Coordinated TLE (transient luminous event) optical observations in Taiwan have been held since 2011, with an aim to achieve triangulation. Currently, there are four observation stations with baselines varying from 100 to 400 km between them. The system recorded eight gigantic jets (GJs) that were recorded by at least two stations on the night of 20 August 2014. The weather radar data indicate that these GJs occurred around the troposphere overshooting tops of a vigorous cumulonimbus cloud. A leader‐to‐streamer transition was discerned as the appearance of these GJs changed from jet‐like (leader) to fan‐like (streamer) at ~40 km altitude. Most of these GJs terminated at the lower ionosphere boundary (80–90 km), but one GJ topped with a 10 km thick diffuse region extended higher than 100 km. Moreover, three sets of the GJs occurred within 0.5–100 s in the same general region. The residual plasma patches from the preceding GJs appear to cause the subsequent GJs to contain more bead structures and to be brighter. Also, three streamer columns of a subsequent GJ that occurred more than 100 s after the preceding GJ were identified to have rebrightened at 55 to 70 km altitudes. The rebrightened streamers and the bead structure increments in the subsequent GJs suggest that there were GJ‐produced long‐lasting plasma patches in the mesosphere.

According to the Einstein, Weinberg, and Møller energy-momentum complexes, we evaluate the energy distribution of the singularity-free solution of the Einstein field equations coupled to a suitable nonlinear electrodynamics suggested by Ayón-Beato and García. The results show that the energy associated with the definitions of Einstein and Weinberg are the same, but Møller not. Using the power series expansion, we find out that the first two terms in the expression are the same as the energy distributions of the Reissner-Nordström solution, and the third term could be used to survey the factualness between numerous solutions of the Einstein field equations coupled to a nonlinear electrodynamics.

We obtain the energy distribution of the gamma metric using the energy-momentum complex of Møller. The result is the same as obtained by Virbhadra in the Weinberg prescription.

This paper utilizes 10 stations of co-located seismometer, QuakeFinder/infrasound to observe co-seismic signatures triggered by the 6 February 2016 M 6.6 Meinong Earthquake. Each QuakeFinder system consists of a 3-axes induction magnetometer, an air conductivity sensor, a geophone, and temperature/relative humidity sensors. There are no obvious charges in the positive/negative ions, the temperature, and the humidity, while the magnetometer, the geophone, and infrasound data detect clear co-seismic signatures, similar to seismic waves recorded by seismometers. The magnetometers register high-frequency pulsations, like seismic waves, and superimpose with low-frequency variations, which could be caused by the magnetometer shaking/tilting and/or the underground water level change, respectively, upon the arrival of seismic waves. The spectrum centering around 2.0 Hz of the co-seismic geophone fluctuations is similar to that of the seismic waves. However, the energy of co-seismic geophone fluctuations (also magnetometer pulsations) yields an exponential decay to the distance of a station to the epicenter, while the energy of the seismic waves is inversely proportional to the square of the distance. This suggests that the mechanisms for detecting seismic waves of the QuakeFinder system and seismometers are different. In general, the geophone and magnetometer/infrasound system are useful to record high-and low-frequency seismic waves, respectively.

The energy distributions of four 2+1 dimensional black hole solutions were obtained by using the Einstein and Møller energy-momentum complexes. While r → ∞, the energy distributions of Virbhadra's solution for the Einstein-massless scalar equation becames E Ein ∼ π κ (1 − q)R q and E Møl ∼ − 2π κ q(1 − q)R q , and the energy distributions of these three solutions become E Ein ∼ πΛr 2 κ and E Møl ∼ − 4πΛr 2 κ .