Orbital studies of terrestrial dust devils would provide a basis for comparative planetology that would broaden the understanding of these dusty vortices on both planets.Lori FentonSETI InstituteDennis ReissSETI InstituteMark LemmonSETI InstituteBéatrice Marticorena...
the angular velocity\omegaof the relative equilibrium satisfying the third Kepler law\omega ^2\rho ^3 = \mu = \mathcal{G }(m_0+m_1+m_2). The elliptic elements(a_j,e_j,v_j,\varpi _j)can be derived from the canonical heliocentric coordinates({\tilde{\mathbf{r}}}_j,\mathbf{r...
VuP, VvP and VwP are the derivatives of the perturbing potential in the directions radial-, along- and cross-track to the orbit, which are obtained from the position and velocity vector of the perturbed and unperturbed orbits in the CRF. From Eqs. (2.2)–(2.4) and the transformation matri...
Although Trojan asteroids have been known for decades in other Solar System planets2such as Venus3, Mars4, Jupiter5, Uranus6, and Neptune7, it wasn’t until 2011 that asteroid 2010 TK7was found to be the first (and hitherto unique) Earth Trojan (ET) asteroid8. ET asteroids have been b...
Asteroids pose a specific gravitational environment, which is different fromterrestrial planets. Asteroids have abnormal shapes, sizes, compositions, spins, and orbits. Their gravity is usually very weak, and perturbations, such as planetary gravity and sunlight pressure, can influence the dynamics of ...
The present work describes the motion of artificial satellites in the terrestrial atmosphere, points out limitations in current orbital-analysis density determinations, synthesizes mathematical solutions to problems connected with density calculation, and describes the behavior of the physical structure of the...
Progress in understanding how terrestrial ice volume is linked to Earth's orbital configuration has been impeded by the cost of simulating climate system p... CS Jackson,AJ Broccoli - 《Climate Dynamics》 被引量: 129发表: 2003年 The Canada-France Ecliptic Plane Survey : First (L3) data rele...
planets in HD160691 nor the five planets in 55 Cnc have eccentricities larger than 0.2. Electronic address: anglada@dtm.ciw.edu, mercedes@dtm.ciw.edu, chambers@dtm.ciw.edu 1 Carnegie Institution of Washington, Department of Terrestrial
The formulation of GMS suggested previously26 did not include VMS. This assumption works well over India, but not over the BoB at millennial timescales. This is due to the different profiles of vertical velocity over India and the BoB. Over India, the vertical velocity is bottom-heavy and ...
Since these results are quite unexpected we investigated in a next step in detail the orbital elements of the planets in xch-e motion and of the perturber P3, to check if the terrestrial planets still perform an xch-e orbit. In Fig. 18 we show the evolution of the eccentricity (left ...