Iusti Lipsi De vesta et vestalibus syntagma.

Mode of access: Internet.

Liberti Fromondi ... Vesta, siue Antaristarchi vindex, adversus Jac Lansbergium ... : in quo decretum S. Congregationis S. R. E. Cardinalium anno MDCXVI et alterum anno MDCXXXIII adversus Copernicanos terrae motores editum, iterum defenditur

Mode of access: Internet.

Der Tempel der Vesta und das Haus der Vestalinnen.

Mode of access: Internet.

Hestia-Vesta : ein Cyclus religionsgeschichtlicher Forschungen /

Includes bibliographical references.

Janus & Vesta; a study of the world crisis and after,

Mode of access: Internet.

CIL 2.1166 – Sacred dedication to Vesta Augusta

Photograph

A frequency approach to identifying asteroid families II. Families interacting with nonlinear secular resonances and low-order mean-motion resonances

Aims. In an earlier paper we introduced a new method for determining asteroid families where families were identified in the proper frequency domain (n, g, g + s) ( where n is the mean-motion, and g and s are the secular frequencies of the longitude of pericenter and nodes, respectively), rather than in the proper element domain (a, e, sin(i)) (semi-major axis, eccentricity, and inclination). Here we improve our techniques for reliably identifying members of families that interact with nonlinear secular resonances of argument other than g or g + s and for asteroids near or in mean-motion resonant configurations. Methods. We introduce several new distance metrics in the frequency space optimal for determining the diffusion in secular resonances of argument 2g - s, 3g - s, g - s, s, and 2s. We also regularize the dependence of the g frequency as a function of the n frequency (Vesta family) or of the eccentricity e (Hansa family). Results. Our new approaches allow us to recognize as family members objects that were lost with previous methods, while keeping the advantages of the Carruba & Michtchenko (2007, A& A, 475, 1145) approach. More important, an analysis in the frequency domain permits a deeper understanding of the dynamical evolution of asteroid families not always obtainable with an analysis in the proper element domain.

Loxoscelismo en Chile: estudios epidemiológicos, clínicos y experimentales

Se presenta un enfoque panorámico de estudios epidemiológicos, clínicos y experimentales referentes a Loxosceles laeta y loxoscelismo efectuados en 1955-1988 en Santiago, Chile. Se estudiaron 216 casos de loxoscelismo. Los hechos más relevantes fueron: 52,8% correspondió a mujeres; edad entre 7 meses y 78 años; 84,3% fué loxoscelismo cutáneo (LO y 15,7% loxoscelismo cutáneo-visceral (LCV); 73,6% sucedió en época calurosa; en 86,6% el accidente ocurrió en la vivienda, especialmente en dormitorios, mientras la persona dormía o se vestía. La araña fué vista en 60,2% de los casos e identificada en laboratorio como L. laeta en 17,7% (10,6% de los 216 casos). Los sitios más frecuen temente afectados fueron las extremidades con 67,6%, lancetazo urente fué el síntoma inicial más frecuente. Dolor, edema y placa livedoide, la cual posteriormente se transformaría en escara necrótica, fueron las manifestaciones locales predominantes. En LCV hematuria y hemoglobinuria fueron constantes, ictericia, fiebre y compromiso de conciencia se presentaron en la mayoría de los casos. Tratamiento: LC con antihistamínicos o corticoides inyectables, LCV con corti-coides inyectables. La condición de los pacientes en el último control fué: curación completa en 75,5%, curación con secuela cicatrizal en 8,3%, muerte en 3,7% (todos con LCV) y abandono en 12,5%. Adicionalmente, se ha efectuado una serie de estudios experimentales, tanto in vivo como in vitro para esclarecer aspectos básicos sobre el veneno de L. laeta y el tratamiento del loxoscelismo.

[Tivoli. Tempio della Sibilla]

Référence bibliographique : Weigert, 697

Charles C. Chapman's birthday celebration, Fullerton, California,1932

Family portrait taken at Charles C. Chapman's birthday celebration, Fullerton, California,July 2, 1932. The group poses outside his residence on the lawn. Top row [left to right]: Arthur Irvin, Charles Wickett, Irvin Chapman, Sam Collins, Paul Williams, Grant Chapman,, Sidney Chapman, Clay McCarn, Earl Chapman's son David McDougal, Earl Chapman's son William McDougal, Earl Chapman, Harry Chapman, William Wickett Sr. Second row [left to right]: Mr. VanMeter, Mrs. Sinclair, C. C. Sinclair, John Franklin, Way Bagley, Marjorie Collins, Emma Williams, Ruth Chapman, Vesta Chapman, Inez Bagley, Grace Chapman, Bertha Chapman, Clough Chapman, Frank and Bertha Chapman's daughter Agnes McDougal [Streech], Georgiana Chapman, Thela Clough, Mrs. Earl [Ann] Chapman, Bessie Reynolds, Fred Chapman, E. B. [Bert] Reynolds. Seated [left to right]: Mrs. VanMeter, Hattie Clark, Louie Messlar, Charlie Thamer, Louella Thamer, Dolla Harris, Stanley Chapman Sr. holding Mary Anne, Ethel Wickett, Charles C. Chapman, Clara Chapman, Colum C. Chapman, Aunt Annie Colum, Deryth Chapman, Anna Marie Chapman, Floy Chapman, Edith Chapman. Front row [left to right]: Sam E. Collins, Bill Wickett Jr., Joyce Chapman, Marilyn Chapman, Elizabeth Chapman, Mary McCarn, Nina Chapman Lescher, Jodeane Collins, Bob Gibb, Jean Chapman. In front is a floral arrangement with drawing of a Western Union telegram "To Chas. C. Chapman, July 2, 1932, N. Fullerton, Cal., 'Wishing you a happy birthday, Nina."

Chaotic diffusion caused by close encounters with several massive asteroids: II. the regions of (10) Hygiea, (2) Pallas, and (31) Euphrosyne

Context. Close encounters with (1) Ceres and (4) Vesta, the two most massive bodies in the main belt, are known to be a mechanism of dynamical mobility able to significantly alter proper elements of minor bodies, and they are the main source of dynamical mobility for medium-sized and large asteroids (D > 20 km, approximately). Recently, it has been shown that drift rates caused by close encounters with massive asteroids may change significantly on timescales of 30 Myr when different models (i.e., different numbers of massive asteroids) are considered. Aims. So far, not much attention has been given to the case of diffusion caused by the other most massive bodies in the main belt: (2) Pallas, (10) Hygiea, and (31) Euphrosyne, the third, fourth, and one of the most massive highly inclined asteroids in the main belt, respectively. Since (2) Pallas is a highly inclined object, relative velocities at encounter with other asteroids tend to be high and changes in proper elements are therefore relatively small. It was thus believed that the scattering effect caused by highly inclined objects in general should be small. Can diffusion by close encounters with these asteroids be a significant mechanism of long-term dynamical mobility? Methods. By performing simulations with symplectic integrators, we studied the problem of scattering caused by close encounters with (2) Pallas, (10) Hygiea, and (31) Euphrosyne when only the massive asteroids (and the eight planets) are considered, and the other massive main belt asteroids and non-gravitational forces are also accounted for. Results. By finding relatively small values of drift rates for (2) Pallas, we confirm that orbital scattering by this highly inclined object is indeed a minor effect. Unexpectedly, however, we obtained values of drift rates for changes in proper semi-major axis a caused by (10) Hygiea and (31) Euphrosyne larger than what was previously found for scattering by (4) Vesta. These high rates may have repercussions on the orbital evolution and age estimate of their respective families. © 2013 ESO.

Mobilidade asteroidal induzida por encontros próximos com vários asteroides massivos

Pós-graduação em Física - FEG

Encontros próximos: captura gravitacional temporária e esfera de influência

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Dynamical evolution of V-type photometric candidates in the outer main belt

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

Lutetia׳s lineaments

The European Space Agency׳s Rosetta spacecraft flew by asteroid (21) Lutetia on July 10, 2010. Observations through the OSIRIS camera have revealed many geological features. Lineaments are identified on the entire observed surface of the asteroid. Many of these features are concentric around the North Pole Crater Cluster (NPCC). As observed on (433) Eros and (4) Vesta, this analysis of Lutetia assesses whether or not some of the lineaments could be created orthogonally to observed impact craters. The results indicate that the orientation of lineaments on Lutetia׳s surface could be explained by three impact craters: the Massilia and the NPCC craters observed in the northern hemisphere, and candidate crater Suspicio inferred to be in the southern hemisphere. The latter has not been observed during the Rosetta flyby. Of note, is that the inferred location of the Suspicio impact crater derived from lineaments matches locations where hydrated minerals have been detected from Earth-based observations in the southern hemisphere of Lutetia. Although the presence of these minerals has to be confirmed, this analysis shows that the topography may also have a significant contribution in the modification of the spectral shape and its interpretation. The cross-cutting relationships of craters with lineaments, or between lineaments themselves show that Massilia is the oldest of the three impact feature, the NPCC the youngest, and that the Suspicio impact crater is of intermediate age that is likely occurred closer in time to the Massilia event.