Two new feather mite species (Acari, Pteronyssidae) from the white-barred piculet, Picumnus cirratus (Ayes, Piciformes)

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

A NEW SPECIES of THE FEATHER MITE GENUS COTINGODECTES and A NEW GENUS of PTERODECTINAE (ASTIGMATA: PROCTOPHYLLODIDAE)

In this paper a second species of the feather mite genus Cotingodectes Valim and Hernandes, C. breviphallus n. sp., is described from Rupicola rupicola (Passeriformes, Cotingidae) in Brazil. A new genus, Berladectes, is erected to accommodate Dolichodectes neotropicus Hernandes and Valim.

Feather mites of Brazil (Acari: Astigmata: Analgoidea and Pterolichoidea)

We present a checklist of feather mites known from native birds in Brazil. The list was compiled from a survey of Brazilian records published in indexing databases (e.g. Zoological Records) and from the available literature. To date, 185 nominal species representing 21 families have been recorded from Brazilian birds. Associations with 15 bird orders were found: Anseriformes, Apodiformes, Caprimulgiformes, Ciconiiformes, Columbiformes, Cuculiformes, Falconiformes, Galliformes, Gruiformes, Opisthocomiformes, Passeriformes, Piciformes, Psittaciformes, Tinamiformes and Trogoniformes. These birds sum to 218 species, which represent only 12.4% of all bird species occurring in Brazil. The feather mite fauna of several species-rich and important bird orders in Brazil remain unexplored, including Cathartiformes, Charadriiformes, Coraciiformes, Galbuliformes and Strigiformes. We estimate that between 900 and 5300 feather mite species are expected to occur on Brazilian birds, which is at least five times greater than current records. The training of researchers with expertise in the taxonomy of this group of mites should be stimulated so that there is a compatible number of taxonomists to discover and describe the almost unexplored feather mite fauna in Brazil.

Evolution of magnetic field and spin period in accreting neutron stars

Based on the accretion-induced magnetic field decay model, in which a frozen field and an incompressible fluid are assumed, we obtain the following results: (1) an analytic relation between the magnetic field and spin period, if the fastness parameter of the accretion disk is neglected (The evolutionary tracks of accreting neutron stars in the P-B diagram in our model are different from the equilibrium period lines when the influence of the fastness parameter is taken into account.); (2) the theoretical minimum spin period of an accreting neutron star is max(1.1ms (DeltaM/M(circle dot))(-1)R(6)(-5/14) I(45)(M/M(circle dot))(-1/2),1.1ms (M/M(circle dot))(-1/2) R(6)(17/14)), independent of the accretion rate (X-ray luminosity) but dependent on the total accretion mass, DeltaM; however, the minimum magnetic field depends on the accretion rate; (3) the magnetic field strength decreases faster with time than does the period.

Awaking the Vacuum in Relativistic Stars

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Particle creation due to tachyonic instability in relativistic stars

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

Two new genera and five new species of the feather mite subfamily Proctophyllodinae (Astigmata : Proctophyllodidae) from suboscine birds in Brazil

Two new genera and five new species of feather mites of the family Proctophyllodidae are described from passerine birds from Brazil: Tyranniphyllodes pitangi gen. n., sp. n. from Pitangus sulphuratus (Tyrannidae); Atrichophyllodes delalandi gen. n., sp. n. from Corythopis delalandi (Tyrannidae); A. mentalis gen. n., sp. n. from Dysithamnus mentalis (Thamnophilidae); Anisophyllodes candango sp. n. from Elaenia chiriquensis (Tyrannidae); and Platyacarus sittasomi sp. n. from Sittasomus griseicapillus (Dendrocolaptidae). The discovery of these taxa might give data for a better understanding of the evolution of the family Proctophyllodidae in general and the dispersion of these mites on passerines in South America in paricular.

A possible stellar metallic enhancement in post-T Tauri stars by a planetesimal bombardment

The photospheres of stars hosting planets have larger metallicity than stars lacking planets. This could be the result of a metallic star contamination produced by the bombarding of hydrogen-deficient solid bodies. In the present work we study the possibility of an earlier metal enrichment of the photospheres by means of impacting planetesimals during the first 20-30 Myr. Here we explore this contamination process by simulating the interactions of an inward migrating planet with a disc of planetesimal interior to its orbit. The results show the percentage of planetesimals that fall on the star. We identified the dependence of the planet's eccentricity (e(p)) and time-scale of migration (tau) on the rate of infalling planetesimals. For very fast migrations (tau= 10(2) and 10(3) yr) there is no capture in mean motion resonances, independently of the value of e(p). Then, due to the planet's migration the planetesimals suffer close approaches with the planet and more than 80 per cent of them are ejected from the system. For slow migrations (tau= 10(5)and 10(6) yr) the percentage of collisions with the planet decreases with the increase of the planet's eccentricity. For e(p) = 0 and 0.1 most of the planetesimals were captured in the 2:1 resonance and more than 65 per cent of them collided with the star. Whereas migration of a Jupiter mass planet to very short pericentric distances requires unrealistic high disc masses, these requirements are much smaller for smaller migrating planets. Our simulations for a slowly migrating 0.1 M-Jupiter planet, even demanding a possible primitive disc three times more massive than a primitive solar nebula, produces maximum [Fe/H] enrichments of the order of 0.18 dex. These calculations open possibilities to explain hot Jupiter exoplanet metallicities.

AN INEXPENSIVE METHOD FOR CHROMOSOME PREPARATIONS FROM FEATHER PULP IN BIRDS, USING SHORT-TERM TREATMENT WITH COLCHICINE IN-VITRO, DEMONSTRATED ON AMAZONA-AMAZONICA (PSITTACIDAE)

In order to develop an efficient and low-cost technique for obtaining bird chromosome preparations, and to adapt the cytogenetic process of bird sexing for general use at zoos and breeding farms with the technical support of cytogenetics laboratories, we tested variants of the technique described by Giannoni et al. (Genet. Sel. Evol. 23: 123-125, 1991), based on the utilization of cellular material from growing feather pulp cultured in complete medium for six hours. Hanks' saline solution gave satisfactory performance as a substitute for complete medium, with no need to use PHA, serum of collagenase, when utilized in material obtained from feather pulp of Amazona amazonica (Psittacidae).

Distribution of refractory and volatile elements in CoRoT exoplanet host stars

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Stars of WIMPs

A class of boson-fermion stars, whose spin-0 and spin-1/2 constituents interact through a U(1) current-current term in the Lagrangian density, is analyzed. It is shown that it describes the low-energy behavior of a system of weakly interacting massive particles (WIMPs) from the leptonic sector of the minimal supersymmetric standard model. In this case the effective coupling constant A is related to the Fermi constant GF.

Collective scattering of massive stars in higher order gravity

In the weak field approximation of higher order gravity theory a gravitational potential is described by a Newtonian plus a Yukawa-like term. This new term is used to explain some aspects of galactic dynamics, without considering dark matter. Its presence modifies the scattering probability of a massive intruder star and relaxation time of the stellar system.

Model for stars of interacting bosons and fermions

In this paper we introduce a current-current type interaction term in the Lagrangian density of gravity coupled to complex scalar fields, in the presence of a degenerated Fermi gas. For low transferred momenta, such a term, which might account for the interaction among boson and fermion constituents of compact stellar objects, is subsequently reduced to a quadratic one in the scalar sector. This procedure enforces the use of a complex radial field counterpart in the equations of motion. The real and the imaginary components of the scalar field exhibit different behavior as the interaction increases. The results also suggest that the Bose-Fermi system undergoes a phase transition for a suitable choice of the coupling constant.

The saturated magnetic field of the neutron stars

Considering the ferromagnetic screening for the decay of the X-ray neutron star magnetic field in the binary accretion phase, the phase transition of ferromagnetic materials in the crust of neutron star induces the ferromagnetic screening saturation of the accreted crust, which results in the minimum surface magnetic field of the accreting neutron star, about 108 G, if the accreted matter has completely replaced the crust mass of the neutron star. The magnetic field evolution versus accreted mass is given as Bs ∝ ΔM-0.9, and the obtained magnetic field versus spin period relation is consistent with the distribution of the binary X-ray sources and recycled pulsars. The further thermal effect on the magnetic evolution is also studied.