A new calibration of Wesselink's correlation for the determination of stellar radii

By means of a new homogeneous set of data from 34 double-lined detached systems, we have recalibrated the colour-surface brightness correlation in the interval –0.3(B-V)_o0.95. A comparison is made with Wesselink's calibration. We find that Wesselink's method can provide a good estimate of the stellar radii.     

85 Peg A: what age for a low-metallicity solar-like star?

We explore the possible evolutionary status of the primary component of the binary 85 Pegasi, listed as a target for asteroseismic observations by the MOST satellite. In spite of the assessed 'subdwarf' status, and of the accurate distance determination from the Hipparcos data, the uncertainties in the metallicity and age, coupled with the uncertainty in the theoretical models, lead to a range of predictions on the oscillation frequency spectrum. Nevertheless, the determination of the ratio between the small separation in frequency modes, and the large separation as suggested by Roxburgh, provides a very good measure of the star age, quite independent of the metallicity in the assumed uncertainty range. In this range, the constraint on the dynamical mass and the further constraint provided by the assumption that the maximum age is 14 Gyr limits the mass of 85 Peg A to the range from 0.75 to  0.82 M_⊙  . This difference of a few hundredths of a solar mass leads to well detectable differences both in the evolutionary stage (age) and in the asteroseismic properties. We show that the age determination which will be possible through the asteroseismic measurements for this star is independent either of the convection model adopted or the microscopic metal diffusion. The latter conclusion is strengthened by the fact that, although metal diffusion is still described in an approximate way, recent observations suggest that real stars suffer a smaller metal sedimentation compared with the models.     

An instrument for commissioning the active and adaptive optics of modern telescopes: the Infrared Test Camera for the Large Binocular Telescope

We describe the design, integration, and operation of the infrared test cameras for the commissioning of the Large Binocular Telescope. The design and construction phase lasted slightly more than one year from February 2007 to April 2008 and was the result of a joint collaboration among INAF Osservatorio Astronomico di Bologna, Università di Bologna Dipartimento di Astronomia (Italy) and the Max-Planck-Institut für Astronomie (Heidelberg, Germany). Thereafter, the camera was delivered to the LBT Observatory (USA) for commissioning of the telescope active optics and, more recently, for commissioning of the first light adaptive optics.     

On the interpretation of white dwarf spectra

Following the line of research outlined by Strittmatter and Wickramasinghe (1971) and recently by Shipman (1972), attention was drawn to the study of convective zones in white dwarfs for various masses and chemical compositions, in order to understand some observational features of their spectra. According to the results, convection strongly depends on the mass of the star, forM<0.5 M_⊙, and low hydrogen abundancesX?0.2) are sufficient to decrease the extension of the He-convection zones with respect to pure-He models. It is shown that the existence of DB white dwarfs seems not in agreement with the accretion rates predicted by Bondi (1952), and that DB's must evolve into H-lacking white dwarfs.     

Polymorphism of As4S3 (tris-(μ2-sulfido)-tetra-arsenic): accurate structure refinement on natural α- and β-dimorphites and inferred room temperature thermodynamic properties

An accurate structure refinement, using single-crystal X-ray diffraction data, on natural α- and β-dimorphites collected at Solfatara di Pozzuoli, in the Phlegraean Fields, near Naples and at Vesuvius (Italy) is reported. Theoretical calculations at various levels of sophistication have been used to calculate molecular vibrational frequencies and gas-phase specific heats, to analyze the crystal packing, and to estimate lattice energies of both phases. All computational methods contribute to demonstrate that the β-phase is the thermodynamically stable one at room temperature.     

Cooling sequence of a pure helium white dwarf of 0.15 solar masses

A new method of integration has been performed and applied to the computation of the cooling sequence of a 0.15M white dwarf consisting of helium. The results are discussed and compared with the previous ones obtained by other authors.

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Riassunto E' stato elaborato un nuovo metodo di integrazione numerica, ed applicato al calcolo della sequenza evolutiva di raffreddamento di una nana bianca di puro elio di 0.15M . I risultati vengono discussi e confrontati con i precedenti modelli ottenuti da altri autori.

     

Luminosity and mass functions for low main-sequence stars

The luminosity function derived for main sequence stars in the neighbourhood of the Sun shows evidence for a flattening in the interval 5≲M _v ≲8. An interpretation of this feature by means of theoretical models enables us to deduce the mass function for stars belonging to the main sequence.

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Sommario Viene ricavata la funzione di luminosità per stelle di sequenza principale vicine al Sole. Si evidenzia un pianerottolo per 5≲M _v ≲8. II confronto con i modelli teorici consente di desumere la funzione di massa della sequenza principale.

     

Synthetic integrated fluxes and colours for elliptical galaxies

Photometric intergrated colours (UBVRI+UV selected bands) of elliptical galaxies are theoretically evaluated, accounting for stellar populations of different metal abundance (0.00001Z0.04). The contribution of different evolutionary phases (from M.S. up to Post-A.G.B.) to the integrated fluxes in the various photometric bands is computed. An explanation for the UV-excess in elliptical galaxies and of its dependence on the metallicity (Mg₂) and mass is also suggested.     

Chemical and physical properties of nearby population I stars

An analysis of some photometric and kinematic data for nearby Population I stars has been carried out. The main results show that a good correlation exists between the dynamic state and age; but a non-negligible chemical inhomogeneity seems to be present in the disk, independently of the age.     

Parascandolaite,KMgF3, a new perovskite-type fluoride from Vesuvius

The new mineral parascandolaite, isotypic to cubic perovskites, space group Pm \(\overline{3}\) m (no. 221) is the natural analog of the synthetic fluoride KMgF₃ and is related to neighborite, NaMgF₃. It was found as a volcanic sublimate at Vesuvius volcano on 1944 eruption lava scoria, associated with opal, cerussite, mimetite, phoenicochroite and coulsellite. It occurs as transparent colorless to white cubic crystals up to 0.5 mm in length with vitreous luster. The density measured by flotation in a diiodomethane–toluene mixture is 3.11(1) g/cm³; that calculated from the empirical formula and single-crystal X-ray data is 3.123 g/cm³. The mineral is isotropic with n = 1.395(5) (580 nm). The six strongest reflections in the X-ray powder diffraction pattern are: [d _obs in Å(I)(h k l)] 2.001(100)(2 0 0), 2.831(83)(1 1 0), 2.311(78)(1 1 1), 1.415(56)(2 2 0), 1.633(35)(2 1 1) and 1.206(22)(3 1 1). The unit-cell parameter is a = 4.0032(9) Å. The structure was refined to a final R(F) = 0.0149 for 35 independent observed reflections [I > 2σ(I)]. The mineral is named after the Italian mineralogist Antonio Parascandola (1902–1977).