We demonstrate a synthetic Hall effect for light, using an acousto-optically modulated nanophotonic resonator chain. To produce this effect, we simultaneously generate the required synthetic electric field using temporal modulation and the required synthetic magnetic field using spatial modulation of the resonator chain. We show how the combination of these synthetic fields transverse to the direction of light propagation can be used to produce non-reciprocal optical transmission, as a basis for new photonic and topological devices.
We experimentally realize a synthetic Hall effect for light, by producing synthetic electric and magnetic fields in a nanophotonic resonator chain. We show that the effect can be dynamically reconfigured and manifests as non-reciprocal light transmission through the system.
Microquasars, nearby stellar-scale analogy of quasars, are producing jets at speeds very close to the speed of light up to 0.98 c. Microquasars are also accreting transient or persistent X-ray binaries. For a decade since its discovery, the phenomena of microquasars have had a great deal of attention. The observation of transient flares and accompanied jet phenomena is one of the highlights in the fields of X-ray, radio and, very recently, infrared astronomy. The recent observations have indicated that the superluminal jets probably are the common nature of the black hole X-ray binaries and, in part, of the neutron star binary sources. The recent development in observational techniques has made it possible to study detailed feature of jet phenomena. In the radio the very long baseline interferometry (VLBI) is required to map images of jets. The first Korean VLBI Network (KVN), recently proposed for the mm-wave multi-channel receiver system of 2.5, 8.5, 23, 43, 86 129 GHz, therefore, can be a promising tool of probing the nature of microquasars. In this paper, we present the strategy of observing microquasar phenomena with radio telescopes in Korea, including KVN, and international collaboration with Japanese VLBI system, VERA. Monitoring program for microquasars with 6 14 21 m array is also presented. As an example radio timing of frequently flaring, radio-bright microquasars such as GRS 1915+105 and Cyg X-3 are discussed.
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