Evolution of twist-shear and dip-shear in Faring active region NOAA 10930

We study the evolution of magnetic shear angle in a flare productive active region NOAA 10930. The magnetic shear angle is defined as the deviation in the orientation of the observed magnetic field vector with respect to the potential field vector. The shear angle is measured in horizontal as well as vertical plane. The former is computed by taking the difference between the azimuth angles of the observed and potential field and is called the twist-shear, while the latter is computed by taking the difference between the inclination angles of the observed and potential field and is called the dip-shear. The evolution of the two shear angles is then tracked over a small region located over the sheared penumbra of the delta sunspot in NOAA 10930. We find that, while the twist-shear shows an increasing trend after the flare the dip-shear shows a significant drop after the flare.Comment: 4 pages, Proceedings of IAU Symposium 273 "Physics of Sun and Starspots" Eds. D.P. Choudhary and K.G. Strassmeie

The aerodynamic effects of wing rotation and a revised quasi-steady model of flapping flight

We used a dynamically scaled model insect to measure the rotational forces produced by a flapping insect wing. A steadily translating wing was rotated at a range of constant angular velocities, and the resulting aerodynamic forces were measured using a sensor attached to the base of the wing. These instantaneous forces were compared with quasi-steady estimates based on translational force coefficients. Because translational and rotational velocities were constant, the wing inertia was negligible, and any difference between measured forces and estimates based on translational force coefficients could be attributed to the aerodynamic effects of wing rotation. By factoring out the geometry and kinematics of the wings from the rotational forces, we determined rotational force coefficients for a range of angular velocities and different axes of rotation. The measured coefficients were compared with a mathematical model developed for two-dimensional motions in inviscid fluids, which we adapted to the three-dimensional case using blade element theory. As predicted by theory, the rotational coefficient varied linearly with the position of the rotational axis for all angular velocities measured. The coefficient also, however, varied with angular velocity, in contrast to theoretical predictions. Using the measured rotational coefficients, we modified a standard quasi-steady model of insect flight to include rotational forces, translational forces and the added mass inertia. The revised model predicts the time course of force generation for several different patterns of flapping kinematics more accurately than a model based solely on translational force coefficients. By subtracting the improved quasi-steady estimates from the measured forces, we isolated the aerodynamic forces due to wake capture

Polarization Measurements and the Pairing Gap in the Universal Regime

We analyze recent cold-atom experiments on imbalanced Fermi systems using a minimal model with a BCS-like superfluid phase coexisting with a normal phase. This model is used to extract the T=0 pairing gap in the fully paired superfluid state. The recently measured particle density profiles are in good agreement with the theoretical predictions obtained from the universal parameters from previous Quantum Monte Carlo calculations. We find that the T=0 pairing gap is greater than 0.4 times the Fermi energy $E_F$, with a preferred value of $0.45 \pm 0.05$ $E_F$. The ratio of the pairing gap $\Delta$ to the Fermi Energy $E_F$ is larger here than in any other system of strongly-paired fermions in which individual pairs are unbound.Comment: 4 pages, 3 figures. Revised verison includes cosmetic changes to the text and figures. One reference adde

Opinion Leaders in Real Estate Markets

The purpose of this research paper is to examine the influence of opinion leaders in real estate markets. First, we provide a literature review of opinion leaders and real estate markets in India. Secondly, the variables that influence the opinion leaders are established and their measurement is well defined. Thirdly, a survey has been conducted by using a self-administered questionnaire, which was sent to 234 individuals who are responsible for handling real estate firms. The research model is empirically tested in a sample of 128 respondents by using a chi-square analysis. This study finds that opinion leaders in real estate markets possess significantly higher levels in exposure to media sources, social involvement, product knowledge, innovativeness, and computer usage than non-leaders. Opinion leaders also possess a higher degree of social networking and have used the internet more frequently for longer sessions than non-leaders. Finally, we identify the key implications, conclude the research finding and explore potential avenues for future research.Financial leverage; Asset valuation; Taxation

Evolution of twist-shear and dip-shear during X-class flare of 13 December 2006: Hinode observations

The non-potentiality (NP) of the solar magnetic fields is measured traditionally in terms of magnetic shear angle i.e., the angle between observed and potential field azimuth. Here, we introduce another measure of shear that has not been studied earlier in solar active regions, i.e. the one that is associated with the inclination angle of the magnetic field. This form of shear, which we call as the "dip-shear", can be calculated by taking the difference between the observed and potential field inclination. In this Letter, we study the evolution of dip-shear as well as the conventional twist-shear in a $\delta$-sunspot using high-resolution vector magnetograms from {\it Hinode} space mission. We monitor these shears in a penumbral region located close to flare site during 12 and 13 December 2006. It is found that: (i) the penumbral area close to the flaring site shows high value of twist-shear and dip-shear as compared to other parts of penumbra, (ii) after the flare the value of dip-shear drops in this region while the twist-shear in this region tends to increase after the flare, (iii) the dip-shear and twist-shear are correlated such that pixels with large twist-shear also tend to exhibit large dip-shear, and (iv) the correlation between the twist-shear and dip-shear is tighter after the flare. The present study suggests that monitoring twist-shear during the flare alone is not sufficient but we need to monitor it together with dip-shear.Comment: Astrophysical Journal Letters (In Press), 20 pages, 5 figure

Neutrino Emissivity of Dense Stars

The neutrino emissivity of compact stars is investigated in this work. We consider stars consisting of nuclear as well as quark matter for this purpose. Different models are used to calculate the composition of nuclear and quark matter and the neutrino emissivity. Depending on the model under consideration, the neutrino emissivity of nuclear as well as quark matter varies over a wide range. We find that for nuclear matter, the direct URCA processes are allowed for most of the relativistic models without and with strange baryons, whereas for the nonrelativistic models this shows a strong dependence on the type of nuclear interaction employed. When the direct URCA processes are allowed, the neutrino emissivity of hadronic matter is larger than that of the quark matter by several orders of magnitude. We also find that the neutrino emissivity departs from $T^6$ behavior when the temperature is larger than the difference in the Fermi momenta of the particles, participating in the neutrino-producing reactions.Comment: Latex file. 5 figures available on request. accepted in Int. J. Mod. Phys.