用引力波干涉仪天线探测新物理和非线性真空QED效应
Probing For New Physics and Detecting non linear vacuum QED effects using gravitational wave interferometer antennas
摘要：
真空中的低能非线性QED效应自1936年以来就被预言，并且几十年来一直是研究的主题。两个主要的方案已经提出了这样的'第一'检测：测量椭圆度的线偏振光束通过磁场和直接光-光散射。研究光在外场中的传播也可以用来探索新的物理学，如轴子粒子和毫荷电粒子的存在。它们在自然界中的存在会导致真空的折射率在存在外场的情况下不同于1，并且取决于光传播的偏振方向。在LIGO和VIRGO等引力波干涉仪中达到项目灵敏度的主要成就，为使用此类仪器检测电动力学中的QED校正和在极低能量下探索新物理开辟了可能性。本文讨论了直接测量双折射率与折射率测量的区别。我们提出了一个几乎寄生的实施外部磁场沿武器的处女座干涉仪，并讨论了这种选择的优势相比，以前提出的配置的基础上较短的原型干涉仪，我们认为是不够的。考虑到应变的设计灵敏度，对于不久的将来的VIRGO+干涉仪，$h<2\cdot10^{-23} \frac{1}{\sqrt{\rm Hz}}$在40 Hz范围内$- 400$ Hz导致在20 Hz以上的频率处的可变偶极磁体配置，使得$B^{2}D \ge 13000$ T $^{2}$ m/ $\sqrt{\rm Hz}$用于"第一“真空非线性QED检测。
英文摘要：
Low energy non linear QED effects in vacuum have been predicted since 1936 and have been subject of research for many decades. Two main schemes have been proposed for such a 'first' detection: measurements of ellipticity acquired by a linearly polarized beam of light passing through a magnetic field and direct light-light scattering. The study of the propagation of light through an external field can also be used to probe for new physics such as the existence of axion-like particles and millicharged particles. Their existence in nature would cause the index of refraction of vacuum to be different from unity in the presence of an external field and dependent of the polarization direction of the light propagating. The major achievement of reaching the project sensitivities in gravitational wave interferometers such as LIGO an VIRGO has opened the possibility of using such instruments for the detection of QED corrections in electrodynamics and for probing new physics at very low energies. In this paper we discuss the difference between direct birefringence measurements and index of refraction measurements. We propose an almost parasitic implementation of an external magnetic field along the arms of the VIRGO interferometer and discuss the advantage of this choice in comparison to a previously proposed configuration based on shorter prototype interferometers which we believe is inadequate. Considering the design sensitivity in the strain, for the near future VIRGO+ interferometer, of $h<2\cdot10^{-23} \frac{1}{\sqrt{\rm Hz}}$ in the range 40 Hz $- 400$ Hz leads to a variable dipole magnet configuration at a frequency above 20 Hz such that $B^{2}D \ge 13000$ T$^{2}$m/$\sqrt{\rm Hz}$ for a `first' vacuum non linear QED detection.
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