Spin and Accretion Rate Dependence of Black Hole X-Ray Spectra

We present a survey of how the spectral features of black hole X-ray binary systems depend on spin, accretion rate, viewing angle, and Fe abundance when predicted on the basis of first-principles physical calculations. The power-law component hardens with increasing spin. The thermal component strengthens with increasing accretion rate. The Compton bump is enhanced by higher accretion rate and lower spin. The Fe Kα equivalent width grows sublinearly with Fe abundance. Strikingly, the Kα profile is more sensitive to accretion rate than to spin because its radial surface brightness profile is relatively flat, and higher accretion rate extends the production region to smaller radii. The overall radiative efficiency is at least 30%–100% greater than as predicted by the Novikov–Thorne model.

THE DIFFERENCES IN THE BALL SPEED AND THE SPIN RATE DEPENDING ON THE RESULTS OF A TENNIS SERVE

In tennis, the service is the only shot that a player can give himself without being influenced by his opponent, and it is said to be the most powerful and essential shot in the game to win the game (Kovacs and Ellenbecker, 2011). In this study, we will investigate the difference in speed and spin rate in services when a service is entered, when it is not entered, and when an ace is taken. Fourteen three-set singles matches of 20 participants in the ATP Challenger tournament were included in the analysis. The speed and spin rate was measured using the Trackman. The analysis included 1343 1st service balls. We compared the speed and spin rate for each IN, FAULT and ACE in the 1st service using one-way ANOVA. The speed of the 1st service, IN was significantly slower than that of FAULT and ACE. The spin rate of the 1st serve, IN had significantly more revolutions than the FAULT and ACE. The results of this study showed that the service was faster and lower spin rate when ACE was taken. However, it was found that the faster the speed of the service and the lower the spin rate, the higher the rate of FAULT. These considerations suggest that it is important to decide whether to take risks or play it safe, depending on the game situation at the time.

Synthesis and Analysis of Zirconium Titanate Thin Films by using Sol-Gel Method

Titanium-doped zirconium oxide (mixed high-k) has been used as the gate oxide layer for the future generation metal oxide semiconductor devices. This mixed high-k layer was prepared by using Sol-Gel based spin-coated method. This mixed high-k layer’s chemical, structural, and initial electrical properties are investigated thoroughly. It is clearly confirmed that the suitable chemical composition and bond formation of the proposed mixed high-k layer from EDAX and FTIR analysis observations. The XRD spectra strengthened the presence of ZrTiO2. The measured dielectric constant of the proposed mixed high-k layer from the extracted C-V plots has been varying from 29.1 to 37.6 with respect to spin coating from 4000 to 6000 rpm. With lower spin rates, the leakage current is less.

Characterizations of Hollow Polyvinylidene Fluoride-Co-Trifluoroethylene (P(VDF-TrFE)) Nano-Bundles Produced by Template-Assisted Method

The present study describs the fabrication of hollow polyvinylidene fluoride-co-trifluoroethylene (P(VDF-TrFE)) nano-bundles by the template-assisted method. The P(VDF-TrFE) solution was spin-coated onto porous templates at four different rotation speeds, e.g., 1000 rpm, 2000 rpm, 3000 rpm, and 4000 rpm. The characteristics of the prepared nanostructures were evaluated to examine their morphological, structural, and hysteresis behaviors. All the P(VDF-TrFE) nanostructures were characterized as bundles rather than individual structures due to their agglomeration properties. The P(VDF-TrFE) nanostructures, which were synthesized at 4000 rpm, ensured a shorter length in comparison to the others fabricated at lower spin rates. Despite their different diameters and lengths, no clear difference was observed in the crystallinities of these nanostructures.

The physical origins of low-mass spin bias

ABSTRACT At z = 0, higher-spin haloes with masses above $\log (M_{\text{c}}/h^{-1}\, \text{M}_\odot)\simeq 11.5$ have a higher bias than lower-spin haloes of the same mass. However, this trend is known to invert below this characteristic crossover mass, Mc. In this paper, we measure the redshift evolution and scale dependence of halo spin bias at the low-mass end and demonstrate that the inversion of the signal is entirely produced by the effect of splashback haloes. These low-mass haloes tend to live in the vicinity of significantly more massive haloes, thus sharing their large-scale bias properties. We further show that the location of the redshift-dependent crossover mass scale Mc(z) is completely determined by the relative abundance of splashbacks in the low- and high-spin subpopulations. Once splashback haloes are removed from the sample, the intrinsic mass dependence of spin bias is recovered. Since splashbacks have been shown to account for some of the assembly bias signal at the low-mass end, our results unveil a specific link between two different secondary bias trends: spin bias and assembly bias.

Total Routhian surface calculations to study the abrupt band termination phenomenon in 121,123I

The phenomenon of abrupt band termination in [Formula: see text]I has been revisited in the light of total Routhian surface (TRS) calculations. Both axial ([Formula: see text]) and nonaxial ([Formula: see text]) quadrupole deformation parameters have been estimated for the negative parity states. The calculation has also been extended for [Formula: see text]I and the theoretical result has been compared with the available experimental information. The calculated transition quadrupole moments ([Formula: see text]) are matching nicely upto [Formula: see text] MeV. The noncollective oblate shapes become yrast at higher angular frequency in [Formula: see text]I. At lower spin, all of these nuclei exhibit a collective prolate shape. This sudden change in shape at [Formula: see text] is indicative of the loss of collectivity at [Formula: see text]–[Formula: see text] MeV.

Velocity pointing error reduction for symmetric spinning spacecraft via a two-burn scheme

During axial thrusting of a symmetric spinning spacecraft, misalignment and center-of-mass offset can cause unwanted body-fixed torques. The two-burn scheme is applied to eliminate velocity pointing error. Solutions for angular velocity, Euler angle, and inertial velocity with nonzero initial conditions are derived in a new form for axisymmetric spacecraft with constant mass. Simulations show that the solutions closely match numerical simulations and the two-burn scheme decrease the velocity pointing error obviously. Based on the solutions, the effect of two-burn scheme is analyzed. The results show that the spacecraft will obtain the minimum velocity pointing error if the burn and coast times are controlled accurately. Also, the two-burn scheme allows for a lower spin rate and the spacecraft can be maneuvered at nonzero initial conditions compared with the continuous thrust scheme.