The morphology of the ǫ Eridani dust ring is reproduced by a numerical simulation of dust particles captured into the 5:3 and 3:2 exterior mean-motion resonances with a 0.3 eccentricity 10 solar mass planet at periastron at a semi-major axis of 40 AU. The morphology will differ when the planet is at aphelion, in about 140 years. Moderate eccentricity planets in outer extra-solar systems will ca...

We have investigated whether Earth-mass planets could survive in the habitable zone (HZ) of the 47 Ursae Majoris system. Mixed-variable symplectic numerical integration has been used to investigate the orbits of putative Earth-mass planets. Whereas the 47 UMa system as previously known, with just one giant planet, could have Earth-mass planets that remain confined to the HZ for a fairly wide ra...

We investigate the estimation of orbital parameters by least-χ2 Keplerian fits to radial velocity (RV) data using synthetic data sets. We find that while the fitted period is fairly accurate, the best-fit eccentricity and Mp sin i are systematically biased upward from the true values for low signal-to-noise ratio K/σ . 3 and moderate number of observations Nobs . 60, leading to a suppression of...

In a series of papers, we developed a technique for estimating the inner eccentricity in hierarchical triple systems, with the inner orbit being initially circular. However, for certain combinations of the masses and the orbital elements, the secular part of the solution failed. In the present paper, we derive a new solution for the secular part of the inner eccentricity, which corrects the pre...

We used an Isospin dependent Quantum Molecular Dynamics (IQMD) model to simulate Au + collisions at beam energy $E_{beam}$ = 1.23$A$ GeV, which corresponds center of mass $\sqrt{s_{NN}} 2.4$ GeV. Firstly, we obtained reasonable rapidity and transverse spectra $\pi^-$ $\pi^+$ as well "apparent" temperature parameters in comparison with the HADES data. Then by calculating three-dimensional Hanbur...

Self-stabilizing algorithms model distributed systems, which automatically recover from transient failures in the state of the system. The center of a graph comprises a set of vertices with minimum eccentricity. Farley and Proskurowski showed the linear time algorithm for locating the center of an outerplanar graph in the classical computing paradigm. The present paper investigates the selfstab...

Milli-second pulsars with highly stable periods can be considered as very precise clocks and used for pulsar timing array (PTA) which attempts to detect nanoheltz gravitational waves (GWs) directly. Main sources of GWs are supermassive black hole (SMBH) binaries have sub-pc-scale orbits. On the other hand, a SMBH binary is in an earlier phase has pc-scale orbit emits ultra-low-frequency ($\less...

We examine the distributions of eccentricity and host star metallicity of exoplanets as a function of their mass. Planets with M sin i & 4 MJ have an eccentricity distribution consistent with that of binary stars, while planets with M sin i . 4 MJ are less eccentric than binary stars and more massive planets. In addition, host star metallicities decrease with planet mass. The statistical signif...

The "distractor eccentricity effect" refers to the finding of reduced interference from an incompatible distractor at a central relative to a peripheral location (Chen, 2008). The present study examines the mechanism that underlies the distractor eccentricity effect, and relates it to the inattentional blindness explored by Mack and Rock (1998), which was also more marked at a foveal than at a ...