%R 1995A&AS..109....1R
%J-7
%A Richtler T.
%T CCD photometry of the globular clusters NGC 6496, NGC 6624, and NGC 6637.
%F 1994.12.20
%B This paper presents the data part of work concerning the age, metallicity, and distance of three globular clusters, which are believed to belong to the disk system of galactic globular clusters, NGC 6496, NGC 6624, and NGC 6637 (M69). Information is given on: the observations, the reduction, the photometric calibration. A new photoelectric sequence around NGC 6496 is presented as well. The present data are compared with previous work. Finding charts as well as recipes for
cross identification are given. Lists containing the brighter stars in the cluster regions are added.
%K globular clusters: individual: NGC 6496, NGC 6624, NGC 6637; general

%R 1995A&AS..109....9G
%J-28
%A Gottwald M., Parmar A.N., Reynolds A.P., White N.E., Peacock A., Taylor B.G.
%T The EXOSAT GSPC iron line catalog.
%F 1994.12.20
%B We report on the global properties of the Fe feature seen in the 6-7keV spectra of X-ray sources observed with the EXOSAT Gas Scintillation Proportional Counter (GSPC). Of a total of 431 spectra extracted from the EXOSAT archive, 205 required the addition of a Gaussian emission line to the continuum spectrum in order to obtain satisfactory fits. The majority of these sources are X-ray binaries. The best fit line properties are given for each of these spectra as well as
being summarized by source class. For the 226 spectra which did not require the addition of an emission feature, upper limit equivalent widths for narrow and broad lines are presented.
%K catalogs; X-rays

%R 1995A&AS..109...29H
%J-69
%A Hambly N.C., Steele I.A., Hawkins M.R.S., Jameson R.F.
%T Very low mass stars in the galactic cluster Praesepe.
%F 1994.12.20
%B In this paper we present the results of a deep proper motion survey of a 19 square degree area of the Galactic open cluster Praesepe. Details of the astrometric and photometric reductions are given, along with the selection process for members. A list of these probable members, along with cross identifications from previous less sensitive surveys, is presented and finder charts given in an Appendix.
%K astrometry - proper motions; clusters - open; stars - low mass

%R 1995A&AS..109...71Z
%J-77
%A Zaninetti L.
%T Dynamical Voronoi tessellation. V. Thickness and incompleteness.
%F 1994.12.20
%B Given a normal Voronoi diagram made by lines/faces we introduce the concept of incompleteness that restricts the number of chosen lines/faces through a random process. After this operation we develop the concept of thickness after which the lines/faces loose their mathematical behavior. The developed techniques are then used to produce isodensity contours in the distribution of the galaxies similar to those deduced from the observations like the QDOT survey or
latitude/longitude slices like those observed at the CFA.
%K methods: numerical - large-scale structure of the Universe

%R 1995A&AS..109...79E
%J-108
%A Espagnet O., Muller R., Roudier T., Mein N., Mein P.
%T Penetration of the solar granulation into the photosphere: height dependence of intensity and velocity fluctuations.
%F 1994.12.20
%B A 16-min time series of two-dimensional "Multichanel Subtractive Double Pass" spectrograms, recorded in the NaD_2_ 5690 line, has been used to study the vertical structure of the photosphere and, in particular, the penetration of granules. A statistical and a morphological investigations have been made. The 5-min oscillations have been carefully filtered in the k-{omega} space. Intensity fluctuations associated to granules disappear in a very short distance, about 60 to
90km above the continuum level. The intensity features in the upper photosphere are not related to the granules. The velocity fluctuations associated to the granulation, cross the whole thickness of the photosphere. The photosphere can thus be separated into two distinct layers, but only for the intensity features, not for the velocity features which are the same from the bottom to the top of the stable atmosphere. In the lower photosphere, below 90km, only granules are
detected. In the upper photosphere, our observations suggest that the weak pattern visible there, is turbulent in origin. In addition to this weak pattern, bright sinking plumes have been discovered; they are associated with strong downflows, often adjacent to strong upflows. The size of most plumes is 1" to 2"; however the most outstanding of them may be as large as 4". Their origin, which may be photospheric or chromospheric, is still unknown.
%K Sun: photosphere; granulation

%R 1995A&AS..109..109G
%J-123
%A Guillot T., Morel P.
%T CEPAM: a code for modeling the interiors of giant planets.
%F 1994.12.20
%B The aim of this paper is to describe the numerical techniques used in the code CEPAM, developed to study the internal structure of giant planets. The main originality of CEPAM is the solution of the two point boundary value problem of the quasi-static equilibrium by a collocation implicit method based on piecewise polynomial approximations projected on a B-spline basis. An automatic mesh refinement is designed to adjust the location of the grid points depending on the
variation in the unknowns. Moreover, a grid point can be adjusted at any determined position. This allows an exact treatment of the problem, even when the first derivatives of the integration variables (M, R, P, T, L) are discontinuous. A robust optimization method allows the calculation of models matching the observed equatorial radius and gravitational moments. The numerical accuracy of the models calculated is found to be satisfactory even with a small number of mesh
points (the relative accuracy is better than 10^-5^ on all the variables with 100 mesh points). The whole precision of models of giant planets is limited by the accuracy of physical data.
%K methods: numerical - planets: individual; Jupiter; Neptune; Saturn; Uranus

%R 1995A&AS..109..125V
%J-133
%A Verner D.A., Yakovlev D.G.
%T Analytic fits for partial photoionization cross sections.
%F 1994.12.20
%B We present a compact, uniform and complete set of analytic fits to the partial Hartree-Dirac-Slater photoionization cross sections for the ground state shells of all atoms and ions of elements from H to Zn (Z<=30). Comparison with experiment and theory demonstrates generally high accuracy of the fits up to energies of 100keV.
%K atomic data - atomic processes

%R 1995A&AS..109..135M
%J-145
%A Montes D., Fernandez-Figueroa M.J., De Castro E., Cornide M.
%T Excess H{alpha} emission in chromospherically active binaries: the spectroscopic survey.
%F 1994.12.20
%B We present new spectroscopic H{alpha} observations for a sample of 24 chromospherically active binary systems (RS CVn and BY Dra classes), of different activity levels. By using the spectral subtraction technique (subtraction of a synthesized stellar spectrum constructed from reference stars of similar spectral type and luminosity class) we obtain the active-chromosphere contribution to the H{alpha} line. The H{alpha} emissions arising from each individual star were
obtained when it was possible to deblend the contribution of both components.
%K stars: activity - stars: binaries: close - stars: chromospheres - stars: late-type - stars: rotation

%R 1995A&AS..109..147B
%J-170
%A Brinkmann W., Siebert J., Reich W., Fuerst E., Reich P., Voges W., Truemper J., Wielebinski R.
%T The ROSAT AGN content of the 87GB 5 GHz survey: bulk properties of previously optically identified sources.
%F 1994.12.20
%B The cross-correlation of the source list from the ROSAT All-Sky Survey with the 5 GHz Green Bank survey yields a list of 2127 objects. About two thirds of them are optically unidentified. The majority of the objects with known optical counterparts are quasars and radio galaxies, most of them detected in X-rays for the first time. In this paper we present a list of the previously optically identified objects with their main characteristics and discuss their general
(bulk) properties. We find strong correlations between luminosities in the radio, optical, and X-ray bands which differ for quasars and radio galaxies. The fraction of flat radio spectrum sources increases with redshift and ~ 95% of all sources above z = 2 are of that type. In the relatively large group of blazars, radio selected BL Lacs and highly polarized quasars show very similar properties while X-ray selected BL Lacs have markedly different X-ray to radio flux ratios.
The sample is large enough and of sufficiently high quality to reveal clearly various detection biases and selection effects which strongly influence the physical interpretation of the correlations. Radio follow - up observations for the determination of the morphological and spectral properties as well as environmental conditions are needed for a statistically reliable study of the sample. The very large group of sources with low radio fluxes remains to be optically
identified.
%K galaxies: active - quasars; X-rays: general - radio sources: general

%R 1995A&AS..109..171F
%J-175
%A Flynn C., Sommer-Larsen J., Christensen P.R., Hawkins M.R.S.
%T A catalog of blue horizontal branch stars in the outer galactic halo.
%F 1994.12.20
%B We present a sample of faint blue stars at medium to high galactic latitude, and classify the stars as blue horizontal branch (BHB) or probable non-BHB stars on the basis of medium dispersion spectra and broadband photoelectric BV photometry. The classification scheme (Flynn et al. 1993) is as accurate as Stroemgren photometry. Using this method we have identified a sample of 100 BHB objects in the galactic halo to faint magnitudes (13.5 < V < 19.5), the selection criteria
ensuring that the sample is the cleanest to date. We analyse the kinematics of the BHB stars in a subsequent paper.
%K stars: horizontal-branch - Galaxy: halo, kinematics and dynamics

%R 1995A&AS..109..177W
%J-179
%A Wendker H.J.
%T Radio continuum emission from stars: a catalogue update.
%F 1994.12.20
%B An updated version of my catalogue of radio stars is presented. Some statistics and availability are discussed.
%K catalogues; stars: general; radio continuum: stars

%R 1995A&AS..109..181C
%J-192
%A Chapront J.
%T Representation of planetary ephemerides by frequency analysis. Application to the five outer planets.
%F 1994.12.20
%B A new type of representation for planetary ephemerides is proposed. Using as a mother ephemeris the result of a numerical integration which has been fitted to observations, an approximation is constructed under the form of Poisson series - a combination of periodic and secular terms -. The significant frequencies of the solution are determined by frequency analysis. The approximation is performed on a finite time interval, few centuries in the case of outer planets. The
secular and Poisson terms absorb either arguments with long periods which are lacking in the analysis or close frequencies. Such a representation has practically been realized with JPL's reference ephemeris DE200, a version which spans 250 years, and also with a numerical integration spanning a much longer time interval - named ME200 - which is an extension of DE200 over 560 years computed with Moshier's numerical tools. The rectangular, heliocentric, equatorial coordinates
of the five outer planets are represented with a precision below 0.004" in the case of DE200 and below 0.02" in the case of ME200, in angular variables. The resulting series are very compact since they contain less than 215 terms - in the worse case of Jupiter - for each coordinate. Solutions are available in electronic form.
%K ephemerides - planets and satellites: general - methods: numerical

%R 1995A&AS..109..193B
%J-197
%A Berrington K.A.
%T Atomic data from the IRON Project. VIII. Electron excitation of the 3d^4^ ^5^D_J_ ground state fine-structure transitions in Ti-like ions V II, Cr III, Mn IV, Fe V, Co VI and Ni VII.
%F 1994.12.20
%B Electron excitation collision strengths for the 3d^4^ ^5^D_J-J'_ ground term fine-structure transitions in titanium-like ions V II, Cr III, Mn IV, Fe V, Co VI and Ni VII are calculated using R-matrix techniques. The model target ion includes all 3d^4^ terms, and the low-energy collision strengths are dominated by autoionizing resonances. The collision strength is averaged over a Maxwellian velocity distribution to obtain effective collision strengths as a function of
electron temperature. To our knowledge, these are the first published data for these processes.
%K atomic data