arXiv subjects

Yota Endo

Publications and source records attributed to Yota Endo.

4 recordsLinked to original sources

arXiv2026

Motion of a charged test particle around a static black hole in a monopole magnetic field

We study the motion of a charged test particle in the spacetime with a spherically symmetric black hole which is immersed in a monopole magnetic field. We show that the radial motion of the charged test particle is governed by completely the same equation as that in the case of no magnetic field. This result implies that the black hole will acquire the electric charge if it is surrounded by the collisionless plasma composed of protons and electrons which obey the Maxwell velocity distribution. The drastically different situation appears in the tangential motions of charged test particles due to the magnetic field. The trajectory of a charged test particle in the black hole with the magnetic field of the order of 10 Gauss near the black hole, is confined on a very thin cone as long as the specific angular momentum of the particle is not much larger than the gravitational radius of the black hole times the speed of light. This result leads to a possibility that a plasma lump can hover over the black hole and is very hot, in the monopole magnetic field.

gr-qc↗

arXiv2026

Performance evaluation of Luxium Solutions BCF-XL wavelength-shifting fibers

We evaluate the performance of single-clad wavelength-shifting fibers newly developed by Luxium Solutions, BCF-92XL, BCF-9929AXL, and BCF-9995XL and compare them with the multi-clad Kuraray Y-11 fiber. The BCF-XL fibers exhibit faster decay times (92XL: $2.10\pm0.01$ ns, 9929AXL: $2.10\pm0.02$ ns, 9995XL: $2.41\pm0.03$ ns) than Y-11 ($7.44\pm0.06$ ns). The attenuation lengths are comparable to that of Y-11 within the measurement range up to 3.2 m. When coupled to an EJ-204 plastic scintillator, the BCF-XL fibers achieve superior time resolution while maintaining light yields comparable to those expected for a single-clad Y-11 fiber.

physics.ins-det↗

arXiv2025

Vacuum Magnetospheres around Kerr Black Holes with a Thin Disk

We construct a model for stationary and axisymmetric black hole magnetospheres by solving the vacuum Maxwell equations in Kerr backgrounds. The poloidal magnetic field is generated by a toroidal electric current in a thin disk on the equatorial plane with an inner edge, and the poloidal electric field is induced due to the black hole spin. We assume a current distribution whose direction reverses at a radius on the disk. The magnetospheric structure is divided into the inner region and the outer one due to the current reversal. In the inner region, some magnetic field lines connect the black hole and the disk, and others surround the inner edge of the disk. In the outer region, the field lines connect the disk and infinity. We investigate the black hole spin dependence of the magnetospheric structure. In the magnetosphere around the Kerr black hole, the electric fields are generated by the black hole spin. In our model, the charge distribution is induced on the disk and the event horizon. Except near the black hole, the electric field strength is proportional to the black hole spin, while the direction of the electric field remains almost the same regardless of the spin. On the other hand, the electromagnetic field near the event horizon strongly depends on the spin. In the maximally rotating case, the magnetic field lines are expelled from the event horizon and the electric equipotential surface coincides with the horizon.

gr-qc↗

arXiv2022

Relativistic Nontopological Soliton Stars in a U(1) Gauge Higgs Model

We study spherically symmetric nontopological soliton stars (NTS stars) numerically in the coupled system of a complex scalar field, a U(1) gauge field, a complex Higgs scalar field, and Einstein gravity, where the symmetry is broken spontaneously. The gravitational mass of NTS stars is limited by a maximum mass for a fixed breaking scale, and the maximum mass increases steeply as the breaking scale decreases. In the case of the breaking scale is much less than the Planck scale, the maximum mass of NTS stars becomes the astrophysical scale, and such a star is relativistically compact so that it has the innermost stable circular orbit. The first author contributed with a part of numerical calculations. The second did with planning and conducting the research, and the third did with all numerical calculations and finding new properties of the system.

hep-th↗