Aspects physionomiques de la végétation halo résistante et halophile du Nord et du Sud de l’Algérie occidentale

On se propose, à travers cette étude de cartographier la végétation halo résistante et halophile de deux zones de l’Algérie occidentale l’une au Nord (région de Hammam Boughrara) et l’autre au Sud (région du Chott El-Gharbi). Une comparaison de ces deux zones d’un point de vue physionomique a été menée, afin de mettre en évidence la diversité phytoécologique de ces peuplements. Les données bioclimatiques montrent que les zones d’étude sont toutes deux caractérisées par une longue période de sécheresse estivale variant de 6 à 7 mois. D’un autre côté, l’approche édaphique montre une texture limono-sableuse à sableuse aussi bien au Nord qu’au Sud. Par contre la salinité est nettement plus accentuée au Sud atteignant 1350 μ.S/cm. La carte physionomique de la végétation de la zone nord fait apparaitre la dominance de formations pures à Tamarix gallica L. (27,13%) ou à Atriplex halimus L. (37,99%), et de formations en mosaïques, où les deux genres se trouvent mêlés (16,87%). Au niveau de la zone sud deux grandes unités physionomiques se distinguent: les groupements à Salsola vermiculata L. (24 %) et les groupements à Lygeum spartum L. (6 %). Les groupements à Artemisia herba– alba Asso. occupent par contre de petites surfaces (2 %) de qualité moyenne à médiocre. Les peuplements à Arthrocnemum glaucum (Del.) Ung. quant à eux, se répartissent tout autour de la daya du Chott El-Gharbi, où la salinité est à son maximum, en constituant un tapis végétal assez dense (1 %).

Total cross sections of nuclei for 280 Mev neutrons.

The measurement of 28O-Mev neutron cross sections of various nuclei is described. The neutron beam used results from 340-Mev protons in the 184-in. cyclotron striking a 2-in. Be target. The neutron detector consists of a double coincidence anthracene scintillation counter telescope which counts recoil protons scattered at 15 deg from a paraffin cylinder placed in the collimated neutron beam. A 2-in. Cu absorber placed between the counters assures that only protons of energy greater than 250 Mev are counted. The cross sections for all nuclei measured from Li to Pb are smaller than the corresponding cross sections measured at 90 Mev by factors between 0.5 and 0.6.

Sifre de-agadeta: ʻal Megilat Ester; halo ̣ hemah ḳevutsat midreshim shonim : Midrash Aba Guriyon, Midrash Panim Aḥarim, Midrash Leḳaḥ Ṭov /

Includes bibliographical references.

Analysis of (n, 2n) cross sections for nuclei of mass A>30 /

"Physics; Reactor technology--TID-4500, 36th ed."

Condensation of vapor as induced by nuclei and ions.

"The contemporaneous variations of the nucleation and the ionization of the atmosphere of Providence, by Lulu B. Joslin": p. 123-154.

Ueber den einfluss von alkylgruppen auf die abspaltung der halo...

Thesis (doctoral)--

Galaxy threshing and ultra-compact dwarfs in the Fornax cluster

We have discovered a new type of galaxy in the Fornax Cluster: 'ultra-compact' dwarfs (UCDs). The UCDs are unresolved in ground-based imaging and have spectra typical of old stellar systems. Although the UCDs resemble overgrown globular clusters, based on VLT UVES echelle spectroscopy, they appear to be dynamically distinct systems with higher internal velocity dispersions and M/L ratios for a given luminosity than Milky Way or M31 globulars. Our preferred explanation for their origin is that they are the remnant nuclei of dwarf elliptical galaxies which have been tidally stripped, or 'threshed' by repeated encounters with the central cluster galaxy, NGC1399. If correct, then tidal stripping of nucleated dwarfs to form UCDs may, over a Hubble time, be an important source of the plentiful globular cluster population in the halo of NGC1399, and, by implication, other cD galaxies. In this picture, the dwarf elliptical halo contents, up to 99% of the original dwarf luminosity, contribute a significant fraction of the populations of intergalactic stars, globulars, and gas in galaxy clusters.

Cluster cannibalism and scaling relations of galactic stellar nuclei

Recently, very massive compact stellar systems have been discovered in the intracluster regions of galaxy clusters and in the nuclear regions of late-type disk galaxies. It is unclear how these compact stellar systems - known as ultracompact dwarf (UCD) galaxies or nuclear clusters (NCs) - form and evolve. By adopting a formation scenario in which these stellar systems are the product of multiple merging of star clusters in the central regions of galaxies, we investigate, numerically, their physical properties. We find that physical correlations among velocity dispersion, luminosity, effective radius, and average surface brightness in the stellar merger remnants are quite different from those observed in globular clusters. We also find that the remnants have triaxial shapes with or without figure rotation, and these shapes and their kinematics depend strongly on the initial number and distribution of the progenitor clusters. These specific predictions can be compared with the corresponding results of ongoing and future observations of UCDs and NCs, thereby providing a better understanding of the origin of these enigmatic objects.

A comparison of surface brightness profiles for ultracompact dwarfs and dwarf elliptical nuclei: implications for the “threshing” scenario

Using imaging from the Hubble Space Telescope, we derive surface brightness profiles for ultracompact dwarfs in the Fornax Cluster and for the nuclei of dwarf elliptical galaxies in the Virgo Cluster. Ultracompact dwarfs are more extended and have higher surface brightnesses than typical dwarf nuclei, while the luminosities, colors, and sizes of the nuclei are closer to those of Galactic globular clusters. This calls into question the production of ultracompact dwarfs via threshing, whereby the lower surface brightness envelope of a dwarf elliptical galaxy is removed by tidal processes, leaving behind a bare nucleus. Threshing may still be a viable model if the relatively bright Fornax ultracompact dwarfs considered here are descended from dwarf elliptical galaxies whose nuclei are at the upper end of their luminosity and size distributions.