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71.
72.
A time series of zooplankton sampling carried out at Station 18 off Concepción (36°S, 73°W) from August 2002 to December 2003 allowed the study of annual life cycles of the copepods Calanus chilensis and Centropages brachiatus in association with environmental variability in the coastal upwelling zone. Changes in the abundance of eggs, nauplii, and copepodids were assessed from samples taken at a mean time interval of ca. 20 days. Upwelling variability in near-surface waters was reflected in seasonal changes in salinity, water column stratification, and oxycline depth, as well as a weak seasonal signal in sea surface temperature (1-2 °C). Both copepods exhibited similar life cycles, characterized by continuous reproduction throughout the year. Estimates of generation times, as a function of temperature, were 25-30 days for C. chilensis and 27-35 days for C. brachiatus, predicting about 12 and 10 generations a year, respectively. These estimates were consistent with reproduction pulses observed in the field. It was thus suggested that copepods may grow under non-limiting food conditions in this upwelling area. However, despite continuous reproduction, there were abrupt changes in population sizes along with the disappearance of early naupliar and copepodid stages taking place even during the upwelling season (spring/summer). These changes were attributed to sudden increases in mortality taking place in spring or early summer, after which the populations remained at low levels through the fall and winter. It is thus suggested that, in addition to variability in the physical environment, biological interactions modulating changes in copepod mortality should be considered for understanding copepod life cycles in highly productive upwelling systems. 相似文献
73.
N.?Jeremy?KasdinEmail author Pini?Gurfil Egemen?Kolemen 《Celestial Mechanics and Dynamical Astronomy》2005,92(4):337-370
This paper presents a Hamiltonian approach to modelling spacecraft motion relative to a circular reference orbit based on
a derivation of canonical coordinates for the relative state-space dynamics. The Hamiltonian formulation facilitates the modelling
of high-order terms and orbital perturbations within the context of the Clohessy–Wiltshire solution. First, the Hamiltonian
is partitioned into a linear term and a high-order term. The Hamilton–Jacobi equations are solved for the linear part by separation,
and new constants for the relative motions are obtained, called epicyclic elements. The influence of higher order terms and
perturbations, such as Earth’s oblateness, are incorporated into the analysis by a variation of parameters procedure. As an
example, closed-form solutions for J2-invariant orbits are obtained. 相似文献
74.
75.
We present profiles of the line-of-sight (l.o.s.) ionospheric wind velocities in the southern auroral/polar region of Saturn. Our velocities are derived from the measurement of Doppler shifting of the H3+ν2Q(1,0−) line at 3.953 microns. The data for this study were obtained using the facility high-resolution spectrometer CSHELL on the NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawaii, during the night of February 6, 2003 (UT). The l.o.s. velocity profiles finally derived are consistent with an extended region of the upper atmosphere sub-corotating with the planet: the ion velocities in the inertial reference are only 1/3 of those expected for full planetary corotation. We discuss the results in the light of recent proposals for the kronian magnetosphere, and suggest that, in this region, Saturn's ion winds may be under solar wind control. 相似文献
76.
Nikolaos Georgakarakos 《Celestial Mechanics and Dynamical Astronomy》2004,89(1):63-82
In a previous paper, we developed a technique for estimating the inner eccentricity in coplanar hierarchical triple systems
on initially circular orbits, with comparable masses and with well-separated components, based on an expansion of the rate
of change of the Runge-Lenz vector. Now, the same technique is extended to non-coplanar orbits. However, it can only be applied
to systems with I
0 < 39.23° or I
0 > 140.77°, where I is the inclination of the two orbits, because of complications arising from the so-called ‘Kozai effect’. The theoretical
model is tested against results from numerical integrations of the full equations of motion.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
77.
78.
Zhenglu Jiang 《Celestial Mechanics and Dynamical Astronomy》2009,103(1):31-47
In this paper we analyse the relations between a previously described oblate Jaffe model for an ellipsoidal galaxy and the
observed quantities for NGC 2974, and obtain the length and velocity scales for a relevant elliptical galaxy model. We then
derive the finite total mass of the model from these scales, and finally find a good fit of an isotropic oblate Jaffe model
by using the Gauss-Hermite fit parameters and the observed ellipticity of the galaxy NGC 2974. The model is also used to predict
the total luminous mass of NGC 2974, assuming that the influence of dark matter in this galaxy on the image, ellipticity and
Gauss-Hermite fit parameters of this galaxy is negligible within the central region, of radius 0.5R
e. 相似文献
79.
Xufen Wu HongSheng Zhao Yougang Wang Claudio Llinares Alexander Knebe 《Monthly notices of the Royal Astronomical Society》2009,396(1):109-120
We perform a stability test of triaxial models in Modified Newtonian Dynamics (MOND) using N -body simulations. The triaxial models considered here have densities that vary with r −1 in the centre and r −4 at large radii. The total mass of the model varies from 108 to 1010 M⊙ , representing the mass scale of dwarfs to medium-mass elliptical galaxies, respectively, from deep MOND to quasi-Newtonian gravity. We build triaxial galaxy models using the Schwarzschild technique, and evolve the systems for 200 Keplerian dynamical times (at the typical length-scale of 1.0 kpc). We find that the systems are virial overheating, and in quasi-equilibrium with the relaxation taking approximately 5 Keplerian dynamical times (1.0 kpc). For all systems, the change of the inertial (kinetic) energy is less than 10 per cent (20 per cent) after relaxation. However, the central profile of the model is flattened during the relaxation and the (overall) axis ratios change by roughly 10 per cent within 200 Keplerian dynamical times (at 1.0 kpc) in our simulations. We further find that the systems are stable once they reach the equilibrium state. 相似文献
80.
Richard J. Stancliffe Ross P. Church George C. Angelou John C. Lattanzio 《Monthly notices of the Royal Astronomical Society》2009,396(4):2313-2318
There is an apparent dichotomy between the metal-poor ([Fe/H]≤−2) yet carbon-normal giants and their carbon-rich counterparts. The former undergo significant depletion of carbon on the red giant branch after they have undergone first dredge-up, whereas the latter do not appear to experience significant depletion. We investigate this in the context that the extra mixing occurs via the thermohaline instability that arises due to the burning of 3 He . We present the evolution of [C/Fe], [N/Fe] and 12 C/13 C for three models: a carbon-normal metal-poor star, and two stars that have accreted material from a 1.5 M⊙ AGB companion, one having received 0.01 M⊙ of material and the other having received 0.1 M⊙ . We find the behaviour of the carbon-normal metal-poor stars is well reproduced by this mechanism. In addition, our models also show that the efficiency of carbon-depletion is significantly reduced in carbon-rich stars. This extra-mixing mechanism is able to reproduce the observed properties of both carbon-normal and carbon-rich stars. 相似文献