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We have analysed the 1978 UBV photoelectric observations of the short-period (RS CVn type) binary system RT And, using the rectifiable methods of Russell and Merrill (1952) and Kitamura (1965). The primary minimum is a transit. The solutions allow us to classify the system as a detached one, but a certain disagreement results with respect to solutions of previous epochs. A graphical test of the reliability of the solution is given. 相似文献
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The scenario of magnetohydrodynamic turbulence in connection with coronal active regions has been actively investigated in recent years. According to this viewpoint, a turbulent regime is driven by footpoint motions and the incoming energy is efficiently transferred to small scales due to a direct energy cascade. The development of fine scales to enhance the dissipation of either waves or DC currents is therefore a natural outcome of turbulent models. Numerical integrations of the reduced magnetohydrodynamic equations are performed to simulate the dynamics of coronal loops driven at their bases by footpoint motions. These simulations show that a stationary turbulent regime is reached after a few photospheric times, displaying a broadband power spectrum and a dissipation rate consistent with the energy loss rates of the plasma confined in these loops. Also, the functional dependence of the stationary heating rate with the physical parameters of the problem is obtained, which might be useful for an observational test of this theoretical framework. 相似文献
3.
We have analyzed the existing photoelectric light curves of twoK-type binary systems: UU Cnc, with a period of about 100 days, and VZ Psc, with a period of about 6 hours. Both show a large overcontact (38% for UU Cnc, 56% for VZ Psc) and a large temperature difference between components (T1500 K and 1100 K, respectively). In the case of VZ Psc, the variability is due only to the non-spherical shape, i.e., no eclipse occurs, but the determination of the photometric solution is made possible by the existence of a spectroscopic mass ratio. We find that UU Cnc is now probably undergoing Case C mass transfer in a dynamical time-scale, with the mass ratio reversal having already occurred; the system is in contact, and is likely to evolve to a 100% filling factor, that is the so-called pre-common envelope phase, a unique case never observed before. The situation for VZ Psc is more uncertain, but a similar, although not identical, possibility exists.Associated with the Istituto Nazionale Fisica Nucleare, Italy.On leave from N. Copernicus Astronomical Center, Polish Academy of Sciences, Warsaw, Poland. 相似文献
4.
An analysis of the spatial distribution of the seismicity of the southern Tyrrhenian Sea is presented with the aim of putting constraints on the geometry of the complex Benioff zone of this area by relocating the earthquakes that occurred in the period 1985–1990. The data set used in this analysis is based on information from ING, ISC, and NEIS databases.
In order to ensure the quality of epi/hypocentral locations, we based our selection of earthquakes on both the available number of P- and S-readings (at least eight P- and two S-pickings) and the epicentral distances of the stations reporting the event (< 5°). Such a selection enabled us to obtain a catalogue of 450 well-located events with focal depths of up to 500 km.
The seismogenetic volumes estimated from the distribution of hypocentres of the whole seismicity analysed were interpreted according to a recent geodynamic model proposed for this area. This has led us to the hypothesis of an active NW-SE-oriented subduction of the lithosphere generated and stressed by the opening of the Tyrrhenian Basin. 相似文献
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L. Milano S. Mancuso A. Vittone A. D'Orsi S. Marcozzi 《Astrophysics and Space Science》1986,124(1):83-100
From the observed light curves of six eclipsing binaries with solar-type activity and from the analysis of their period variations some problems in the interpretation of the observations came out: Are these binaries similar to classical RS CVn stars? Is the stellar surface spot coverage the unique interpretation of the observed light curves? Are these systems really linked with W UMa's? In a further study some models will be tempted to try to solve these problems. 相似文献
7.
TheV andB light curves of three Algol-type eclipsing binaries (UZ Cyg, VW Cyg, AQ Peg), observed by Ammanet al. (1979), have been analysed using the Wilson and Devinney (1971) model. We find that all of them are semi-detached systems, with A-type primary components and K-type evolved secondary which fill the corresponding lobe, although VW Cyg should perhaps be considered as an sd-d system. 相似文献
8.
R. Burchi D. Chochol A. Dipaolantonio S. Mancuso L. Milano A. Vittone 《Astrophysics and Space Science》1983,89(2):387-393
We present three colour photoelectric observations of CI Cyg during the 1980 eclipse. Some interesting photometric peculiarities are shown that must be taken into account for a theoretical model of this eclipsing symbiotic star. 相似文献
9.
The V light curve of CW Cas, observed during 1972, has been analysed by different methods of solution. The results show great differences between rectifiable and direct methods. 相似文献
10.
The observed minima of RT Persei up to 1971 are collected and treated by the method of least squares to establish periodic terms with a fundamental period of 40y0 and, furthermore, a quadratic term. It is shown that the periodic terms might be explained by the presence of a third body, but this hypothesis seems unlikely, and could be definitively ruled out by new spectroscopic observations. A dynamical instability of the system may constitute a more likely explanation of the observed period changes. 相似文献