Observation of outer planets at Lyman alpha

A triple planetary observation in one IUE shift was conducted to measure the Lyman alpha reflectivity of Jupiter, Saturn and Uranus. The exposures were planned to take account of the light travel times, Sun to planet and planet to Earth, in order to assess the response of the three atmospheres to essentially the same incident solar flux. All additional uncertainties that were introduced when different instruments were used for such a comparative measurement were automatically eliminated

Correlations between environmental parameters and nuclear activity

The occurrence and quantitative properties of Seyfert 1 and Seyfert 2 galaxies as a function of the galaxy environment were studied in a systematic way. For this investigation the authors selected from the Catalogue of Quasars and Active Nuclei (Veron & Veron, 1989) all Seyfert galaxies with the following properties: (1) m sub V less than or equal to 15; (2) listed classification as Sey 1, Sey 2, or Sey 3; (3) v sub rad less than or equal to 20,000 km s(sup -1). This results in a sample size of 242 Seyfert galaxies. For all these objects their galaxy environment was inspected on plates. The vicinity of each sample Seyfert galaxy was searched for companion galaxies out to at least 0.5 Mpc. Lacking redshift information, the authors adopted as a companion galaxy any galaxy in this area having a size between 20 and 200 percent of the Seyfert galaxy size. As an important environmental parameter for Seyfert activity, the authors consider the galaxy density within an environment of 500 kpc radius. They distinguish four density classes: D1: no companion (isolated Seyfert); D2: 1 companion; D3: 2 to 5 companions (group); and D4: less than or equal to 6 companions (dense group). The distribution of the various Seyfert classes among these density classes is listed in tabular form, both in absolute numbers and in percentages (given in brackets). From these statistics the environments of Sey 1, Sey 2, and Sey 3 galaxies do not differ in general with the exception that among the isolated galaxies the Seyfert 1 galaxies dominate conspicuously. No significant dependence of morphological type (de Vaucouleurs T-type) on density class is observed both for Sey 1 and Sey 2 galaxies. On the basis of an extensive search of the Seyfert literature the authors also investigated the dependence of the intrinsic parameters of the sample Seyfert galaxies on density class

Masses and Radii of the Nuclei with N>=Z in an Alpha-Cluster Model

In the framework of a recently developed alpha-cluster model a nucleus is represented as a core (alpha-cluster liquid drop with dissolved excess neutron pairs in it) and a nuclear molecule on its surface. From analysis of experimental nuclear binding energies one can find the number of alpha-clusters in the molecule and calculate the nuclear charge radii. It was shown that for isotopes of one Z with growing A the number of alpha-clusters in the molecule decreases to three, which corresponds to the nucleus 12C for even Z and 15N for odd Z, and the specific density of the core binding energy \rho grows and reaches its saturation value. In this paper it is shown that the value \rho=2.55 MeV/fm^3 explains the particular number of excess neutrons in stable nuclei.Comment: 7 pages, 3 eps figures, submitted as a contribution to the Proceedings of the International Conference, Messina, Italy, October 5-9, 200

Improved transport equations including correlations for electron-phonon systems. Comparison with exact solutions in one dimension

We study transport equations for quantum many-particle systems in terms of correlations by applying the general formalism developed in an earlier paper to exactly soluble electron-phonon models. The one-dimensional models considered are the polaron model with a linear energy dispersion for the electrons and a finite number of electrons and the same model including a Fermi sea (Tomonaga-Luttinger model). The inclusion of two-particle correlations shows a significant and systematic improvement in comparison with the usual non-Markovian equations in Born approximation. For example, the improved equations take into account the renormalization of the propagation by the self-energies to second order in the coupling.Comment: 20 pages, 15 Postscript figures, uses RevTeX, to be published in: Annals of Physics (N.Y.