arXiv subjects

Aiichi Iwazaki

Publications and source records attributed to Aiichi Iwazaki.

At least 19 recordsLinked to original sources

arXiv2026

Power of Axion Microwave Absorbed by Quantum Hall State in Haloscope

We propose a new method for detecting dark matter axions using a resonant cavity coupled to a two-dimensional electron system in the quantum Hall regime. When the cavity is tuned to the axion frequency, the axion-induced electromagnetic field is resonantly enhanced and drives a transverse Hall current in the quantum Hall system. On a quantum Hall plateau, the longitudinal dissipative response is strongly suppressed, $\mathrm{Re}(σ_{xx})\simeq0$, while the Hall conductivity remains finite and quantized, $\mathrm{Re}(σ_{xy})=νe^2/h$. Consequently, the Hall current is essentially nondissipative and introduces only a small additional loss to the cavity, allowing the loaded quality factor to approach the unloaded value, $Q_L\simeq Q_0$. The resulting Hall current is therefore enhanced by the large cavity quality factor, $I_H\propto\mathrm{Re}(σ_{xy})E\propto Q_L$. For a 2D electron density of $3\times10^{11}\mathrm{cm}^{-2}$, filling factor $ν=1/3$, and $Q_L\sim10^5$--$10^6$, we estimate a Hall current of order $I_H\sim10^{-13}$--$10^{-12}\mathrm{A}$ for an axion mass $m_a\sim10^{-5}\mathrm{eV}$ and a magnetic field of order $1.5\times 10^5\mathrm{G}$. The axion mass can be inferred from the resonant frequency, $m_a=2πν_a$. Under the assumed thermal-noise level and readout conditions, the estimated Hall-current signal can achieve a signal-to-noise ratio greater than unity for an observation time of order $100\mathrm{s}$. The proposed method exploits the unique combination of a finite, quantized transverse response and a strongly suppressed longitudinal dissipation in the quantum Hall state, providing an alternative to conventional metallic-antenna detection in axion haloscopes.

hep-ph↗

arXiv2026

Detection of Dark Matter Axions via the Quantum Hall Effect in a Resonant Cavity

We propose a new method for detecting dark matter axions using a resonant cavity coupled with a quantum Hall system. When a small sample exhibiting quantum Hall effect is placed inside the cavity and the cavity is tuned to resonance, two-dimensional electrons absorb the amplified radiation, leading to a rise in the sample's temperature. By monitoring this temperature increase, the mass $m_a$ of the axion can be inferred. As an example, consider a GaAs sample with surface area $S=0.01\text{cm}^2$ and small thickness $d = 1\,μ\mathrm{m}$ and its heat capacity $C_s$ at temperature $T = 20\,\mathrm{mK}$. Because the energy flux of the incoming radiation is $P_{ra}\sim 5.9\times10^{-20}\text{W}\,(S/0.01\text{cm}^2)\,(g_{aγγ}/10^{-14}\text{GeV}^{-1})^2\,(σ/10^7\text{eV})\, (10^{-5}\mbox{eV}/m_a)^3(B/15\text{T})^2 (ρ_d/0.3\rm GeV cm^{-3})$ at the resonance with electrical conductivity $σ$ of the cavity wall, the temperature increase is $P_{ra}t_{ob}/C_s \simeq 4.8\mbox{mK}(t_{ob}/1\text{s})(g_{aγγ}/10^{-14}\text{GeV}^{-1})^2(20\mbox{mK}/T)^3 (10^{-5}\mbox{eV}/m_a)^3(σ/10^7\text{eV})(1μ\text{m}/d) (B/15\text{T})^2$ with $1\text{T}=10^4$ Gauss where $t_{ob}=1$s is the observation time. It must be smaller than a time constant $τ>1$s associated with the heat dissipation into thermal bath. Such a large time constant can be realized using superconducting nanowire lead and thin film pedestal supporting the sample dilution refrigerator. The temperature increase $ΔT\sim 5$mK is detectable using quantum point contact thermometer.

hep-ph↗

arXiv2026

A Way of Axion Detection with Mass $10^{-4} \text{-}10^{-3}$eV Using Cylindrical Sample with Low Electric Conductivity

A dark matter axion with mass $m_a$ induces an oscillating electric field in a cylindrical sample placed under a magnetic field $B_0$ parallel to the cylinder axis. When the cylinder is made of a highly electrically conductive material, the induced oscillating current flows only at the surface. In contrast, if the cylinder is composed of a material with small conductivity, e.g. $σ= 10^{-3}\text{eV}$, the electric current flows inside the bulk of the cylinder. Within the QCD axion model, the current $I$ is estimated as $I(σ=10^{-3}\text{eV})\simeq 2.8\times 10^{-14}\text{A}g_γ\big(R/6\text{cm}\big)^2 \big(σ/10^{-3}\text{eV}\big)\big(B_0/15\text{T}\big)\big(10/ε\big)\big(ρ_a/0.3\rm GeVcm^{-3}\big)^{1/2}$ for $m_a=10^{-4}$eV, with radius $R$, permittivity $ε= 10$ of the cylinder and axion energy density $ρ_a$, where $g_γ$ is model dependent parameter; $g_γ(\text{KSVZ}) = -0.96$ and $g_γ(\text{DFSZ}) = 0.37$. Because the current is proportional to $R^2$, using large sample with $R=80$cm, we have large signal-noise ratio ( $>1$ ) even in temperature $T=4$K, $I(σ=10^{-3}\text{eV})/I_n({σ=10^{-3}\text{eV})}\times \sqrt{δωδt_{ob}/2π} \simeq 1.1g_γ(4\text{K}/T)^{1/2}(L/100\text{cm})^{1/2}(R/80\text{cm}) (B_0/7\mbox{T})(ρ_a/0.3\rm GeVcm^{-3})^{1/2} (δt_{ob}/10^3\,\text{s})^{1/2}$ for $m_a=10^{-4}\text{eV}$ with $ε=10$ and $σ=εm_a$, where thermal noise is $I_n=\sqrt{2Tδω/πR_c}$ with $δω=10^{-6}m_a$ and resistance $R_c=L/(σπR^2)$ of the cylinder with length $L$. Although a superconducting solenoid sufficiently large to accommodate such a sample is required, the detection of dark matter axions in our proposal may be feasible in the mass range $m_a =10^{-4}\text{-}10^{-3}\text{eV}$.

hep-ph↗

arXiv2025

Axion Dark Matter and Plateau-Plateau Transition in Quantum Hall Effect

Axion dark matter inevitably generates electromagnetic radiation in quantum Hall effect experiments that use strong magnetic fields. Although these emissions are very weak, we have shown using a QCD axion model that they influence the plateau-plateau transition at low temperatures (below $100$ mK) in a system with a large surface area (greater than $10^{-3}\rm cm^2$) of two-dimensional electrons. By analyzing previous experiments that show saturation of the transition width $ΔB$ as temperature and microwave frequency change, we provide evidence for the presence of axions. Notably, in most experiments without axion effects, the saturation frequency $f_s(T)$ is less than $1$ GHz at temperatures of $100$ mK or higher and for system sizes of $10^{-3}\rm cm^2$ or smaller. Additionally, the frequency $f_s(T)$ decreases with decreasing temperature or increasing system size. However, there are experiments that show a saturation frequency $f_s(T)\simeq 2.4$GHz despite a low temperature of 35 mK and a large surface area of $6.6\times 10^{-3}\rm cm^2$ for the Hall bar. This identical frequency of approximately $2.4$ GHz has also been observed in different plateau transitions and in Hall bars of varying sizes. These unexpected results are caused by axion microwaves. The saturation frequency $f_s=m_a/2π$ of $\simeq 2.4$ GHz implies an axion mass of $\simeq 10^{-5}$eV. By comparing the axion effect with thermal effect on the width $ΔB$, we have shown the dominance of the axion effect over thermal effect at low temperature less than $50$mK. The dominance of the axion effect is attributed to significant absorption of axion energy, which is proportional to the square of the number of electrons involved.

hep-ph↗

arXiv2024

Axion Detection with Quantum Hall Effect

Plateau-plateau transition in integer quantum Hall effect is a phase transition between metal and insulator. The behavior how the width $ΔB$ of the transition changes with temperature and frequency of radiations imposed has been explored extensively. It decreases with the decrease of temperature and frequency, but saturates at critical temperature or frequency. We have recently discussed the effect of axion dark matter on the saturation. The axion generates radiations under strong magnetic field in the experiment of quantum Hall effect. The radiations play a similar role to the one of radiations imposed externally. In this paper we discuss in detail how the width behaves in temperature and frequency under the effect of axion dark matter. We show that the axion effect can be observable in low temperature roughly below $100$mK. According to our detailed analysis of the saturation, we find that critical frequency of saturation observed in previous experiment strongly suggests axion mass $m_a=(0.95\sim 0.99)\times 10^{-5}$eV.

hep-ph↗

arXiv2023

A Way of Determination of Axion Mass with Quantum Hall Effect

Axion dark matter is converted to electromagnetic radiations in the presence of strong magnetic field. The radiations possibly give rise to non trivial phenomena in condensed matter physics. Especially, we discuss that saturation of plateau-plateau transition width observed at low temperature in integer quantum Hall effect is caused by the axion. The radiations from axions are inevitably present in the experiment. Although the radiations generated by axion is extremely weak, Hall conductivity jumps up to next plateau even if only a single electron occupies an extended state; a localized electron is transited to the extended state by absorbing the radiation. According to our analysis, previous experiment\cite{sat6} of the saturation in detail suggests that the axion mass is in the range $10^{-5}\mbox{eV}\sim 10^{-6}$eV. We propose a way of the determination of the axion mass by imposing microwaves on Hall bar and also a way of the confirmation that the axion really causes the saturation of the width.

hep-ph↗

arXiv2022

Resonant Axion Radiation Conversion in Solar Spicules

It has recently been observed that solar spicules covering almost of all solar surface have strong magnetic field $B\sim 10^2$G. They are supposed to be plasma jets emitted from chromosphere and they arrive up to $\sim 10^4$km. Their electron number density is such that $n_e=10^{10}\rm cm^{-3}\sim $$10^{12}\rm cm^{-3}$. Corresponding plasma frequency $m_p=\sqrt{e^2n_e/m_e}$ ( electron mass $m_e$ ) is nearly equal to axion mass $m_a=10^{-5}$eV$\sim 10^{-4}$eV. Thus, resonant radiation conversion of axion with the mass can arise in the spicules. We show that radiations converted from axion dark matter possess flux density $\sim 10^{-6}\mbox{Jy}(m_a/10^{-4}\mbox{eV})(B/3\times 10^2\rm G)^2$. The radiations show line spectrum with frequency $\simeq 24$GHz$(m_a/10^{-4}\rm eV)$. Our estimation has fewer ambiguities in physical parameters than similar estimation in neutron stars because physical parameters like electron number density have been more unambiguously observed in the sun. But, much strong solar thermal radiations would preclude sensitive observations of such radiations from the axions.

hep-ph↗

arXiv2022

Radiation Burst by Axion Star Collision with Star in the Andromeda Galaxy

Axion is a promising candidate of dark matter in the universe. A fraction of dark matter axion may forms axion star with radius $\sim 10^2$km. We show that the axion star emits radiation burst by the collision with K and M types main sequence star in the Andromeda Galaxy. The emission arises in the atmosphere of the star, in which electrons coherently oscillate due to oscillating electric field of the axion star. The electric field is produced under magnetic field $B$ of the star. We estimate the flux density of the radiation $\sim 1.6\times 10^{-3}\mbox{Jy} (10^{-12}M_{\odot}/M_a)^2(10^{-5}\mbox{eV}/m_a)^3(B/10^2\mbox{G})^2\sqrt{3\times10^3\mbox{K}/T}$ and the rate of the collision per hour $\sim 0.06/\mbox{hour}\,(10^{-12}M_{\odot}/M_a)$ in the galaxy, where $M_a$ ( $m_a$ ) denotes the mass of axion star ( axion ) and $T$ does temperature of the electrons. We assume the number $10^{11}$ of the stars with $B\sim 10^{2}$G and radius $\sim 3.5\times10^{5}$km in the galaxy. We also assume that a half of the dark matter is composed of axion star. We show that the emission of the radiation burst only arises in the atmosphere in which the plasma frequency $m_p\simeq m_a$. The duration of the burst lasts for the period which it takes the axion star to pass the region with $m_p\simeq m_a$. It would be longer than $1$ second.

hep-ph↗

arXiv2022

Detectable Electric Current induced by Dark Matter Axion in a Conductor

We propose a way of detecting dark matter axion by using two slabs of conductor. The flat surfaces are put to meet face to face so that they are parallel to each other. External magnetic field $B$ parallel to the surfaces is impressed. Radiations converted from the axion arise between two slabs. When we tune the spacing $l$ between two surfaces such as $l=π/m_a$ with axion mass $m_a$, a resonance occurs so that the radiations become strong. Furthermore, electric current flowing on the surface of the slabs is enhanced. We show that the electric current is large enough to be detectable at the resonance. It reaches $0.7\times 10^{-9}$A$(10^{-5}\mbox{eV}/m_a)^{1/2}(B/5\mbox{T})(L/10\mbox{cm})(σ/3.3\times 10^7\rm eV)$, using $6$N copper of the square slab with side length $L$ and high electrical conductivity $σ$ at temperature $T\sim 1$K. The power of the Joule heating is $0.3\times10^{-22}\mbox{W}(B/5\mbox{T})^2(10^{-5}\mbox{eV}/m_a)^{1/2}(L/10\mbox{cm})^2(σ/3.3\times 10^7\rm eV)$. When we amplify the power using LC circuit with $Q$ value, the signal to noise ratio is $4.5\times 10^4(Q/10^6)(B/5\mbox{T})^2(t_{obs}/1\sec)^{1/2}\,(10^{-5}\mbox{eV}/m_a) (L/10\mbox{cm})^2(σ/3.3\times 10^7\rm eV)$ with $t_{obs}$ observational time.

hep-ph↗

arXiv2021

Enhanced Radiation ? from (Super) Conductor by Dark Matter Axion

In our previous paper we have shown that enhanced radiations arise from (super) conductor by dark matter axion under strong magnetic field. We have recalculated the radiation by carefully treating boundary conditions between vacuum and the conductor. We show that the radiation is never enhanced. We interpret it such that electromagnetic field induced by axion collides the conductor and it is reflected by the conductor. The reflecting wave is the radiation from the conductor. It is reasonable that the amplitude of the reflection wave is identical to that of the incoming wave, i.e. radiation induced by axion.

hep-ph↗

arXiv2021

Spectral-temporal features of repeating ( one-off ) FRBs and Axion Star

The fast radio bursts ( FRBs ) are energetic radio bursts with millisecond duration only observed at radio frequencies. The generation mechanism is still mysterious. We have proposed a generation mechanism of both repeating and one-off FRBs. They arise from the axion star collision with neutron star or magnetized accretion disk of galactic black hole. Once we accept the existence of the axions, we find that the mechanism well explain previously observed spectral-temporal features. In this paper we show that it also explains recently observed phenomena such as downward drifting in the repeating FRBs, etc.. Analysis of the downward drifting based on Doppler effects has been presented in recent papers, in which a superradiance system of molecular or atom has been proposed as a source of FRBs. We apply the analysis to our mechanism and find that it well explains the relation between the downward drifting rate and the duration of the repeating FRBs. The Doppler effects lead to the fact that the duration of radio burst with higher center frequency is shorter than that of radio burst with lower center frequency in the repeating FRBs. Our generation mechanism naturally explain polarization angle swing observed in the repeating FRB180301 and one-off FRBs. We also discuss the association between the FRB200428 and magnetar SGR J1935+2154. The X ray burst observed just after the observation of the FRB could be triggered by the axion star collision with the magnetar. We also explain the consistency of our generation mechanism with observed spectral-temporal differences in the repeating and one-off FRBs, e.g. longer duration ( smaller flux density ) of repeating FRBs than duration ( flux density ) of one-off FRBs.

astro-ph.HE↗

arXiv2021

Radiation Production by Axion in Space between Two Flat Conductors

We have shown a new production mechanism of radiations produced by dark matter axion $a(t)$ under strong magnetic field $B$. The axion generates oscillating electric current in the surface of conductor. The current is extremely enhanced such as $J_c=(m_aδ_e)^{-2}J_a$ compared with vacuum current $J_a\equiv g_{aγγ}\partial_t a(t)B$; $δ_e$ is skin depth and axion mass $m_a$. We have shown that sufficiently strong radiation is emitted by cylindrical super ( normal ) conductor to be easily detected. Then, we naively expect that such strong radiation also arises in resonant cavity experiment. But we show that the expectation is wrong. The radiation generated in the cavity is just the one given in the standard estimation, even if we consider the enhanced current in the conductor of the cavity. This is because the radiation in the cavity is standing wave, while the radiation emitted from the cylindrical conductor is outgoing wave. For simplicity we consider radiation arising in the space between two parallel flat conductors.

hep-ph↗

arXiv2020

Axion-Radiation Conversion by Super and Normal Conductors

We have proposed a method for the detection of dark matter axion. It uses superconductor under strong magnetic field. As is well known, the dark matter axion induces oscillating electric field under magnetic field. The electric field is proportional to the magnetic field and makes charged particles oscillate in conductors. Then, radiations of electromagnetic fields are produced. Radiation flux depends on how large the electric field is induced and how large the number of charged particles is present in the conductors. We show that the electric field in superconductor is essentially identical to the one induced in vacuum. It is proportional to the magnetic field. It is only present in the surface because of Meissner effect. On the other hand, although the magnetic field can penetrates the normal conductor, the oscillating electric field is only present in the surface of the conductor because of the skin effect. The strength of the electric field induced in the surface is equal to the one in vacuum. We obtain the electric field in the superconductor by solving equations of electromagnetic fields coupled with axion and Cooper pair described by Ginzburg-Landau model. The electric field in the normal conductor is obtained by solving equations of electromagnetic fields in the conductor coupled with axion. We compare radiation flux from the cylindrical superconductor with that from the normal conductor with same size. We find that the radiation flux from the superconductor is a hundred times larger than the flux from the normal conductor. We also show that when we use superconducting resonant cavity, we obtain radiation energy generated in the cavity two times of the order of the magnitude larger than that in normal conducting resonant cavity.

hep-ph↗

arXiv2020

A New Method for Detecting Axion With Cylindrical Superconductor

We propose a method for searching dark matter axion in axion-photon conversion. We consider a superconductor of cylindrical shape under strong magnetic field. The dark matter axion generates oscillating electric field which induces oscillating superconducting current in the surface of the superconductor. The current gives rise to dipole radiation with the frequency $m_a/2π$ given by axion mass $m_a$. We show that the radiation flux generated by the current is of the order of $10^{-18}$W under magnetic field $\sim 3$T in the case of radius $\sim 1$cm and length $\sim 10$cm of the cylindrical superconductor. %The superconducting current flows in the surface to the depth $λ\simeq 5\times 10^{-6}$cm. The large amount of the radiation flux arises because Cooper pairs with large number density ( $\sim 10^{22}/\rm cm^{3}$ ) is present in the superconductor. With the high detection sensitivity, we can simultaneously search wide bandwidth of the radio frequency with existing radio telescope.

hep-ph↗

arXiv2019

Chiral Nonsymmetric Interaction in Strong Coupled QCD

Chiral symmetry in massless QCD is believed to be broken spontaneously. We discuss a possibility that the chiral symmetry is explicitly broken by QCD monopoles which appear only in strong coupled QCD. Namely, the monopole quark interaction explicitly breaks the chiral symmetry ( SU$_A(2)\times $U$_A$(1) ) just like bare quark mass terms. We show that the strength of the interaction is roughly $10$ times smaller than standard strong interactions. We describe it as an effective interaction $g'\bar{q}qΦ^{\dagger}Φ$ with the monopole field $Φ$ and $g'$ being of the order of $(10\rm \,GeV)^{-1}$ or less. It produces small constituent quark masses less than $1$MeV when the monopoles condense ( $\langleΦ\rangle\neq 0 $ ). We examine to what extent such a weak but explicit symmetry breaking interaction is allowed. In particular, examining Gell-Mann-Oakes-Renner relation we find that the presence of such a small symmetry breaking term is still allowed within the present accuracy of lattice gauge simulations. We predict some phenomenological effects caused by the chiral nonsymmetric monopole quark interaction. Quark confinement and chiral condensate ( $\langle\bar{q}q\rangle\neq 0$ ) arise simultaneously. The condensate $\langle\bar{q}q\rangle$ caused by the monopoles is proportional to monopole density and is estimated such that $(-\langle\bar{q}q\rangle)^{1/3}\sim 160$MeV. The weak monopole quark interaction leads to the small decay width of an observable monopole to hadrons.

hep-ph↗

arXiv2019

Explanation of Detailed Spectral Properties of FRBs by Axion Star Model

We have proposed a generation mechanism of non repeating ( repeating ) fast radio bursts: They arise by axion star collisions with neutron stars ( accretion disks of galactic black holes ). The axion star as coherent state of axions with mass $m_a$ generates homogeneous electric field oscillating with frequency $m_a/2π$ under strong magnetic fields. The field makes electrons coherently oscillate and emit the coherent dipole radiations ( FRBs ). The radiations stop when thermal fluctuations produced by the oscillation disturb the coherent oscillations. Thus, the duration of the FRBs is determined by the time scale of the thermalization; it is much shorter than $1$ms. Line spectra of the dipole radiations are broadened by the thermal effects. The thermally broaden spectra have a feature that the bandwidths $δν$ are proportional to their center frequencies $ν_c$. The presence of various center frequencies ( $1.2$GHz$\sim $$7$GHz ) in repeating FRB 121102 is attributed to Doppler shifts owing to the various relativistic velocities of the accretion disk. On the other hand, non repeating FRBs do not show such variety of the center frequencies. They come from the surfaces of neutron stars. The Doppler shift also makes the durations of the bursts with higher frequencies become shorter. Because the magnetic fields of the neutron stars are supposed to be stronger than those of the accretion disks, the peak flux densities of non repeating FRBs are larger than those of repeating FRB 121102. The strong magnetic fields of the neutron stars also lead to much wide bandwidths of non repeating FRBs, which are over the extent of the receiver frequency range. The spectral features of the recently discovered new repeating FRB 180814.J0422+75 are coincident with our general analyses of the repeating FRB 121102.

astro-ph.HE↗

arXiv2019

Nonvanishing pion masses for vanishing bare quark masses

It is generally thought that pion masses vanish when bare light quark masses $m_q$ vanish. The pions are Nambu-Goldstone bosons of chiral $SU_{A}(2)$ symmetry. We discuss a possibility that even when $m_q=0$, the chiral symmetry is explicitly broken in strong coupled QCD, while it is not in weakly coupled QCD. The point is that QCD monopoles are dynamical degrees of freedom in the strong coupled QCD. We show that the monopole quark interactions break the chiral $U_5(1)$ symmetry as well as the chiral $SU_{A}(2)$ symmetry. They are weak relative to the other chiral symmetric interactions of quarks and gluons. These weak interactions produce small pion masses as well as quark masses $\sim 20$MeV in the phase with the monopole condensation. The presence of the interactions modifies the Gell-Mann Oakes Renner relation. Using the relation we predict the value $(-\langle\bar{q}q\rangle)^{1/3}\simeq 160$MeV. We also show that the monopole quark interactions do not prevent the monopole condensation in dual superconducting model.

hep-ph↗

arXiv2019

A phenomenological model of QCD monopole hadron interactions

Monopoles have recently been discussed to be a dominant component in strong coupled quark gluon plasma ( QGP ) and to play a role for chiral symmetry breaking as well as quark confinement. We analyze monopole quark interactions and show that massless quarks colliding with the monopoles inevitably change their chiralities keeping their flavors. The monopole quark interaction explicitly breaks the chiral symmetry ( SU$_A(2)\times $U$_A$(1) ) just like bare quark masses. It is given by $\bar{q}qΦ^{\dagger}Φ$ with the monopole field $Φ$. The pions are not Nambu-Goldstone bosons even in the vanishing bare quark masses. Their masses are mainly determined by the interaction because the monopole condensation generates a larger current quark mass than the bare quark masses. Based on the analysis of the monopole quark interaction, we propose a phenomenological linear sigma model coupled with the monopoles. The monopoles couple only with isoscalar scalar mesons e.g. sigma meson $σ$ such as $σΦ^{\dagger}Φ$ indicated by the monopole quark interaction. The coupling explicitly breaks the chiral SU(2)$_A\times $U$_A$(1) symmetry. Pion masses are generated by the chiral condensate, which arises only when the monopole condensate takes place. We show that one of the monopoles is a color singlet and observable. The monopole decays into hadrons ( pions, kaon, etc. ) through the coupling. Our analysis indicates that $f_0(1500)$ meson is a candidate of the observable monopole. As phenomenological effects of these monopoles, we point out that the masses of hadrons decrease in dense nuclear matters and that chiral magnetic effects disappear in strong coupled QGP.

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