ar X iv : a st ro - p h / 03 01 35 3 v 4 2 7 Fe b 20 03 The Apsidal Antialignment of the HD 82943 System †

ar X iv : a st ro - p h / 03 01 35 3 v 1 1 7 Ja n 20 03 The Apsidal Alignment of the HD 82943 System

We perform numerical simulations to explore the dynamical evolution of the HD 82943 planetary system. By simulating diverse planetary configurations, we find two mechanisms to maintain the stability of the system: the 2:1 mean motion resonance between the planets can act as the first mechanism for all stable orbits. The second mechanism is the apsidal alignment and we find that the difference o...

ar X iv : a st ro - p h / 03 01 35 3 v 3 3 F eb 2 00 3 The Apsidal Alignment of the HD 82943 System

We perform numerical simulations to explore the dynamical evolution of the HD 82943 planetary system. By simulating diverse planetary configurations, we find two mechanisms to maintain the stability of the system: the 2:1 mean motion resonance between the planets can act as the first mechanism for all stable orbits. The second mechanism is the apsidal alignment and we find that the difference o...

ar X iv : a st ro - p h / 03 02 17 7 v 1 1 0 Fe b 20 03 Polarization in GRB Afterglows

ar X iv : a st ro - p h / 03 02 48 6 v 1 2 4 Fe b 20 03 HD 112914 : A nearby one solar mass binary system

In paper 167 of his serie published in The Observatory, Griffin presented the spectroscopic orbit of HD 112914, a late main sequence star. He also noticed that this star, also known as HIP 63406, was one of the few for which the DMSA/O Annex of the Hipparcos Catalogue derived an orbit prior to any spectroscopic one. Albeit in agreement with each others, the astrometric orbit was however determi...

ar X iv : a st ro - p h / 03 02 30 7 v 1 1 6 Fe b 20 03 The Local Interstellar Spectrum of Cosmic Ray Electrons . Direct measurements

The local interstellar spectrum of cosmic ray electrons is derived by correcting the data from balloon and space measurements for the solar modulation effect. The resulting spectrum, after the renormalization of some experimental data set, can be fitted with a single power law from about 3 GeV to 2 TeV with spectral index γ = 3.42± 0.02. On the other hand, at low energies the measurements by CA...