摘要:

AbstractEinstein's field theory of elementary particles (Einstein 1919) yields black holes with a massM˜G−1Λ−1/2c2and a chargeQ˜G−1/2λ−1/2c2, their curvatu re radius is Λ−1/2. Here 4Λ is an integration constant of Einstein's ‘trace‐less’ gravitation equations.The choice λ =G−1h−1c3for this constant defines Planckions and implies “strong gravity”. The choice λ = λ = 3Hinf2c−2(whereHinfmeans the Hubble parameter of a final de Sitter cosmos) involves “weak gravity” and descr

ISSN:0004-6337    

DOI:10.1002/asna.2103150502

出版商:WILEY‐VCH Verlag    

年代:1994

数据来源: WILEY

摘要:

AbstractThe analysis of all the available data between 1968 and 1991 on rapid variability of optical and X‐ray luminosity of three AGNs, NGC 3516, NGC 4151 and 3C 273, shows the presence of small‐amplitude (˜ 1 %) but statistically confident (≈︁ 5s̀) periodicity of 160.0105 (± 6) min. Within the error limits it coincides with the periodP0= 160.0101 (± 1) min of global oscillations of the Sun. An independence of the observed period on AGN red shiftzfavours the hypothesis about a cosmological origin of the 160min

ISSN:0004-6337    

DOI:10.1002/asna.2103150503

出版商:WILEY‐VCH Verlag    

年代:1994

数据来源: WILEY

摘要:

AbstractThe characteristics of two stars, 25 Sex and HD 21699, as additional candidates for the sample of magnetic stars belonging to superclusters, are discussed. For 25 Sex, which was already accepted as a probable member of the Hyades supercluster in a previous study, arguments supporting the view that this star indeed is a magnetic star are presented. In the case of HD 21699, the radial velocity derived from our observations is not inconsistent with membership. But from the determinations of its proper motion found in the literature, this star cannot be regarded as a probable member of the α Per cluster. On the basis of recent evolutionary models, all the well established Ap cluster members appear to be close to the end of their main‐sequence life. This suggests that A stars possibly become magnetic at the end of core hydrogen burni

ISSN:0004-6337    

DOI:10.1002/asna.2103150504

出版商:WILEY‐VCH Verlag    

年代:1994

数据来源: WILEY

摘要:

AbstractIn order to get a satisfactory understanding of the periodic variation of the orbital period in the binary system HS Herculis, the study of this problem is resumed. Using recently observed primary and secondary minima, it is evident that after 1955 (E>‐2000) the correspondingO – Cdiagram reflects the effect of apsidal motion. Any assumption on the presence of a third body is rejected, at least as long as the current aspect of theO–Cdiagram is concerned. For the interpretation of the sinusoidal period variation of the semi‐detached system SW Cygni, 130 primary minima were compiled form the literature. Though it is considered as very likely that this variation of the period is primarily caused by apsidal motion, the hypothesis of a third body is analysed too. Further precise photometric and spectroscopic observations are reco

ISSN:0004-6337    

DOI:10.1002/asna.2103150505

出版商:WILEY‐VCH Verlag    

年代:1994

数据来源: WILEY

摘要:

AbstractAnalytical expressions were derived for the expectation of the autocorrelation function (ACF) corresponding to lowfrequency least squares fits and deviations from them in the case of a limited number of observationsN. A vector of values of the autocovariation function may be obtained by multiplication of aN . NmatrixZ(dependent on concrete basic functions used for trend determination) by a vector of the unbiased ACF. Because much computational time is needed to obtain such a matrix, its components are to be computed once for concreteNand basic functions, and then stored as a file. An algorithm is proposed for determining the contribution of the correlated signal to the ‘signal+noise’. The expressions are written for general form of the ACF, and illustrated by the application to autoregressive models. The statistical properties of the model parameters are studied. The method is applied to cataclysmic binaries AM Her and TT Ari. The precise expressions allow us to obtain reliable results and to avoid misinterpretation being possible when using the approximate meth

ISSN:0004-6337    

DOI:10.1002/asna.2103150506

出版商:WILEY‐VCH Verlag    

年代:1994

数据来源: WILEY

摘要:

AbstractWe found an evidence that the luminosity of the Sun systematically decreased about 20 days before sunspot surface appearance by analysing time‐lag correlation of time derivatives of running mean time profiles of the data of the Active Cavity Radiometer Irradiance Monitor (ACRIM) I experiment on board of Solar Maximum Mission (SMM) and of the data of the daily sunspot number. This indicates that sunspot flux tube cooling and heat transport blocking by the flux tubes start to take place in the interior of the solar convection zone well before the sunspot surface appearance. From this finding and our previous finding that the luminosity of the Sun systematically increased and the blocked heat appeared on the surface about 50 days after the sunspot surface appearance, a new view of sunspot formation and dynamics and a new view of the luminosity modulation emerged. (i) Sunspots of a solar cycle are formed from clusters of flux tubes which can be seen in the running mean time profile of the sunspot number as a peak with duration on the order of 100 to 200 days. (ii) Heat flow is blocked by the cluster of sunspot flux tubes inside the convection zone to decrease the luminosity about 20 days before the surface emergence of the sunspot cluster. (iii) The blocked heat appears on the surface about 50 days after the surface emergence of the cluster of sunspot flux tubes to heat up the surface. This appears as a thermal pulse in the running mean time profile of the ACRIM dat in between the peaks of the sunspot running mean time profile. This process of heating the surface makes the temperature gradient less steep and weakens the buoyancy of sunspot flux tubes below the surface. (vi) The radiative cooling of the surface layer by the excess heat release steepens the temperature gradient so that the buoyancy of the sub‐surface magnetic flux tubes becomes stronger to cause the next surge of emergence of a cluster of sunspots and other magnetic activities, which creates a peak in the time profile of the sunspot number. We call this peak a magnetic pulse of the Sun and the coupled process of alternating pulsed appearance of heat and sunspots the magneto‐thermal pulsation of th

ISSN:0004-6337    

DOI:10.1002/asna.2103150507

出版商:WILEY‐VCH Verlag    

年代:1994

数据来源: WILEY

摘要:

AbstractHα profiles of chromospheric spicules computed for a variety of rotational behavior are compared with an observed profile, which was derived by averaging 11 Hα profiles taken near times of maximum spicule intensity. If turbulent velocity is small or equals zero, calculated profiles are in good agreement with the observed one under the conditions that rotation is non‐rigid (faster rotation further away from the axis of the spicule) and the source function decreases in the direction from the spicule axis to the periphery. The comparison of calculated and observed tilts of spicule spectra relative to the direction of dispersion seems to corraborate the non‐rigid character of spicular rot

ISSN:0004-6337    

DOI:10.1002/asna.2103150508

出版商:WILEY‐VCH Verlag    

年代:1994

数据来源: WILEY

ISSN:0004-6337    

DOI:10.1002/asna.2103150509

出版商:WILEY‐VCH Verlag    

年代:1994

数据来源: WILEY

ISSN:0004-6337    

DOI:10.1002/asna.2103150501

出版商:WILEY‐VCH Verlag    

年代:1994

数据来源: WILEY