Context. A small fraction of extremely metal-poor (EMP) stars exhibit moderate to extreme excesses of heavy neutron-capture elements produced in the r-process. The production site(s) of these elements in the early Galaxy remain(s) unclear, as is the reason for their occasional enhancement in the otherwise regular pattern of abundances of elements up to the iron peak. The detailed abundance pattern of the heaviest elements in EMP stars provides insight into their origin and role in the chemical enrichment of the early Galaxy and in radioactive nucleochronology. Aims. The EMP giant star CS 31082-001 ([Fe/H] ∼ −2.9) exhibits an extreme enhancement of neutron-capture elements ([r/Fe] ∼ +1.7) with U and Th enhanced by a further ∼+0.7 dex, and a minimum of blending by molecular lines such as CH or CN. A rich inventory of r-process element abundances was established previously from optical spectra. Here we aim to supplement these data with abundances from near-UV spectroscopy of the third-peak neutron-capture elements, which are crucial for understanding the synthesis of the heaviest elements. Methods. Near-UV spectra from HST/STIS were analysed with LTE model atmospheres and spectrum synthesis calculations to derive new abundances of Os, Ir, Pt, Au, Bi and Pb in CS 31082-001. Results. Together with earlier data, the resulting abundance pattern for the r-process elements provides improved constraints on the nature of the r-process. The observed U and Th abundances and the initial production ratio place CS 31082-001 as one of the oldest stars in the Galaxy, consistent with its extreme metal deficiency. Comparison with the heaviest stable reference elements and with the daughter nuclides Pb and Bi provides a consistency check on this age determination. Finally, the existence of such r-element rich stars indicate that the early chemical evolution of the Galaxy was localised and inhomogeneous.

Context. The origin and site(s) of the r-process nucleosynthesis is(are) still not known with certainty, but complete, detailed r-element abundances offer our best clues. The few extremely metal-poor (EMP) stars with large r-element excesses allow us to study the r-process signatures in great detail, with minimal interference from later stages of Galactic evolution. CS 31082-001 is an outstanding example of the information that can be gathered from these exceptional stars. Aims. Here we aim to complement our previous abundance determinations for third-peak r-process elements with new and improved results for elements of the first and second r-process peaks from near-UV HST/STIS and optical UVES spectra. These results should provide new insight into the nucleosynthesis of the elements beyond iron. Methods. The spectra were analyzed by a consistent approach based on an OSMARCS LTE model atmosphere and the Turbospectrum spectrum synthesis code to derive abundances of heavy elements in CS 31082-001, and using updated oscillator strengths from the recent literature. Synthetic spectra were computed for all lines of the elements of interest to check for proper line intensities and possible blends in these crowded spectra. Our new abundances were combined with the best previous results to provide reliable mean abundances for the first and second-peak r-process elements.Results. We present new abundances for 23 neutron-capture elements, 6 of which -Ge, Mo, Lu, Ta, W, and Re -have not been reported before. This makes CS 31082-001 the most completely studied r-II star, with abundances for a total of 37 neutron-capture elements. We also present the first NLTE+3D abundance of lead in this star, further constraining the nature of the r-process.

Context. Moderately r-process-enriched stars (r-I; +0.3 ≤ [Eu/Fe] ≤ +1.0) are at least four times as common as those that are greatly enriched in r-process elements (r-II; [Eu/Fe] > +1.0), and the abundances in their atmospheres are important tools for obtaining a better understanding of the nucleosynthesis processes responsible for the origin of the elements beyond the iron peak. Aims. The main aim of this work is to derive abundances for a sample of seven metal-poor stars with −3.4 ≤ [Fe/H] ≤ −2.4 classified as r-I stars, to understand the role of these stars for constraining the astrophysical nucleosynthesis event(s) that is (are) responsible for the production of the r-process, and to investigate whether they differ, in any significant way, from the r-II stars. Methods. We carried out a detailed abundance analysis based on high-resolution spectra obtained with the VLT/UVES spectrograph, using spectra in the wavelength ranges 3400-4500 Å, 6800-8200 Å, and 8700-10 000 Å, with resolving power R ∼ 40 000 (blue arm) and R ∼ 55 000 (red arm). The OSMARCS LTE 1D model atmosphere grid was employed, along with the spectrum synthesis code Turbospectrum. Results. We have derived abundances of the light elements Li, C, and N, the α-elements Mg, Si, S, Ca, and Ti, the odd-Z elements Al, K, and Sc, the iron-peak elements V, Cr, Mn, Fe, Co, and Ni, and the trans-iron elements from the first peak (Sr, Y, Zr, Mo, Ru, and Pd), the second peak (Ba, La, Ce, Pr, Nd, Sm, Eu, Gd, Tb, Dy, Ho, Er, Tm, and Yb), the third peak (Os and Ir, as upper limits), and the actinides (Th) regions. The results are compared with values for these elements for r-II and "normal" very and extremely metal-poor stars reported in the literature, ages based on radioactive chronometry are explored using different models, and a number of conclusions about the r-process and the r-I stars are presented. Hydrodynamical models were used for some elements, and general behaviors for the 3D corrections were presented. Although the abundance ratios of the second r-process peak elements (usually associated with the main r-process) are nearly identical for r-I and r-II stars, the first r-process peak abundance ratios (probably associated with the weak r-process) are more enhanced in r-I stars than in r-II stars, suggesting that differing nucleosynthesis pathways were followed by stars belonging to these two different classifications.

Introduction: Pathological love (PL)–behavior characterized by providing repetitive and uncontrolled care and attention to the partner in a romantic relationship–is a rarely studied condition, despite not being rare and causing suffering. This study aims at investigating impulsivity, personality, and characteristics related to the romantic relationship in this population.Methods: Eighty-nine individuals (50 with PL; 39 individuals with no psychiatric disorder) were compared regarding impulsivity, personality, type of attachment, satisfaction with romantic relationship, and love style.Results: Individuals with PL have higher levels of impulsivity (P<.001; Barratt Impulsiveness Scale), higher self-transcendence, that is, are more unconventional and hold sense of communion with a wider reality (P<.001; Temperament and Character Inventory) and keep dissatisfactory romantic relationships (P<.001; Adapted Relationship Assessment Scale).Conclusion: Individuals with PL present personality traits and relationship aspects that must be taken into account in devising assessment and therapeutic strategies for this population.

ResumoContexto: Diversas metodologias foram desenvolvidas para validar instrumentos psicométricos. No entanto, na literatura científica, há escassez de instrumentos para avaliar os relacionamentos amorosos. Objetivo: O presente trabalho tem como objetivo validar para o português o conteúdo dos instrumentos autoaplicáveis Love Attitudes Scale (Escala de Atitudes do Amor -Hendrick et al., 1998), Relationship Assessment Scale (Escala de Avaliação do Relacionamento -Hendrick, 1988) e Adult Attachment Types (Tipos de Apego do Adulto -Hazan et al., 1987), levando em consideração o contexto cultural brasileiro e, consequentemente, possibilitando que o estudo do amor patológico seja viável na população brasileira. Métodos: Tal processo envolveu quatro etapas: (1) tradução para o português, (2) retrotradução, (3) apresentação da versão corrigida para profissionais de saúde mental e estudantes universitários e (4) aplicação da versão final em amostra da população-alvo utilizando uma escala analógico-visual. Resultados: As escalas foram facilmente compreendidas e discriminaram significativamente indivíduos com amor patológico de voluntários saudáveis. Conclusão: Nossos resultados mostram que a versão brasileira desses instrumentos é válida e pode ser usada em investigações envolvendo relacionamentos amorosos.Berti MP, et al. / Rev Psiq Clín. 2011;38(4):135-8 Palavras-chave: Amor, escalas, comportamento compulsivo, validação, tradução. AbstractBackground: Several methodologies were developed to validate psychometric instruments. However, there are, in the scientific literature, a lack of instruments to evaluate romantic relationship. Objective: The present work aims at validating into Portuguese the content of the self-report Love Attitudes Scale (Escala de Atitudes do Amor -Hendrick et al., 1998), the Relationship Assessment Scale (Escala de Avaliação do Relacionamento -Hendrick, 1988), and the Adult Attachment Types (Tipos de Apego do Adulto -Hazan et al., 1987), taking the Brazilian cultural context into consideration, thus rendering the study of pathological love in the Brazilian population feasible. Methods: Such process involved four stages: (1) translation into Portuguese, (2) back translation, (3) presentation of the translated version to mental health professionals and university students, and (4) application of the final version in a sample of the target population using a rating scale. Results: The scales were easily understood and significantly discriminated individuals with pathological love and healthy volunteers. Discussion: Our results show that the Brazilian version of these instruments is valid and may be used in investigations involving romantic relationships.

Context. HD 140283 is a nearby (V = 7.7) subgiant metal-poor star, extensively analysed in the literature. Although many spectra have been obtained for this star, none showed a signal-to-noise (S/N) ratio high enough to enable a very accurate derivation of abundances from weak lines. Aims. The detection of europium proves that the neutron-capture elements in this star originate in the r-process, and not in the s-process, as recently claimed in the literature. Methods. Based on the OSMARCS 1D LTE atmospheric model and with a consistent approach based on the spectrum synthesis code Turbospectrum, we measured the europium lines at 4129 Å and 4205 Å, taking into account the hyperfine structure of the transitions. The spectrum, obtained with a long exposure time of seven hours at the Canada-France-Hawaii Telescope (CFHT), has a resolving power of 81 000 and a S/N ratio of 800 at 4100 Å. Results. We were able to determine the abundance A(Eu) = −2.35 ± 0.07 dex, compatible with the value predicted for the europium from the r-process. The abundance ratio [Eu/Ba] = +0.58 ± 0.15 dex agrees with the trend observed in metal-poor stars and is also compatible with a strong r-process contribution to the origin of the neutron-capture elements in HD 140283.

No abstract

The abundance of heavy r-elements may provide a better understanding of the r-process, and the determination of several reference r-elements should allow a better determination of a star's age. The space UV region (λ < 3000 Å) presents a large number of lines of the heavy elements, and in the case of some elements, such as Bi, Pt, Au, detectable lines are not available elsewhere. The extreme “r-process star” CS 31082–001 ([Fe/H] = –2.9) was observed in the space UV to determine abundances of the heaviest stable elements, using STIS on board Hubble Space Telescope.