortices can have lower energy than the conventional single vortex.Thus it is easier to excite a pair of half-quantum vortices with aˆd-soliton compared to single conventional vortex.In particular,a magneticfield parallel to the a-b plane generates very likely pairs of half-quantum vortices rather than usual vortices when the formers are stable.We consider theˆd-soliton that is a topological planar defect in theˆd configuration.The orientation ofˆd changes by πacross the planar defect whileˆd vectors at far distances are still along the c-axis.Typical configurations ofˆd-soliton in the y-z plane can be found in Fig.1and Fig.2which we will explain later.We take y and z as the coordinates along b-axis and c-axis respectively.Now let us attach a pair of half-quantum vortices to the end points of theˆd-soliton of length R in y-z plane.In the case of an isolated half-quantum vortex,we have e iπ=−1factor in the order parameter due to phase winding around the half-quantum vortex.Therefore,an isolated half-quantum vortex cannot occur.On the other hand,if the half-quantum vortex is attached to the end points of theˆd-soliton,the disgyration inˆd at the same point compensates the phaseπso that there is no net change in the overall phase of the order parameter.In order to show that a pair of half-quantum vortices with theˆd-soliton is a lower energy excitation compared to single conventional vortex,we have to compare the free energies of two cases.The free energy required to create the ˆd-soliton is obtained fromf d=1whereψ(y,z )=1y−arctanz −R/22arctany +R/2z,(7)where two half-quantum vortices are located at (y,z )=(R/2,0)and (−R/2,0).The configuration of the ˆdvector using the above ψis shown in Fig.2.One can easily see that the free energies,f d ,associated with two possible ˆdconfigurations are the same.The total free energy of the ˆd-soliton and a pair of half-quantum vortices is given by f pair =12χN C 2(πK lnλρsp=1+1/3F 11+1/3F 1(1−ρ0s ),(9)where ρs and ρsp are the superfluid density and the spin superfluid density respectively.F 1and F a1are the LandauParametersandρ0s (≡1−Y (T )and Y (T )is the Yosida function)is the superfluid density without the Fermi liquid correction.[1]Notice that K (T c )=1at T =T c and K (0)=1+1/3F 14dydz R 2ξ,I 2=12ξd2ln4ξdln4ξd eR 0>0.(11)Here we have assumed that theξd>√m ,is about4,which means that F1∼9.Therefore,K>1inthe superconducting state,as one can see from Eq.9.Thus this condition is always satisfied below T c.However,the existence of the solution for R0depends on the value of K.Wefind that the solution exists only if1<K≤1.5.For example,for K=1.5,ξd/R=0.85.Since the parameter K depends on temperature as shown in Fig.3,wefind that a pair of half-quantum vortices withˆd-soliton exist only for0.78≤T/T c<1.Now the free energy of a pair of half-quantum vortices and theˆd-soltion at the optimal R0can be obtained asf pair=1ξ+(K−1)2(K−1)ξ2d+K−1√2πχN C2[lnλ2ln2(K−1)ξ2d2].(13)If f v−f pair>0for some values of K>1,a pair of half-quantum vortices are more stable than the conventional single vortex.This condition can be rewritten asλλ K−1>e(K−1)/2Λ(K−1)/2λ>10−11andξd(λbλc)/(ξbξc)=12.186whichis appropriate for Sr2RuO4.One can also see that the stability of a pair of half-quantum vortices with theˆd-soliton is determined by the value of K which depends on temperatures as shown in Fig.3.Now let us discuss the relation betweenˆl-andˆd-solitons.It is difficult to estimate the energy ofˆl-soliton in terms of the texture free energy given by Eq.4.However,it is likely thatˆl-soliton costs much more energy because,if it exists,the order parameter given by Eq.2should vanish inside theˆl-soliton.Therefore,if there is a natural passage for conversion ofˆl-solitons toˆd-solitons,most ofˆl-solitons will be converted intoˆd-solitons.In summary,assumming that the superconducting state of Sr2RuO4is characterized by the spin-triplet order parameter with broken time reversal symmetry,we investigated the existence of half-quantum vortices and associated topological defect;ˆd-soliton.We showed that a pair of half-quantum vortices attached to aˆd-soliton can be created in the presence of the magneticfield parallel to the a-b plane.It was found that a pair of half-quantum vortices with aˆd-soliton is more stable than the conventional single vortex for certain temperatures below T c.As in superfluid 3He-A,the presence ofˆd-soliton may be detected as the deficit in the intensity of electron spin resonance signal at ω=Ωd.[8]There should be a clear electron spin resonance signature due to the half-quamtum vortices.Detection of the half-quantum vortices by scanning tunneling microscopy(STM)would also provide a convincing evidence for the spin-triplet pairing state with time reversal symmetry breaking.We thank Manfred Sigrist and Ying Liu for helpful discussions.The work of H.-Y.Kee was conducted under the auspices of the Department of Energy,supported(in part)by funds provided by the University of California for the conduct of discretionary research by Los Alamos National Laboratory.This work was also supported by NSF CAREER award grant No.DMR-9983783(Y.B.K.)and Alfred P.Sloan Foundation(Y.B.K.).[2]G.E.Volovik,Exotic Properties of Superfluid Helium3(World Scientific Pub.Co.,Singapore,1991).[3]T.M.Rive and M.Sigrist,J.Phys.Cond.Matter,7,L643(1995).[4]M.Sigrist et al,Physica C317-318,134(1999).[5]G.M.Luke et al,Nature394,558(1998).[6]K.Ishida et al,Nature396,658(1998).[7]M.Sigrist and D.F.Agterberg,Prog.Theor.Phys.102,965(1999).[8]K.Maki,Solitons ed.S.E.Trullinger,V.E.Zakharov and V.L.Pokrovskii(North-Holland,Amsterdam,1986).[9]D.F.Agterberg,Phys.Rev.Lett80,5184(1998);Phys.Rev.B58,14484(1998)[10]G.F.Wang and K.Maki,Europhys.Lett45,71(1999)[11]A.C.Mota,G.Juri,P.Visami,A.Pollini,T.Teruzzi,and K.Aupke,Physica C185-189,343(1999)[12]H.Y.Kee,Y.B.Kim,and K.Maki,Phys.Rev.B61,3584(2000).[13]M.M.Salomaa and G.E.Volovik,Phys.Rev.Lett,55,1184(1985).[14]K.Maki,Phys.Rev.Lett.56,1312(1986).[15]J.R.Kirtley et al,Phys.Rev.Lett.81,2140(1998);K.A.Moler et al,Science279,1193(1998).FIG.1.The spatial configuration of d-vector in the b-c plane given by Eq.6.The thick line denotes the domain wall with the length of R, which is parallel to the c axis.FIG.2.The spatial configuration of d-vector in the b-c plane given by Eq.7.The thick line denotes the domain wall with the length of R, which is parallel to the b axis.K1.61.41.210.80.60.70.750.80.850.90.95t FIG.3.The parameter K as a function of the reduced temperature t=T/T c.。

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