11032373
Properties of the Ground-State q bar q Mesons and Possible Classification of Observed Mesons in the U~(12)_SF X O(3,1)_L Scheme
We examine possible assignments for known mesons to the predicted ground-state q bar q multiplets in the U~(12)_SF-classification scheme of hadrons, based on their observed properties. The masses of missing members of the ground-state multiplets are estimated, using a phenomenological mixing scheme for the normal- and extra-spin wave functions specific to this classification scheme. We also examine experimental candidates for the excited 1P, 1D and 2S multiplets in a framework of the U~(12)_SF X O(3,1)_L-classification scheme, based on the analysis of the ground-state masses. Then we see that the two exotic mesons pi_1(1400) and pi_1(1600) with J^PC=1^-+ have suitable masses to be assigned to the P-wave excitation and also there are a number of observed mesonic states which could be classified in terms of the U~(12)_SF X O(3,1)_L scheme.
121019776
Radiative Decays of Ground-State Mesons in the Covariant Quark Model
17021934
On the existence of light-scalar mesons kappa(800) and kappa-prime(1150): The ~U(12) scheme and BES II data
We present that there should exist a light strange-scalar meson kappa', in addition to the kappa(800), which has a mass around 1.1-1.2 GeV, a rather narrow width, and couples strongly to kappa(800)sigma(600) (Kpipipi) but weakly to Kpi, based upon the U~(12)-classification scheme of hadrons and BES II data on J/psi -> barK*(892)0K+pi- decay.
3204285
Candidates for Chiral Particles
We find possible candidates for the new type of q bar q meson, mesonic chiralons, whose existence is predicted in the covariant level-classification scheme of hadrons with U(12)_SF * O(3,1)_L symmetry, by assigning all the known light-unflavored and strange mesons, with masses below about 1.8 GeV, to U(12)_SF * O(3,1)_L multiplets.
116028786
Regge trajectories of mesons and baryons and a universal spring
59929438
Is the f1(1420) Our First Hybrid Meson
119199264
Improving the moment approach for astrometric binaries: possible application to Cygnus X-1
A moment approach for orbital determinations of astrometric binaries from astrometric observations alone has been recently studied for a low signal-to-noise ratio (Iwama et al. 2013, PASJ, 65, 2). Through avoiding a direct use of the time-consuming Kepler equation, temporalinformationistakenintoaccount toincrease theaccuracy ofstatistical moments. As numerical tests, 100 realizations are done and the mean value and the standard deviation are also evaluated. For a semimajor axis, the difference between the mean of the recovered values and the true value decreases to less than a tenth in the case of 10000 observed points. Therefore, the present approach works better than the previous one for orbital determinations when one has a large number of observed points. The present approach is thus applicable to CygX-1.
118837610
Possible latitude effects of Chern-Simons gravity on quantum interference
It has been recently suggested that possible effects of Chern-Simons gravity on a quantum interferometer are dependent on the latitude and direction of the interferometer on Earth in orbital motion around Sun. Continuing work initiated in the earlier publication [Okawara, Yamada and Asada, Phys. Rev. Lett. 109, 231101 (2012)], we perform numerical calculations of time variation in the induced phase shifts for nonequatorial cases. We show that the maximum phase shift at any latitude might occur at 6, 0 (and 12), and 18 hours (in local time) of each day, when the normal vector to the interferometer is vertical, eastbound and northbound, respectively. If two identical interferometers were located at different latitudes, the difference between two phase shifts that are measured at the same local time would be $O(\sin \delta\varphi)$ for a small latitude difference $\delta\varphi$. It might thus become maximally $\sim 20$ percents for $\delta\varphi \sim 10$ degrees, for instance.
118481414
Marginally stable circular orbit of a test body in spherically symmetric and static spacetimes
We study a marginally stable circular orbit (MSCO) such as the innermost stable circular orbit (ISCO) of a timelike geodesic in any spherically symmetric and static spacetime. It turns out that the metric components are separable from the constants of motion along geodesics. We show also that a metric component $g_{rr}$ with a radial coordinate $r$ does not affect MSCOs. This suggests that, as a test of gravity, any ISCO measurement may be put into the same category as gravitational redshift experiments. MSCOs for exact solutions to the Einstein's equation are also mentioned.
119108584
Moment Approach to Determining the Orbital Elements of an Astrometric Binary with a Low Signal-to-Noise Ratio
A moment approach to the orbit determination of an astrometric binary with a low signal-to-noise ratio from astrometric observations alone is proposed, especially aiming at a close binary system with a short orbital period, such as Cyg X-1, and also at a star wobbled by planets. As an exact solution to the nonlinearly coupled equation, the orbital elements are written in terms of the second and third moments of projected positions that are measured by astrometry. This may hold the possibility of the true orbit estimate.
119307503
Post-Newtonian effects on Lagrange's equilateral triangular solution for the three-body problem
Continuing work initiated in earlier publications [Yamada, Asada, Phys. Rev. D 82, 104019 (2010); ibid.83, 024040 (2011)], we investigate the post-Newtonian effects on Lagrange's equilateral triangular solution for the three-body problem. For three finite masses, it is found that the equilateral triangular configuration satisfies the post-Newtonian equation of motion in general relativity, if and only if all three masses are equal. When a test mass is included, the equilateral configuration is possible for two cases: (1) one mass is finite and the other two are zero, or (2) two of the masses are finite and equal, and the third one is zero, namely, a symmetric binary with a test mass. The angular velocity of the post-Newtonian equilateral triangular configuration is always smaller than the Newtonian one, provided that the masses and the side length are the same.