Evolution of binary stars and the effect of tides on binary populations

We present a rapid binary-evolution algorithm that enables modelling of even the most complex binary systems. In addition to all aspects of single-star evolution, features such as mass transfer, mass accretion, common-envelope evolution, collisions, supernova kicks and angular momentum loss mechanisms are included. In particular, circularization and synchronization of the orbit by tidal interactions are calculated for convective, radiative and degenerate damping mechanisms. We use this algorithm to study the formation and evolution of various binary systems. We also investigate the effect that tidal friction has on the outcome of binary evolution. Using the rapid binary code, we generate a series of large binary populations and evaluate the formation rate of interesting individual species and events. By comparing the results for populations with and without tidal friction, we quantify the hitherto ignored systematic effect of tides and show that modelling of tidal evolution in binary systems is necessary in order to draw accurate conclusions from population synthesis work. Tidal synchronism is important but, because orbits generally circularize before Roche lobe overflow, the outcome of the interactions of systems with the same semilatus rectum is almost independent of eccentricity. It is not necessary to include a distribution of eccentricities in population synthesis of interacting binaries; however, the initial separations should be distributed according to the observed distribution of semilatera recta rather than periods or semimajor axes.     

An Attempt to Integrate Reflection Seismics and Balanced Profiles

—Different techniques in Geophysics and Geology are used to derive the structure of the subsurface. They are based on different data sets, i.e., seismic and geological data, and a combination of these techniques should produce better earth models. The case study presented in this paper is based on data of the German Continental Reflection program (DEKORP) collected in the Münsterland basin and the Rhenish Massif located at the northern border of the Rhenohercynian fold and thrust belt of the Mid-European Variscides. In this study we present an attempt to integrate balanced profiles, i.e., structural geology, and reflection seismics. The integration is performed by synthetically modelling seismic waves according to the acquisition of the field data, where the velocity model is based on the balanced profile. The synthetic data are compared with the field observations. Differences between observed data and field data are either caused by velocity errors in the model or by errors in the balanced profile. Criteria are developed to interpret these differences in order to improve the joint model of geologists and geophysicists. The case study presented in this paper shows that the combination of balanced profiles and reflection seismics may lead to shortcuts in the determination of seismic velocities of the subsurface. These shortcuts can reduce processing times and processing costs of reflection seismic data.     

Zur Rekonstruktion der Geosynklinalgeschichte mit Hilfe von Inkohlungskurven (am Beispiel Ebbeantiklinorium,Rheinisches Schiefergebirge)

It is proposed to determine certain aspects in the development of a geosyncline by constructing the gradient of coalification. The analysis provides important hints as to the degree of erosion (≈ postorogenic uplift — heigh above sea level), the total thickness of the geosynclinal sediments and the geosynclinal heat flow, which can all be partly evaluated. The application of the proposed method to the Ebbe anticline (Rheinisches Schiefergebirge) produces some interesting results; close relations are recognised between the geosynclinal development and the tectonic structure of the anticline and the surrounding synclines. The Ebbe anticline, former zone of relatively lesser subsidence with elevated heat flow and largest uplift is regarded as a model case for the northeastern Schiefergebirge (and other, similarly built mountains?).     

Stellar evolution models for Z = 0.0001 to 0.03

We have calculated a grid of empirically well tested evolutionary tracks with masses M between 0.5 and 50 M⊙, spaced by approximately 0.1 in log M , and with metallicities Z  = 0.0001, 0.0003, 0.001, 0.004, 0.01, 0.02 and 0.03. We use a robust and fast evolution code with a self-adaptive non-Lagrangian mesh, which employs the mixing-length theory but treats convective mixing as a diffusion process, solving simultaneously for the structure and the chemical composition. The hydrogen and helium abundances are chosen as functions of the metallicity: X  = 0.76 − 3.0 Z Y  = 0.24 + 2.0 Z .   Two sets of models were computed, one without and one with a certain amount of enhanced mixing or 'overshooting'. This amount has been empirically chosen by means of various sensitive tests for overshooting: (1) the luminosity of core helium burning (blue loop) giants of well-known mass, (2) the width of the main sequence as defined by double-lined eclipsing binaries with well-measured masses and radii, and (3) the shape and implied stellar distribution of isochrones of various open clusters. The first two tests have been the subject of previous papers, the third test is discussed in this paper. On the basis of these tests, we recommend the use of the overshooting models for masses above about 1.5M ⊙.   We describe here the characteristics of the models, the procedure for constructing isochrones for arbitrary age and metallicity from the models, and the performance of these isochrones for several intermediate-age and old open clusters. All original models are available in electronic form and we describe the means by which they may be obtained.     

Gondwana break-up and the northern margin of the Saxothuringian belt (Variscides of Central Europe)

At the northwestern edge of the Hercynian Bohemian Massif (Saxothuringian belt) new U-Pb zircon age data from rift-related magmatic rocks indicate that the initiation of Gondwana break-up in this area started during the Middle to Upper Cambrian. Magmatic rocks from a bimodal, MORB- to within-plate volcanic sequence in the Vesser area are dated between ca. 517 and 501 Ma. The volcaniclastic sequences analysed exhibit basal layers of conglomerates and mature sandstones, which can be correlated with a widespread Gondwana-derived onlap horizon of an uppermost Cambrian/Tremadocian age that links the Vesser area with the Saxothuringian continental basin. The association of the Vesser rocks with the Saxothuringian terrane as part of the Armorican terrane assemblage is further demonstrated by a coeval magmatic development and by identical detrital components which are derived from a common Cadomian basement (white mica with a ca. 539 Ma K-Ar minimum age and inherited zircon signatures). The Vesser unit, situated between the NW margin of the Saxothuringian zone and the Mid-German Crystalline Zone, probably represents a N-facing remnant of an ocean-continent transition of the, or within the, Armorican terrane assemblage and involves sections of the early break-up process at the peri-Gondwanan shelf south of the Rheic ocean.     

Direct N-body modelling of stellar populations: blue stragglers in M67

We present a state-of-the-art N -body code which includes a detailed treatment of stellar and binary evolution as well as the cluster dynamics. This code is ideal for investigating all aspects relating to the evolution of star clusters and their stellar populations. It is applicable to open and globular clusters of any age. We use the N -body code to model the blue straggler population of the old open cluster M67. Preliminary calculations with our binary population synthesis code show that binary evolution alone cannot explain the observed numbers or properties of the blue stragglers. On the other hand, our N -body model of M67 generates the required number of blue stragglers and provides formation paths for all the various types found in M67. This demonstrates the effectiveness of the cluster environment in modifying the nature of the stars it contains, and highlights the importance of combining dynamics with stellar evolution. We also perform a series of N =10 000 simulations in order to quantify the rate of escape of stars from a cluster subject to the Galactic tidal field.