Dynamics of rotating triple systems: statistical escape theory versus numerical simulations     

M. Valtonen  A. Mylläri  V. Orlov  A. Rubinov 《Monthly notices of the Royal Astronomical Society》2005,364(1):91-98

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The radial distribution of blue straggler stars and the nature of their progenitors     

M. Mapelli  S. Sigurdsson  F. R. Ferraro  M. Colpi  A. Possenti  B. Lanzoni 《Monthly notices of the Royal Astronomical Society》2006,373(1):361-368

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Extracting star formation histories from medium-resolution galaxy spectra     

H. Mathis  S. Charlot  J. Brinchmann 《Monthly notices of the Royal Astronomical Society》2006,365(2):385-400

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Direct mid-IR images of Gl 2591,W51-IRS2 and S140     

P. Persi  M. Ferrari-Toniolo  A. R. Marenzi  M. Busso  L. Corcione  M. Marengo  M. Tapia 《Astrophysics and Space Science》1995,224(1-2):535-536

We present the results of direct mid-IR images of the luminous young stellar objects GL 2591, S140-IRS1, and W51-IRS2. The sources show an extended mid-IR emission at the limit of our spatial resolution indicating the presence of dense circumstellar dust disks.  相似文献   

Photo—gravitational effects in the two—body problem     

I. Todoran  R. Roman 《Astronomische Nachrichten》1993,314(1):35-38

The effect of the radiation-pressure in the problem of the two bodies is analysed. It is found that such an effect is the same as that of reducing the stellar mass, m, by the factor p (0 ≤ p ≤ 1). The case p < 0 leads to stellar instability and, consequently, it is not considered here. The problem of the mass determination from spectroscopic observations is reviewed and an iterative method is recommended.  相似文献   

Stellar populations and dust in the galaxy NGC 2976, a low-luminosity member of the M81 group     

W. Bronkalla  P. Notni  A. A.-R. Mutter 《Astronomische Nachrichten》1992,313(1):1-20

Photographic UBV photometry of NGC 2976, a low-luminosity member of the central M81 group of galaxies, is presented. Young stars in the central disk determine the optical view and the classification of this Sc(pec) galaxy. It is surrounded by a halo of an old population which contains nearly all the mass and half the luminosity of the system. This halo has some properties typical of spheroidal dwarf galaxies: an exponential brightness profile, an ellipticity trend of the isophotes typical of low-mass systems, and mass and luminosity near the upper limit of typical dwarfs. In the central population I disk, star formation proceeds in dense associations scattered irregularly in a broad ringlike region of 1.2 kpc radius just inside the turnover of the rotation curve. This star formation episode may last since some 10⁸ a; it is possibly triggered by gas infall from the interstellar cloud generated during encounters between other group members in the central M81 group. A direct triggering by recent encounters is excluded since NGC 2976 is undisturbed in its outer parts.  相似文献   

Programme of the Galactic meridian: Star counts and Galactic models 2. Distribution of absolute proper motions     

V. Andruk  N. Kharchenko  E. Schilbach  R.-D. Scholz 《Astronomische Nachrichten》1996,317(1):19-28

A comparison of the observed distribution of absolute proper motions with a kinematical model of the Galaxy is presented. Proper motions with respect to galaxies were obtained for about 40 000 stars along the main Galactic meridian and in two fields near the North Galactic pole (programme MEGA). The Galaxy is considered as composed of the disk (main sequence and disk red giants), the thick disk and spheroid populations. For each subsystem, spatial velocity components and their dispersions were computed. The distribution of kinematical parameters were modelled for stars located in different directions of the Galaxy.  相似文献   

The irregular galaxy Cassiopeia 1 – a new member of the Local group     

N. Tikhonov 《Astronomische Nachrichten》1996,317(3):175-178

A photometry in the V, R, I (Cousins) system has been performed for stars in the galaxy Cassiopeia 1. The resulting colour-agnitude (CM) diagram of Cas 1 reveals the existence of blue stars and the absence of red ones. From an analysis of the CM diagram of the galaxy it is concluded that A_v = 4.0 mag, and the distance modulus (m – M)_o = 24.5 mag, corresponding to a distance of 790 kpc. The visual magnitude of the galaxy is V = 14^m.62 (M_v = −13^m.8) and the colour index (V – R) = 0.89 mag. From the distance determination the galaxy Cassiopeia 1 is a member of the Local group.  相似文献   

A multiple shooting approach for the numerical treatment of stellar structure and evolution     

J. Reiter  R. Bulirsch  J. Pfleiderer 《Astronomische Nachrichten》1994,315(3):205-234

We present a new numerical method for solving the system of partial differential equations describing the structure and evolution of a spherically symmetric star. As usual, we employ the transversal method of lines in order to split the equations into a coupled spatial and temporal part. The novel features of the algorithm are the following: (a) Instead of using the Lagrangian picture we formulate the system of partial differential equations in the Eulerian picture. (b) We reformulate the equations of stellar structure as a multipoint boundary-value problem. By means of this reformulation the rather clumsy iterative matching procedure of stellar atmosphere and interior is avoided. (c) The multipoint boundary-value problem is solved by the multiple shooting method. This approach not only ensures a high accuracy of the stellar models calculated at each time step but also allows the free boundaries inside the star due to different energy transport mechanisms to be located exactly. (d) The time derivatives involved in the stellar-structure equations are discretized implicitly to second order accuracy. Moreover, at each time step, the chemical abundances are determined by using a sophisticated update procedure. In this way, a high accuracy is achieved with respect to the integration in time. The algorithm has turned out to be exceedingly reliable and numerically accurate. This is shown by the evolution of a 1 M_⊙ star up to the hydrogen-shell burning phase. In this example, the virial theorem, the law of mass conservation, and the law of energy conservation is fulfilled to a hitherto unattainable degree of accuracy. Since the multiple shooting method, which is at the heart of our approach, is a perfect example of a parallel algorithm, the computational speed of the algorithm might be substantially improved provided easy-to-program, high-performance parallel computers with sufficiently many processors become available in the near future.  相似文献   

Photographic photometry for stellar statistics with Tautenburg Schmidt telescope     

V. Andruk  N. Kharchenko  E. Schilbach 《Astronomische Nachrichten》1994,315(6):431-437

Photometric properties of deep Tautenburg Schmidt plates in the UBV system over the whole field and over a wide range of stellar magnitudes are discussed. Different reduction models based on the calibration curve alone and with additional terms containing colour and plate coordinates are considered. With the filter-emulsion combinations used the Johnson UBV system can be reproduced quite well by the Tautenburg telescope. The accuracy of photometric data can be improved if geometrical terms are taken into account. For deep plates with a significant effect of background nebulosity a supplementary term is to be included in the reduction model. The polynomial coefficients vary in dependence on spectral bands and individual properties of each plate.  相似文献