bluuebunny/crossref_metadata_2025 huggingface dataset:
Line formation in turbulent media with finite correlation lenghs. II.
Authors: Stahlberg J.
Published: July 2007

Der Einflüß stochastischer Geschwindigkeitsfelder auf die Linienentstehung wird untersucht. Der Anwendungsbereich der Methode in Teil I wird auf große Korrelationslängen ausgedehnt. Die Methoden für große und kleine Korrelationslängen werden kombiniert um den Charakter der Turbulenze realistischer zu berücksichtigen.

Resultate für diskontinuierliche Geschwindigkeitsfelder werden abgeleitet und mit kontinuierlichen verglichen.
Relationen zwischen Störungen des lokalen Temperaturfeldes und den geodätisch‐astronomischen Beobachtungsresultaten am Astrolab DANJON (Mitteilungen des Zentralinstituts für Physik der Erde, Nr. 955)
Authors: Dittrich J.
Published: July 2007

Die Resultate geodätisch‐astronomischer Zeit‐ und Breitenbestimmungen werden durch äußere, insbesondere mikroklimatische Einflüsse verfälscht. Sie sind bei der Auswertung der Messungen als physikalische Korrelationen zu berücksichtigen oder bei der Messung durch vorbeugende Maßnahmen weitgehend auszuschalten. Im geodätisch‐astronomischen Observatorium Potsdam durchgeführte Untersuchungen zum thermischen Feld am Astrolab DANJON zeigen, daß thermische Anomalien eine Neigung der Isopyknen in unmittelbarer Nähe des Beobachtungsinstrumentes und damit eine Störung der Normalrefraktion hervorrufen. Ein aus Temperaturmessungen hergeleitetes Temperaturmodell dient der Ermittlung horizontaler Temperaturgradienten im Azimut der beobachteten Sterne als Indizien wirksamer Störungen. Sie sind je nach Intensität der thermischen Asymmetrie mehr oder weniger stark mit den geodätisch‐astronomischen Beobachtungsresultaten korreliert und im Falle der Signifikanz entsprechender Korrelationskoeffizienten zur Ermittlung von Korrektionen geeignet.
S 10830 Trianguli – ein interessanter kataklymischer Veränderlicher
Authors: Richter G. A. , Notni P. , Börngen F. , Afanasjev V. , Karachentsev I. D. , Kopylov A.
Published: July 2007

Mit Hilfe von Spaltspektrogrammen, am 6‐Meter‐Teleskop Selenchukskaja und am 2‐Meter‐Teleskop Tautenburg gewonnen, konnte ein kräftiger Helligkeitsausbruch (der einzige bisher bekannte!) spektroskopisch verfolgt werden. Der spektrale Verlauf erinnert an den von SS Cygni, jedoch ist das Vorhandensein hoch angeregter Emissionen (CIII und NIII) untypisch für Zwergnovae. Möglicherweise liegt eine gewisse Verwandtschaft mit der anormalen wiederkehrenden Nova WZ Sge vor. Eine eindeutige Zuordnung zu einem bekannten Untertyp kataklysmischer Veränderlicher kann erst nach Gewinnung umfangreicheren photometrischen Materials erfolgen.
Selection, Statistics and Photometry of Compact Galaxies with Different Instrumental Equipment, Part II. The Cluster Abell 1775
Authors: Richter N. , Schnell A.
Published: July 2007

In Fortsetzung von Teil I unserer Untersuchung wird mit zwei großen photographischen Teleskopen stark verschiedener optischer Konstanten ein Feld von 0.8 in der Nähe des galaktischen Nordpoles auf kompakte Galaxien untersucht. Das Feld enthält den Haufen Abell 1775. Statistik und Photometrie bestätigen die Resultate von Teil I. Der Prozentsatz von optisch kompakten Galaxien bis zur Identifikationshelligkeit 18m9 an der Gesamtheit der Haufengalaxien ergibt sich zu mehr als 30%. Die Daten einer besonderen Standard‐Sternsequenz, die für die Photometrie der Galaxien bestimmt werden mußte, werden mitgeteilt.
Éléments Orbitaux Provisoires des E'toiles Doubles Visuelles ADS 10279 et ADS 12889
Authors: Scardia M.
Published: July 2007

Die Bahnelemente der Doppelsterne ADS 10279 und ADS 12889 wurden bestimmt, sowie die dynamischen Parallaxen und die Gesamtmassen der Systeme berechnet.
Differential Corrections of Comet Orbits
Authors: Buffoni L. , Manara A. , Scardia M.
Published: July 2007

Auf der Grundlage der in den Circularen des Smithsonian Astrophysical Observatory veröffentlichten Beobachtungen wurden korrigierte Bahnelemente von 7 Kometen berechnet.
Dusty KING Spheres
Authors: Fröhlich H.‐E.
Published: July 2007

In order to determine the quantitative influence of small amounts of dust on the luminosity profile of spherical galaxies, we represent an elliptical galaxy by a KING sphere filled with dust. The density of dust particles is assumed to be related to the density of stars according to a simple power law. Assuming that the observed central reddenings in NGC 4874 and NGC 4889 are really caused by dust, we estimate the optical depths in the centres of both galaxies to be about 0.75.
The Interstellar 2200 Å Band: A Catalogue of Equivalent Widths (Mitteilungen der Universitäts‐Sternwarte zu Jena Nr. 151)
Authors: Gürtler J. , Schielicke R. , Dorschner J. , Friedemann C.
Published: July 2007

Using the data of the Ultraviolet Bright‐Star Spectrophotometric Catalogue, the equivalent width of the interstellar absorption band at 2200 Å is derived for 422 stars. A preliminary statistical analysis confirms the good correlation between the equivalent width of the 2200 Å band and the colour excess. The wavelength position of the band centre seems to vary to a small extent.
Physical Processes in Stars on Late Stages of their Evolution
Authors: Bisnovatyi‐Kogan G. S.
Published: July 2007

A review of the physical processes on late stages of stellar evolution and in neutron stars is given. Different types of accretion into black holes are considered. The models of γ‐ray bursts and Cyg X‐1 are discussed briefly.
Einfluß verbesserter Deklinationswerte auf die PZT‐Breiten‐bestimmungen in Potsdam (Mitteilungen des Zentralinstituts für Physik der Erde Nr. 1027)
Authors: Meinig M.
Published: July 2007

Die Ergebnisse der Breitenbestimmungen mit dem PZT in Potsdam in den Jahren 1972–78 wurden verwendet, um die Deklination der beobachteten Sterne zu verbessern. Mit den berechneten Deklinationskorrektionen wurden die Breitenbestimmungen auf das System des neuen Katalogs umgerechnet. Die erhaltenen Ergebnisse zeigen eine wesentlich bessere Übereinstimmung und eine größere Stabilität in bezug auf das BIH‐System als die Ergebnisse im System des bisher verwendeten Sternkatalogs.
New Dwarf Galaxies in the M81/M82 Group
Authors: Börngen F. , Karachentseva V. E.
Published: July 2007

A survey for dwarf galaxies (Sculptor‐type dwarfs) was carried out in the M81/M82 group of galaxies in an area of about 195 sq. degrees by means of Tautenburg 52‐in. Schmidt plates. Eight new faint dwarf galaxies were discovered. Coordinates, linear and absolute dimensions as well as finding charts are given. Results of the photometry will be published in a second article.
Inhomogeneous Cosmological Models Containing Homogeneous Inner Hypersurface Geometry. Changes of the BIANCHI Type.
Authors: Schmidt H.‐J.
Published: July 2007

There are investigated such cosmological models which instead of the usual spatial homogeneity property only fulfil the condition that in a certain synchronized system of reference all spacelike sections t = const. are homogeneous manifolds. This allows time‐dependent changes of the BIANCHI type. Discussing differential‐geometrical theorems it is shown which of them are permitted. Besides the trivial case of changing into type I there exist some possible changes between other types. However, physical reasons like energy inequalities partially exclude them.
Application of a Computer Controlled Intensity Registering Procedure to the Spectral Region at 4430 Å
Authors: Lehmann H.
Published: July 2007

A computer controlled measuring procedure is presented ascertaining intensity courses. The procedure is capable for measurement and storage of the transmittance of photographic spectrograms and for the determination of residual intensities derived from a mean local continum. Residual intensity courses obtained from several spectrograms can be superimposed and correlated with wavelength scale.

The method was applied to eight weakly or not reddened early type stars in order to obtain data on atomic lines in the central part of the diffuse interstellar line at 4430 Å. The results show the general influence of the stellar portion on the central depth and equivalent width of the whole diffuse feature.
Zur kosmologischen Testung des Machschen Prinzips
Authors: Treder H.‐J.
Published: July 2007

The Machian models of isotropic expanding universes according to the “inertia‐free” gravo‐dynamics imply the equations

between the instantan valuesH0andq0of the HUBBLEparameterH, the accelerationq, and the matter density o. Therefore, in Machian universes with linear expansionq0= 0 the energy integralE= ‐1/2ϵc2is zero and the matter density becomes (withH02R02=c2/3)

(f0the Newtonian gravitational constant). This is the critical density in general relativistic cosmology.
Membership of faint stars in the globular cluster M3
Authors: Scholz R.‐D. , Kharchenko N. V.
Published: July 2007

A proper motion study from Tautenburg Schmidt plates is presented for the globular cluster M3 and its vicinity. The plates were scanned with the Automated Photographic Measuring (APM) system in Cambridge (UK). A photographic B,V photometry and star counts on the deepest plates were carried out. With a limiting magnitude of about B = 21.4 proper motions with an accuracy from 2 to 3 mas/yr have been obtained for stars with B 19. The proper motions were determined using a stepwise regression method with 3rd order polynomials in the plate‐to‐plate solutions with about 2000 reference galaxies. The results which were corrected for systematic errors dependent on position and magnitude of the stars were used for the determination of membership probabilities. We also looked for possible internal motions of M3.
Elliptic‐type motion in Fock's gravitational field
Authors: Mioc V.
Published: July 2007

The elliptic‐type motion in the gravitational field found by Fock as exact solution of Einstein's vacuum equations in the case of spherical symmetry (Solution called here Fock's gravitational field) is studied by means of a classic method based on the perturbation theory. Regarding the deviations of the orbit from a Kepleian orbit as perturbations, the first and second order variations of the Keplerian orbital elements over one nodal period as well as those of the nodal period itself are determined.
Brightness variability investigation of BD+61°154
Authors: Chkhikvadze J. N.
Published: July 2007

Photoelectric ubvyHαHβ observations of the Herbig Ae/Be star BD+61°154 are presented. The observational data are analyzed proceeding from the simple hypothesis that the light variation is mainly due to temperature changes of gaseous envelope.
Cosmological constant as integration constant
Authors: Treder H.‐J.
Published: July 2007

Einstein's field theory of elementary particles (Einstein 1919) yields black holes with a mass M ˜ G−1 Λ−1/2c2 and a charge Q ˜ 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−1c3 for this constant defines Planckions and implies “strong gravity”. The choice λ = λ = 3Hinf2c−2 (where Hinf means the Hubble parameter of a final de Sitter cosmos) involves “weak gravity” and describes an electro‐vac spherical universe.
The evolutionary state of magnetic Ap stars
Authors: Hubrig S. , Mathys G.
Published: July 2007

The 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 burning.
Remarks on the period variation of HS Herculis and SW Cygni
Authors: Todoran I. , Agerer F.
Published: July 2007

In 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 corresponding O – C diagram 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 the O–C diagram 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 recommended.
Iron abundance and microturbulence in Arcturus, Canopus, α Cen A, and Sun from FeI and FeII lines
Authors: Gadun A. S.
Published: July 2007

The iron abundance and microturbulent velocities in Arcturus, Canopus, and α CenA have been determined from Fel and Fell lines relative to the Sun. α CenA is found to have an enhanced iron abundance, while Canopus and Arcturus are found to have a deficiency of iron. The behaviour of the determined microturbulent velocities is discussed.
Asteroids observed at the GPO, La Silla
Authors: Debehogne H. , Andreev G. V. , Shefer V. A.
Published: July 2007

Continuing the observational programme, which was started in 1976 at the European Southern Observatory (ESO), La Silla, by Debehogne a lot of new photographic plates was obtained during February‐March in 1989.

These plates are used for the determination of positions of asteroids selected by „Ephemerides of Minor Planets for 1989”︁, edited by the Institute of Theoretical Astronomy of Leningrad (ITA) in 1988. They permit also discoveries of new celestial bodies as well as reidentifications of lost or badly observed asteroids during the last years. For the part treated here, the examination of the plates has revealed nine asteroids not mentioned in the Russian Ephemerides or in the disquettes as fournished by the Minor Planet Centre (MPC) of SAO. Seven were present in the ITA source.
Preliminary orbital elements of minor Planets
Authors: Scardia M. , Ghiringhelli D. , Debehogne H.
Published: July 2007

Preliminary orbital elements of Minor Planets 1985 PT4, 1989 CBI are given. The are based on observations Collected at Eropean Southern Observatory, La Silla, Chile.
The problem of the sighting line stabilization for axial meridian circles
Authors: Lazorenko P. F. , Sergeev A. V.
Published: July 2007

The paper deals with the method based on treating the axial meridian circle and a long‐focus light mark in the prime vertical as a single virtual instrument that has properties of meridian circle. A horizontal axis, a sighting line, and a micrometer cross‐wire of the instrument are created by optical means. The key function here is performed by the light mark that ensures a reference direction used for formation of instrumental principal planes and directions. Stability of instrumental azimuth, inclination, and collimation is expected to be about ±0.″01. Besides, an accuracy of observations is not affected by any temperature and weight deformations of telescope mechanics. Owing to the last circumstance, the design is cheap and the telescope aperture may be increased significantly, to about 1m. An estimate of accuracy of observations depends on the adopted model of image motion, and for sites with excellent seeing and bright stars is ±0.″03 to ±0.″05 (rms).
Synthetic luminosity functions of galaxies in different environments
Authors: Böhm P. , Schmidt K.‐H.
Published: July 2007

Adopting luminosity functions of various morphological types of galaxies and galaxy populations for different environments characterized by the density, the overall differential and integrated luminosity functions of Hubble mix in different dense regions have been obtained. The calculated overall luminosity functions show a weak dependence on the density. Although there is a satisfactory agreement between the calculated overall luminosity functions and the observed distributions of samples of corresponding densities, the observed data are too uncertain in order to confirm the expected density dependence.
Photoelectric observations in a wide‐field area around the Praesepe cluster
Authors: Grankin K. N. , Ibragimov M. A. , Tselishchev I. E.
Published: July 2007

The PPM catalogue numbers, photoelectric magnitudes V, color‐indexes U – B, B – V, V – R and rms errors of their determinations for 51 stars of the secondary wide‐angle photoelectric standard are published. The catalogue accuracy of quantities mentioned above is 0.007, 0.015, 0.006, 0.006 mag, respectively. A list of ten stars which are probably variable is published.
The 10‐year time delay of the solar cycle luminosity modulation of the Sun behind the solar cycle magnetic oscillation
Authors: Yoshimura Hirokazu
Published: July 2007

We found an evidence that the solar cycle luminosity modulation of the Sun deduced from the total irradiance modulation which was measured by the Earth Radiation Budget (ERB) experiment on board of Nimbus 7 from November 16, 1978 to December 13, 1993 was not in phase with the solar cycle magnetic oscillation when we used the sunspot relative number as its index. The modulation was delayed in time behind the solar cycle magnetic oscillation by an amount of about 10.3 years on the order of length of one solar cycle. In order to quantitatively evaluate the correlation between the two quantities, we devised a method to extract characteristics which were proper to a particular solar cycle by defining a new index of the correlation called multiplied correlation index (MCI). We found that the characteristics of the ERB data time profile between solar cycles 21 and 22 were more similar to those of the solar cycle magnetic oscillation between solar cycles 20 and 21 than those between solar cycles 21 and 22 and thus the time profile of the luminosity modulation from the maximum phase of solar cycle 21 to the declining phase of the solar cycle 22 corresponded to the solar cycle magnetic oscillation from the maximum phase of solar cycle 20 to the declining phase of solar cycle 21. We interpret this phenomenon as an evidence that main features of the modulation is not caused by dark sunspots and bright faculae and plages on the surface of the Sun that should instantaneously affect the luminosity modulation but is caused by time‐delayed modulation of global convection by the Lorentz force of the magnetic field of the solar cycle. The delay time of about 10.3 years is the time needed for the force to modify the flows of the convection and to modulate heat flow. Thus the delay time is a function of the strength of the magnetic field oscillation of the solar cycle which is represented by amplitude of the solar cycle. Accordingly, the delay time for other time intervals of the solar cycle magnetic oscillation with different amplitudes can be different from 10.3 years for the interval of the present analysis.
Beobachtungen Kleiner Planeten. XIV
Authors: Börngen F.
Published: July 2007

A summary is given about the Minor Planet survey performed in 1993 on Tautenburg Schmidt plates. 392 asteroids were observed and 1462 positions are calculated for them. These are 297 asteroids with provisional designations (217 of them have new designations) and 95 numbered objects. Ten new designations originate from the KSO‐ARI‐Survey IV. Tautenburg observations could give a tribute to 50 planets numbered in the period of this report. Six Tautenburg asteroids have been numbered (Tab. 3).
Observations of variable stars with the R Coronae Borealis phenomenon and other unique objects
Authors: Rosenbush A. E.
Published: July 2007

The results of photometry and polarimetry of the R Coronae Borealis type stars and other interesting objects are given. The observation of the former objects are obtained at the light maximum or at a brightness lower by 2‐3 mag. The polarization of R CrB stars at light maximum has interstellar origin. The absolute magnitude of V 854 Cen is estimated to Msvw = −3m, and for Y Mus it is Mv > −3m.7. ρ Cas has a variable polarization and is probably a giant (Mv ≅ 0m) rather than a supergiant. Many early stars in its surroundings are photometrically and polarimetrically variable. The protoplanetary star BD −0°3679 has a polarization with the Rayleigh component.
Photometric survey near the Main Galactic Meridian: 1. Photoelectric stellar magnitudes and colours in the UBVR system
Authors: Andruk V. , Kharchenko N. , Schilbach E. , Scholz R.‐D.
Published: July 2007

A catalogue of photoelectric stellar magnitudes and colours in the UBVR Johnson system in 47 sky areas with galaxies near the Main Galactic Meridian is presented. The catalogue includes 1141 stars within the V magnitude interval 4m.5–15m.5. The rms errors are ±0.014, ±0.026, ±0.012, ±0.016 mag for stellar magnitudes V and colours (U – B),(B – V),(V – R), respectively. The catalogue contains accurate equatorial coordinates (α, δ)1950.0, too.
uvbyß photometry of the components of Trapezium‐type multiple systems
Authors: Salukvadze G. N. , Javakhishvili G. Sh.
Published: July 2007

The present paper deals with the results of photoelectric observations of 70 components of 19 Trapezium‐type multiple systems in Strömgren and Crawford six‐colour photometric systems. The trapezia were selected from the Abastumani Catalogue. Observations were carried out with the automatic and computer controlled 125‐cm Ritchy‐Cretien telescope (F = 1590 cm) at the Abastumani Astrophysical Observatory. The results are listed in Table 1. In conformity with the Strömgren criteria the components were ascribed to B, AF and A spectral classes (Table 2). Absolute magnitudes of the components were determined and effective temperatures and gravitational forces on the stellar surface calculated.
About possible geophysical causes of the decade fluctuations in the length of day
Authors: Greiner‐Mai H.
Published: July 2007

Fluctuations in the length of day (Δlod) can be caused by temporal variations of the inertia tensor described by the excitation function and by disturbances of the torque balance between core and mantle. Recent models of the atmospheric excitation of the variations of the lod certainly failed with respect to longer periods (e.g., at about 70 years), but seem to be responsible for the annual period, the 22 years period and for a part of the nearly 30 years period. So, another geophysical phenomenon is needed which is responsible for the remaining part of unexplained lod variations. Previous studies of the geomagnetic core‐mantle coupling were re‐examined using lod values from which atmospherically excited parts were removed. The remaining part of the 30 years period could be explained by core‐mantle coupling. Additionally, the torque blance was realized by assuming lower values of the electrical conductivity at the bottom of the mantle. It was concluded that the consideration of geophysical processes within atmosphere and hydrosphere will be important for future refinements of the core‐mantle coupling models of the decade fluctuations in the lod.
Investigation of PPM catalogue accuracy
Authors: Kharchenko I. N. , Pakulyak L. , Molotaj O. , Tel'nyuk‐Adamchuk V.
Published: July 2007

The PPM catalogue contains the most complete and accurate information concerning positions, proper motions and some astrophysical data for practically all stars (about 379000) down to 10m‐11m over the whole sky. The systems and rms errors of the PPm positions, proper motions, stellar magnitudes and spectral classification are studied by comparison with catalogues of stellar characteristics and on the basis of the PPM data itself. The residual errors of stellar data in the PPM catalogue are small and/or they can be determined and eliminated.
Photographic positions of Minor Planets
Authors: Debehogne H. , Scardia M. , Ghiringhelli D.
Published: July 2007

Photographic precise positions of 16 minor planets obtained with the G.P.O. astrograph at ESO (La Silla, Chile) are given.
On the Variability of RZ Cephei
Authors: Glownia Z.
Published: July 2007

A long series of photoelectric observations of RZ Cep was analysed by two independent methods. The derived period is in good agreement with the suspected lengthening of the period. The secondary variability obtained earlier seems to be spurious.
HALLEY's Comet: Orbital Elements Evolution
Authors: Buffoni L. , Manara A. , Scardia M.
Published: July 2007

Orbital evolution of the elements of the comet Halley are calculated. The changes in the orbital elements are very small and caused by Jupiter's perturbation except in two periods in which are predominant those of Venus and Earth.
Zur Bestimmung absoluter Rektaszensionen und Deklinationen von Sterngruppen mittels Kleiner Planeten
Authors: Landgraf W.
Published: July 2007

A method is given to obtain the absolute positions of stars from observations of a minor planet with small excentricity distributed over a short time and possibly over a geocentric loop in the field traversed by the minor planet.
The Cosmological Problem as Initial Value Problem on the Observer's Past Light Cone: Observations
Authors: Dautcourt G.
Published: July 2007

In a previous paper it was shown how cosmological models can be characterized by few initial data on the observer's past light cone. Part of the inner geometry of the past cone as well as some matter variables taken on the cone (in the simplest case the velocity and density of a cosmological fluid) determine a world model uniquely within the past light cone. Since the initial data to some degree enter the relations between observable quantities such as redshift, luminosity, angular diameter, number counts, distortion parameters and background radiation intensity, it might be possible to determine the required initial data from observations. This problem is discussed in the present article for some observable relatios involving the quantities just mentioned.
On Caustic Diffraction of Scalar Matter in General Relativity
Authors: Paul H. G.
Published: July 2007

The intensity behaviour of gravitationally focused (de‐focused) scalar massive matter φ(xϱ) generating the focusing (defocusing) spacetime via Einstein's equation is investigated in different collapse regions (weak collapse, strong and weak dynamical collapse domain in the region of strong collapse). The dynamical collapse of, in general, non‐geodesic moving matter φ is braked by de‐focusing effects inherent in field theoretic description. If the intensity is greater than definite bounds at significant states, the collapsing matter φ cannot be stopped by de‐focusing caustic diffraction before singular states of matter φ and curvature Rμv are reached; this singularities could be related to the notion physical singularity.
An Upper Bound on Neutron Star Masses
Authors: Kämpfer B.
Published: July 2007

We derive an upper bound on neutron star masses by using model equations of state in the nuclear matter density region and the causality limited equation of state in the ultradense region. Supposing that the model equations of state describe neutron star matter at nuclear matter density correctly we find as bound 3.75 M⊙. For large fiducial densities one gets a maximum mass which is above a previous estimate.
Verbesserung der Sternörter des Potsdamer PZT‐Katalogs (Mitteilungen des Zentralinstituts für Physik der Erde Nr. 1220)
Authors: Meinig M.
Published: July 2007

Aus den Ergebnissen der Zeit‐ und Breitenbestimmungen mit dem PZT in den Jahren 1972–78 wurden neue Rektaszensions‐ und Deklinationskorrektionen für den Potsdamer PZT‐Katalog berechnet. Die korrigierten Sternörter bilden den Katalog PZT 80, der im Anhang gegeben ist. Der Vergleich mit dem vorher verwendeten Katalog PZT 74 zeigt eine Qualitätsverbesserung für den neuen Katalog. Auch die systematischen Abweichungen in bezug auf den Katalog der nördlichen PZT‐Sterne NPZT 74 sind vor allem für die Deklinationen kleiner als beim alten Katalog.
The Diameter of (106) Dione
Authors: Kristensen L. K.
Published: July 2007

The mean diameter D = 147 ± 3 km of (106) Dione is derived from visual observations in Denmark, Germany and the Netherlands of the occultation of AGK3 + 25°0989 on 1983 January 19. Photoelectric magnitudes are: B(1, 2°.4) = 8m.51 ± 0m.06 and B – V = 0m.65 ± 0m.07. The visual albedo is pv = .064. Constraints on the axis of rotation are derived from the observed elliptical contour.
Oscillatory motions in the sun corresponding to the solar cycle
Authors: Tuominen I. , Virtanen H.
Published: July 2007

The mean velocities derived from the proper motions of sunspot groups show a similar behaviour as the torsional oscillation found by HOWARD and LABONTE (1980), and the mean velocities have also a meridional component which changes according to the solar cycle. Calculation of the Lorentz force from a kinematical mean‐field dynamo shows that both of these components are a natural consequence of an α–ω dynamo acting in the solar convection zone.
A numerical study on turbulent heat transfer in convective envelopes
Authors: Arlt K. , Rüdiger G.
Published: July 2007

Via a two‐dimensional temperature equation we numerically attack the well‐known solar heat flux problem. A spherically symmetric heat flux may enter the convection zone at its bottom and leave in accord to the Stefan‐Boltzmann law. Meridional circulation is involved, radiation is still ignored. In order to establish the eddy conductivity tensor for the simplest rotating turbulences a second‐order correlation approximation is used.

The resulting pole‐equator differences vary for various profiles of eddy conductivity and turnover time. They prove to be small only for small stratification or strong outward decrease of turnover time. The fact that we do not observe any latitudinally profiled mean temperature might thus have to do with the real outward drop of the rotational influence on convection.
Long periodic variations of magnetic stars caused by precession
Authors: Gerth E.
Published: July 2007

Long‐time observations give evidence of secular variations of the effective magnetic fields for some Ap stars. These secular variations may be interpreted by a precessional motion of the star. The precession of the rotationally flattened star is assumed to be caused either by the orbital motion of a satellite where the plane of the orbit is inclined to the axis of rotation of the star or by rotation of the inner and outer layers of the star around differently inclined axes.
Magnetohydrodynamical model of pulsar rotation. Exact periodic solutions
Authors: Bogoyavlensky O. I.
Published: July 2007

A rotaing rigid body with elipsoidal cavity filled with magnetic fluid is considered as a pulsar model. Dynamical equations for the pulsar model are derived and investigated, certain integrable cases are indicated. Three–parameter sets of periodic solution integrable in terms of elliptic functions of the time variable are obtained. A formula is derived for the period of rotation and magneto–rotational oscillations of the pulsar.
Are galaxies due to accretion?
Authors: Fröhlich H.‐E.
Published: July 2007

Burnt‐out Population III remnants are thought to have acted as protogalactic seeds. Once tepid pancakes have formed such seeds (≈106 M⊙) could be subject to considerable growing by quasi‐stationary accretion.
Photometrically determined mean surface magnetic fields of Ap stars
Authors: Oetken L.
Published: July 2007

The photometrically determined mean surface magnetic fields BS need a revision. None of the stars for which BS can be measured directly by Zeeman line splitting fulfils the relation between the photometric parameter Δ(V1 – G) and the mean surface field BS, which is used by NORTH, CRAMER and MAEDER to determine BS for other B2 – A3 stars. The ratio BeffMax/BS for stars, which define North's relation, shows unreasonable large values.
Photometric reductions and the lightcurve of (51) Nemausa
Authors: Kristensen L. K. , Gammelgaard P.
Published: July 2007

The lightcurve of (51) Nemausa is determined by 1779 photoelectric observations in B and V and reduction by a rigorous least‐squares method is discussed. For the lost (1026) Ingrid is obtained B(1,0) = 14m.7.
A possible cause of the noncircular pattern of the linear polarization in some (bipolar) reflection nebulae
Authors: Notni P.
Published: July 2007

The scattering of linearly polarized light in reflection nebulae is investigated. The distortion of the centrosymmetric pattern of the polarization vectors is calculated; it is found the linear polarization of the illuminating source in an optically thin nebula leads to an “elliptical” pattern. If foreward scattering angles are strongly favoured, for instance if the nebula is optically moderately thick and light from higher scattering angles is suppressed by extinction, arrays of nearly parallel polarizations may arise. In addition, circular polarisation will always occure. – Both pattern types have been observed in bipolar nebulae. We consider it probable that the investigated mechanism is, at least in part, responsible for these patterns. Detailed modelling of concrete cases is required to finally test whether the proposed mechanism is at work.
General Lagrangian approach to the equations of motion for test particles with internal structure
Authors: Fuchs H.
Published: July 2007

The equations of motion for test particles with internal structure are derived from a general Lagrange principle. The internal structure of the particles is described by sets of unspecified geometric objects, which transform homogeneously both under coordinate and under gauge transformations. Most of the Lagrangian approaches known in the literature are special cases of our general formalism.
On the statistical significance of possible variations in the solar neutrino flux
Authors: Subramanian A. , Lal Siddheshwar
Published: July 2007

A statistical study has been made on the flux of the solar neutrinos as recorded in the experiment of DAVIS et al. to see if there is any evidence for its variation with time. It is found that there are certain correlations and fluctuations in the data which when grouped indicate a pattern of temporal variation. The probability that this pattern of variation would have been caused purely by chance is estimated to be ˜ 10−4.
Beobachtungen Kleiner Planeten. VI.
Authors: Börngen F.
Published: July 2007

Es wird eine Übersicht über die im Jahr 1985 auf Tautenburger Schmidtplatten gefundenen kleinen Planeten gegeben. Es wurden 95 Objekte entdeckt und für sie 168 Positionen gerechnet. Es handelt sich um 20 numerierte Objekte und 75 Planetoiden mit provisorischer Bezeichnung, von denen zwei keine neue Bezeichnung haben. Für zwölf im Berichtszeitraum numerierte Planeten haben Tautenburger Beobachtungen einen Beitrag geleistet. Zwei in Tautenburg entdeckte Planetoiden wurden mit Nummer und Namen versehen: (3245) Jensch = 1973 UL5 und (3338) Richter = 1973 UX5.
Distance law and formation of satellite systems
Authors: Zhong‐Wei Hu , Zhi‐Xiong Chen
Published: July 2007

In the solar system satellite systems of Jupiter, Saturn and Uranus are typical ones. The distribution of the semi‐major axis of satellite orbits in each system may be expressed by an empirical formula corresponding to the Titius‐Bode law. We found that it can be written as an=B′ ·Bn, whereB′ andBare constants. Values ofB′ andBdepend on formation conditions of each system.

Satellites should be formed in the gas‐satellitesimal disk around a planet and by aggregation of satellitesimals. The gas is the major component in the disk and its damping effect must play an important role in the process of aggregation of satellitesimals. It may be proved that radial small perturbation in the disk can cause the gravitational instability and the formation of gaseous rings with increased density, where satellitesimals can easy aggregat into satellites.
Surface distribution of the luminous and early‐type emission stars in the OB Vulpecula associations
Authors: Radoslavova T.
Published: July 2007

The surface distribution of the luminous and early‐type emission stars in a Milky Way region in Vulpecula is obtained. The results show a discrepancy between the places of greatest concentration of such kinds of stars and those indicated in literature as positions of OB associations.
Search for nonpotential features in the magnetic field of the solar active region SD 135 on 1984 June 4
Authors: Linke J. , Peregud N. L. , Selivanov V. L.
Published: July 2007

We investigated the structure of the magnetic field in the relatively small and simple solar active region SD 135/1984 in the early, relatively quiet phase on June 24. For this work we used data of the vector magnetograph of SibIZMIR and results of model calculations using a current‐free approximation.

We have compared the measured magnetic field with the transverse field of the model calculation. We could not find a significant nonpotential effect greater than the level of sensitivity of the transverse magnetic field, BT 200 G. Hence, we conclude that the global magnetic field structure in the investigated solar active region had a nearly potential configuration. The effects of evolution in the active region on the magnetic field structure remained negligible.
Pyroxene glasses — candidates for the interstellar silicate dust component
Authors: Dorschner J. , Gürtler J. , Henning T. H. , Wagner H.
Published: July 2007

Experimental work carried out by Jena University Observatory in collaboration with chemical institutions has shown that pyroxene glasses are very promising candidates for identifying silicate grains in the surroundings of very young objects in molecular clouds, e.g. BN objects and T Tauri stars. The experiments are of importance for gaining optical data that are needed for establishing source models and for understanding the mineralogical status of the grain material. In this paper, steps gone toward both goals in recent work of the Jena dust group are reported.
Mini‐inflation prior to the cosmic confinement transition?
Authors: Boyko V. G. , Jenkovszky L. L. , Kämpfer B. , Sysoev V. M.
Published: July 2007

The onset of the confinement transition in the early universe is studied within the Friedmann model. Exploiting a bag model equation of state for the deconfined matter, which is generalized to include also metastable states, the possibility of a mini‐inflationary epoch is demonstrated. A criterion of metastability is derived to estimate parameters of this mini‐inflation.
The outer core rotation about an inclined axis from geomagnetic secular variations (Mitteilungen des Zentralinstituts für Physik der Erde, Nr. 1832)
Authors: Greiner‐Mai H.
Published: July 2007

Non‐axisymmetric motions of the outer core of the Earth are important for the dynamo problem and the excitation of the decade variations of the polar motion. The components of the vector of a rigid rotation of the outer core about an inclined axis were estimated by a first‐order approximation of the frozen‐ field theory of the geomagnetic secular variation from 1903.5 to 1975.5. The trends and quasi‐periodic constituents of these quantities were computed. It was shown that the position and time behaviour of the rotational pole of the outer core differ considerably from the well‐know co‐ordinates of the dipole axis. Some periods of the equatorial components of the rotational vector are comparable with those of the axial component previously derived for a pure axial rotation. Additionally, the time behaviour of the pole path shows events like the well‐known Markowitz wobble but naturally with other extent. These and other results suggested that the investigations are worth to be continued in future by some physical interpretations.
Treatment of a static spherically symmetric matter distribution on the basis of the projective unified field theory
Authors: Avakian R. M. , Chubarian E. V. , Sarkissian A. V. , Schmutzer E.
Published: July 2007

In order to confront the Projective Unified Field Theory with physical experience it is appropriate to apply this theory also to astrophysical objects, for mathematical reasons in particular to a static spherically symmetric matter distribution as a rough model for a star (e.g. neutron star or another exotic compact object). The problem mentioned is treated here as far as possible analytically in order to prepare the basis for the numerical approach.
Some results of cooperative investigations on solar radio emission with RATAN–600
Authors: Krüger A. , Bogod V. M. , Korzhavin A. N. , Gelfreikh G. B.
Published: July 2007

Results of cooperative work between the GAO/SAO and ZIAP obtained during eight years in the field of solar radio astronomy are reviewed. Main topics of investigation concern the S–component, coronal millimetre–wave sources, and different kinds of microwave bursts.
Astrometry of the comet Wilson (1986 I)
Authors: Scardia M. , Cremonese G.
Published: July 2007

Sixteen astrometric positions of comet Wilson (1986 1) (in the pre‐perihelion phase) obtained during 1986 are presented here. These positions and all the M.P.C. observations have been used to determine a set of orbital elements.
Mutual sensitivity of halo and disk parameters in a two‐component model
Authors: Brosche P. , Caimmi R. , Secco L.
Published: July 2007

The mutual interaction between galactic dark halos and visible matter are explored by modelling a galaxy as two homogeneous, concentric and coaxial spheroidal subsystems, one completely lying within the other. The tensor virial theorem in its extended appropriate form is used and a general method outlined, then an application to the Galaxy is done. The values of equatorial semiaxis and axis ratio of the bright subsystem, and of the velocity components of both subsystems, deduced from a number of known observational data, are used in the computations as input parameters. Discussing the results, special effort has been devoted to the mutual sensitivity of halo and disk parameters which we understand in a twofold manner: 1) numerical interdependence between the present parameters of the visible Galaxy and the ones of dark matter, and 2) dependence of the bright component evolution on the characteristics of the dark halo, in which the former was embedded since the beginning. At present, due to the smallness of dark matter inside the bright disk, the halo‐disk interaction is so weak that few informations can be obtained; consequently, the solutions for dark masses and their axis ratios vary in a large range. Nevertheless, if one demands a spherical and isotropic halo, then from ad = 90 kpc a dark mass Md = 1.5 · 1012 M⊙ results in agreement with other independent estimations. Probably this was not the situation in the past when the disk was bigger and contained more dark mass. The dependence on Md/Mb and εd/εb was likely affecting the star formation rate and in this way contributing to the present morphology of the Galaxy and other galaxies.
The binary system AM Herculis and the parameters of its components
Authors: Götz W.
Published: July 2007

For the variable binary AM Her, which is the proto‐type of a subgroup of cataclysmic stars, revised parameters of the system and its components are given.
Surface photometry of the dwarf galaxy VIIZw009
Authors: Richter G.M. , Schmidt K.‐H. , Thänert W. , Stavrev K. , Panov K.
Published: July 2007

Photographic photometry reveals the dwarf galaxy VIIZw009 as an outstanding object with respect to the large colour excess of its central star burst region. It seems to be a similarity to the system IC 10, which also contains at least one star burst region with large internal extinction. The results are supported by the identification of the IRAS source 3550+6657 with VIIZw009.
Perspectives of advance of RATAN‐600 solar observations
Authors: Gogod V. M.
Published: July 2007

The potential possibilities of RATAN‐600 for solar studies are considered which are going on to be realized during the present maximum of solar activity. Different methods of an improvement of the characteristics of the antenna‐receiver system are analyzed. These are:

– realization of tracking the Sun during about 4 hours for a day and attaining temporal resolution up to some msec, – realization of radio‐heliographic observations,

– realization of a full spectral coverage of the radio telescope from 1,5 to 18 GHz with a frequency reslution up to 1–2 MHz, – combination of all possibilities mentioned above in an adaptable solar observing complex.
New and old arguments to the Eddington‐Lemaǐtre model of the universe
Authors: Liebscher D.‐E. , Treder H.‐J.
Published: July 2007

The interpretation of the Lyman‐α forests of quasars as suggested by Hoell and Priester (1991) supports a Friedmann‐Lemaǐtre model for the universe. The components of the Hubble expansion rate are found by a linear regression of the square of the line‐spacing parameter as a polynomial in the redshift 1 + z with a vanishing linear term. In this essay, we try to restrict the model to the special Eddington‐Lemaǐtre model, which develops the deSitter expansion from the Einstein universe. We show the regression results under this restriction and discuss some of its consequences.
Expanding, homogeneous, ellipsoidal density perturbations. I. The effect of the initial shape at some special stages of evolution
Authors: Caimmi R.
Published: July 2007

This paper investigates the effect of the initial shape of expanding, homogeneous, ellipsoidal density perturbations, at some special stages of evolution, namely at the occurrence of: (i) turn‐around along the axes, (ii) maximum volume, (iii) strong decoupling from the Hubble flow, assumed to take place at overdensities equal to unity. To this aim, previous theory is reviewed and extended involving – among others – a deep analysis on the gravitational force induced on the unit mass at the top axes of the ellipsoid, an explicit expression of the overdensity, and a detailed investigation on the limiting cases of flat (two‐dimensional) and oblong (one‐dimensional) configurations. Then some physical parameters related to the above mentioned stages of evolution are computed for a wide range of initial shapes, in connection with an Einstein‐de Sitter universe and an initial overdensity, which is typical for inhomogeneities with galactic masses in a classical CDM scenario. If the gain of spin by tidal torques grows in proportion to time until either the stage of evolution (i) or (ii), or (iii) is attained, it is found a difference in angular momentum related to the initial shape, which never exeeds a factor of about 3.6, 2.0, 1.4, respectively.