bluuebunny/crossref_metadata_2025_split huggingface dataset:
Mediterranean diet in relation to body mass index and waist-to-hip ratio
Authors: Rossi Marta , Negri Eva , Bosetti Cristina , Dal Maso Luigino , Talamini Renato , Giacosa Attilio , Montella Maurizio , Franceschi Silvia , La Vecchia Carlo 
Published: August 2007

AbstractObjectiveThe Mediterranean diet is rich in fat and starch, and hence may be related to overweight. We therefore investigated the relationship between adherence to a Mediterranean diet and body mass index (BMI) and waist-to-hip ratio (WHR).Design and settingData were obtained from the control group of a network of case–control studies on cancer conducted in major teaching and general hospitals in four Italian areas between 1991 and 2002. An interviewer-administered validated 78-item food-frequency questionnaire was used to obtain information on the subjects’ habitual diet. Information on socio-economic factors, lifestyle habits and anthropometric measures was also collected. A Mediterranean diet score (MDS) was derived on the basis of eight characteristics of the Mediterranean diet.SubjectsSubjects were 6619 patients (3090 men, 3529 women) admitted to hospital for a wide spectrum of acute, non-neoplastic conditions, unrelated to known risk factors for cancer and long-term modifications of diet.ResultsIn multiple linear regression models adjusted for age, study centre, education, tobacco smoking, occupational physical activity and total energy intake, the MDS was not related to BMI (β = 0.05 for men and −0.04 for women) or WHR (β = 0.000 and 0.001, respectively) in both sexes.ConclusionsAdherence to the major characteristics of the Mediterranean diet is unrelated to BMI and WHR, confirming previous data from Greece and Spain.
Validity of photographs for food portion estimation in a rural West African setting
Authors: Huybregts L , Roberfroid D , Lachat C , Van Camp J , Kolsteren P 
Published: August 2007

AbstractObjectiveTo validate food photographs for food portion size estimation of frequently consumed dishes, to be used in a 24-hour recall food consumption study of pregnant women in a rural environment in Burkina Faso. This food intake study is part of an intervention evaluating the efficacy of prenatal micronutrient supplementation on birth outcomes.SubjectsWomen of childbearing age (15–45 years).DesignA food photograph album containing four photographs of food portions per food item was compiled for eight selected food items. Subjects were presented two food items each in the morning and two in the afternoon. These foods were weighed to the exact weight of a food depicted in one of the photographs and were in the same receptacles. The next day another fieldworker presented the food photographs to the subjects to test their ability to choose the correct photograph.ResultsThe correct photograph out of the four proposed was chosen in 55% of 1028 estimations. For each food, proportions of underestimating and overestimating participants were balanced, except for rice and couscous. On a group level, mean differences between served and estimated portion sizes were between −8.4% and 6.3%. Subjects who attended school were almost twice as likely to choose the correct photograph. The portion size served (small vs. largest sizes) had a significant influence on the portion estimation ability.ConclusionsThe results from this study indicate that in a West African rural setting, food photographs can be a valuable tool for the quantification of food portion size on group level.
Maternal anthropometry as a predictor of birth weight
Authors: Nahar Shamsun , Mascie-Taylor C G N , Begum Housne Ara 
Published: August 2007

AbstractObjectiveTo determine whether maternal anthropometry predicted birth weight, and if so, to identify which cut-offs provided the best prediction of low birth weight (LBW) in a field situation.DesignCommunity-based longitudinal study.SettingA rural union of Bhaluka Upazila, Mymensingh, located 110 km north-west of Dhaka, the capital of Bangladesh.ParticipantsA total of 1104 normotensive, non-smoking pregnant women who attended community nutrition centres were studied from first presentation at the centre until delivery of their child.ResultsMost of the pregnant mothers were between 20 and 34 years of age. Over one-third of the women were nulliparous, while 12.8% were multiparous (parity ≥ 4). Most (93%) mothers registered between the 3rd and 5th month of pregnancy. The frequency of LBW ( < 2500 g) was 17%. Polynomial regression analyses showed that the best predictors of birth weight (based on adjustedR2values) were in general weight at registration and weight at month 9, with adjustedR2ranging from 2.5% to nearly 20%. Sequential regression analyses with height and weight showed that there was a significant effect of height after removing the weight variables, and adjustedR2increased in all analyses. Weight and height at registration month continued to be the best predictors of LBW. Sensitivity and specificity curves were drawn for each registration month, body mass index and different weight gain groups, and using different weight and height combinations. The results showed that, for registration month 3–5, a combination of weight ( ≤ 45 kg) and height ( ≤ 150 cm) gave the highest sensitivity, which was 50%. However, maternal weight ≤ 43 kg in pregnancy month 3–5 alone gave the highest sensitivity of 80%.ConclusionThe best predictor of birth weight as a continuous variable was maternal weight at registration, each 1 kg increase in weight at registration being associated with an increase in birth weight of about 260 g. Maternal weight ≤ 43 kg in pregnancy month 3–5 alone gave the highest sensitivity of 80%. A combination of initial weight and height of the mother was not as good a predictor of LBW as weight alone.
Laboratory simulation of UV irradiation from the Sun on amino acids. II. Irradiation of phenylalanine and tryptophan
Authors: Scappini F. , Capobianco M.L. , Casadei F. , Zamboni R. , Giorgianni P. 
Published: August 2007

AbstractThe effects of near ultraviolet (UV) irradiation on water solutions of phenylalanine and tryptophan have been investigated using a broad-band xenon lamp in the region 200–800 nm. This is a step in the laboratory simulation of the effects of Solar radiation on the building blocks of life, specifically α-amino acids, with regards to the origin of life. Results are presented showing the photodegradation of phenylalanine and tryptophan against different UV doses. Some of the degradation products are still protein amino acids. An analysis of the irradiated solutions is carried out by spectroscopic and analytic techniques. The laboratory simulations are discussed in the wake of a life emerging scenario on the primitive Earth.
Orbital Period Variation in the Chromospherically Active Binary FF UMa (2RE J0933+624)
Authors: Gálvez M.C. , Montes D. , Fernández-Figueroa M.J. , De Castro E. , Cornide M. 
Published: August 2007

AbstractWe present here a detailed study of FF UMa (2RE J0933+624), a recently discovered, X-ray/EUV selected, active binary system with strong Hα emission. By using high-resolution echelle spectroscopic observations taken during five observing runs from 1998 to 2004, we derived precise radial velocities that allowed us to determine the orbital solution of the system at different epochs. Analyzing these orbital solutions, together with a previous one determined in 1993 by other authors, we have found a change in the heliocentric Julian date on conjunction (Tconj) that can be explained by a change with time in the orbital period of the system. The relative amplitude of the orbital period variation derived from these data was dP/P ≈ 5 x 10−4, which is larger than the variations found in other similar chromospherically active binaries like AR Lac and HR 1099. This orbital period variation can be related (Applegate 1992; Lanza 1998, 2006) with the modulation of the gravitational quadrupole-moment of its magnetically active secondary star produced by angular momentum exchanges within its convective envelope. In addition, using these observations, we have determined the stellar parameters of the components and we have carried out a study of the chromospheric activity using all the optical indicators from Ca ii H&K to Ca ii IRT lines.
Only Binary Stars Can Help Us Actually SEE a Stellar Chromosphere
Authors: Griffin R. Elizabeth 
Published: August 2007

AbstractBinary stars of the ζ Aurigae type (eclipsing systems containing a cool giant plus a hot main-sequence star) offer a unique and highly effective method of probing a stellar chromosphere. Close to occultation the main-sequence star acts as a light probe behind the giant's chromosphere, enabling an observer to detect changing conditions in that chromosphere along the line of sight. The technique is powerful, the effects dramatic. However, presently known eclipsing systems number only about 10, and a much greater sample is required for meaningful statistics of the properties of stellar chromospheres. New surveys of fainter binaries should be investigated for eclipses in order to gain more information on chromospheres in general. Such information is vital for modelling stellar photospheres, from which abundances are derived. This paper describes the very different behaviour of chromospheric material in three 3rd-magnitude giants.
Discovery of a New Dwarf Nova, TSS J022216.4+412259.9: a WZ Sge-type Dwarf Nova Breaking the Shortest Superhump Period Record
Authors: Imada Akira , Kubota Kaori , Kato Taichi , Nogami Daisaku , Maehara Hiroyuki , Nakajima Kazuhiro , Uemura Makoto , Ishioka Ryoko 
Published: August 2007

AbstractWe report on time-resolved CCD photometry of the newly-discovered dwarf nova, TSS J022216.4+412259.9 during its outburst in 2005 November–December. The best-estimated superhump period was 0.0554 days, which is the shortest superhump period among WZ Sge-type dwarf novae ever known. Double-peaked humps were also detected with a period of 0.05487 days in the early stage of the outburst. A rebrightening exhibited after the end of the plateau phase. All of these observations indicate the WZ Sge nature of the system. We mainly discuss the rebrightening stage of the superoutburst, compared with other WZ Sge-type dwarf novae.
V379 Cep: a System of Two Binaries
Authors: Mayer P. , Harmanec P. , Božić H. , Eenens P. , Guinan E.F. , McCook G. , Koubský P. , Ruždjak D. , Sudar D. , Šlechta M. , Wolf M. , Yang S. 
Published: August 2007

AbstractWe obtained new series of electronic spectra and UBV photometry of V379 Cep and analyzed them in an effort to check whether the conclusion about its anomalous masses is not premature. We found that the second system of spectral lines seen in the spectra of V379 Cep does not belong to the secondary but to the primary of another binary Ba+Bb (orbital period of 159d0) which constitutes a quadruple system with the narrow-lined 99d76 eclipsing binary Aa+Ab (for which we report probable detection of the secondary and derive improved period and orbital elements). The mutual motion of the two binaries A+B around the common centre of gravity is also observable and the probable orbital period is some 7878 days. Our result shows that the components Aa and Ba are somewhat evolved but removes the reported discrepancy of anomalously small masses. We find that V379 Cep is an astrophysically interesting quadruple system for which a future combination of interferometry, spectroscopy and photometry can provide individual masses of all four bodies.
A Mass Estimate in a Sample of Double Stars
Authors: Ninković S. , Cvetković Z. 
Published: August 2007

AbstractThe total masses of binaries are calculated on the basis of their orbital elements from the Sixth Catalog of Orbits of Visual Binary Stars. They are then compared with the values resulted from the mass-luminosity relation for the Main Sequence where as the input data are used: trigonometric parallax, total apparent magnitude of the pair (source Hipparcos Catalogue) and magnitude difference (source Hipparcos Catalogue and Photometric Magnitude Difference Catalog). It seems that for the pairs indicated as having qualitative orbital elements the agreement between the total-mass values obtained in these two ways is satisfactory.
Comparison of Selected Methods for Radial Velocity Measurements
Authors: Parimucha Štefan , Škoda Petr 
Published: August 2007

AbstractWe present a comparison of selected methods for measuring radial velocities in stellar spectra. We compare cross-correlation, line-profile fitting with Gauss, Lorentz and Voigt functions and a less-known mirroring method. We discuss their applicability and precision and indicate their advantages and disadvantages. The mirroring method proved to be useful for the analysis of Be stars, but is not implemented in any major astronomical packages.
Interferometric Investigations of Eclipsing Binaries as a Key to an Improved Distance Scale
Authors: Shabun K. , Richichi A. , Munari U. , Siviero A. , Pacsysnki B. 
Published: August 2007

AbstractBinary and multiple systems constitute one of the main tools for obtaining fundamental stellar parameters, such as masses, radii, effective temperatures and distances. One especially fortunate, and at the same time rare, occurrence is that of double-lined eclipsing binaries with well-detached components. In this special case, it is possible to obtain a full solution of all orbital and stellar parameters, with the exception of the effective temperature of one star, which is normally estimated from spectral type or derived from atmospheric analysis of the spectrum. Long-baseline interferometry at facilities such as the ESO VLTI is beginning to have the capability to measure directly the angular separation and the angular diameter of some selected eclipsing binary systems, and we have proposed such observations with the AMBER instrument. In particular, we aim at deriving directly the effective temperature of at least one of the components in the proposed system, thereby avoiding any assumptions in the global solution through the Wilson–Devinney method. We will also obtain an independent check of the results of this latter method for the distance to the system. This represents the first step towards a global calibration of eclipsing binaries as distance indicators. Our results will also contribute to the effective temperature scale for hot stars. The extension of this approach to a wider sample of eclipsing binaries could provide an independent method to assess the distance to the LMC. The observations will extend accurate empirical calibration to spectral type O9 – B0.
Confronting Stellar Evolution Models for Active and Inactive Solar-Type Stars: The Triple System V1061 Cygni
Authors: Torres Guillermo , Lacy Claud H. Sandberg , Marschall Laurence A. , Sheets Holly A. , Mader Jeff A. 
Published: August 2007

AbstractWe present spectroscopic and photometric observations of the chromospherically active (X-ray strong) eclipsing binary V1061 Cyg (P = 2.35 days) showing that it is in reality a hierarchical triple system. We combine these observations with Hipparcos intermediate data (abscissa residuals) to derive the outer orbit with a period of 15.8 yr. We determine accurate values for the masses, radii, and effective temperatures of the eclipsing binary components, as well as for the mass and temperature of the third star. For the primary we obtain M = 1.282 ± 0.015 M⊙, R = 1.615 ± 0.017 R⊙, Teff = 6180 ± 100 K, for the secondary M = 0.9315 ± 0.0068 M⊙, R = 0.974 ± 0.020 R⊙, Teff = 5300 ± 150 K, and for the tertiary M = 0.925 ± 0.036 M⊙ and Teff = 5670 ± 100 K. Current stellar evolution models agree well with the properties of the primary star, but show a large discrepancy in the radius of the secondary in the sense that the observed value is about 10% larger than predicted (a 5σ effect). We also find the secondary temperature to be ∼200 K cooler than indicated by the models. These discrepancies are quite remarkable considering that the secondary is only 7% less massive than the Sun, which is the calibration point of all stellar models. Similar differences with theory have been seen before for lower mass stars. We identify chromospheric activity as the likely cause of the effect. Inactive stars agree very well with the models, while active ones such as the secondary of V1061 Cyg appear systematically too large and too cool. Both of these differences are understood in terms of the effects of magnetic fields commonly associated with chromospheric activity.
A survey of published astronomical outputs of countries from 1976 to 2005 and the dependence of output on population, number of IAU members and gross domestic product
Authors: Hearnshaw John 
Published: August 2007

AbstractIn this paper I report the results of a survey of the astronomical outputs of all 63 IAU member countries as well as several non-member countries, based on an analysis of the affiliations of the authors given for nearly 900 thousand astronomical papers appearing in ADS between the years 1976 and 2005. The results show a roughly three-fold increase in the number of published papers per year over this 30-year interval. This increase is seen both in developed and also in most developing countries. The number of publications per IAU member correlates strongly with gross domestic product. It is over 2 papers per IAU member per year in the countries with the strongest economies but less than 0.5 in the countries with low GDP per capita. Since 2001 there has been a dramatic increase in the number of multi-author multinational papers published. This increase is especially noticeable for authors in developing countries, indicating that astronomers in these countries are increasingly participating in international collaborations for their research activities.
Promoting astronomy in developing countries: an historical perspective
Authors: Kochhar Rajesh 
Published: August 2007

AbstractAny international effort to promote astronomy world wide today must necessarily take into account its cultural and historical component. The past few decades have ushered in an age, which we may call the Age of Cultural Copernicanism. In analogy with the cosmological principle that the universe has no preferred location or direction, Cultural Copernicanism would imply that no cultural or geographical area, or ethnic or social group, can be deemed to constitute a superior entity or a benchmark for judging or evaluating others.In this framework, astronomy (as well as science in general) is perceived as a multi-stage civilizational cumulus where each stage builds on the knowledge gained in the previous stages and in turn leads to the next. This framework however is a recent development. The 19th century historiography consciously projected modern science as a characteristic product of the Western civilization decoupled from and superior to its antecedents, with the implication that all material and ideological benefits arising from modern science were reserved for the West.As a reaction to this, the orientalized East has often tended to view modern science as “their” science, distance itself from its intellectual aspects, and seek to defend, protect and reinvent “our” science and the alleged (anti-science) Eastern mode of thought. This defensive mind-set works against the propagation of modern astronomy in most of the non-Western countries. There is thus a need to construct a history of world astronomy that is truly universal and unselfconscious.Similarly, the planetarium programs, for use the world over, should be culturally sensitive. The IAU can help produce cultural-specific modules. Equipped with this paradigmatic background, we can now address the question of actual means to be adopted for the task at hand. Astronomical activity requires a certain minimum level of industrial activity support. Long-term maintenance of astronomical equipment is not a trivial task. There are any number of examples of an expensive facility falling victim to AIDS: Astronomical Instrument Deficiency Syndrome. The facilities planned in different parts of the world should be commensurate with the absorbing power of the acceptor rather than the level of the gifter.
Astronomy–the Caribbean view from the ground up
Authors: Haque Shirin 
Published: August 2007

AbstractThe historical development of astronomy in the Caribbean is reviewed within its cultural and environmental framework. The present status of astronomy in education, research and at the popular level is presented also with the focus being on its development in the island of Trinidad and Tobago in particular. We review what works in small developing islands versus larger developed or developing countries and the peculiar trials and tribulations of our circumstances as well as the rewards of such efforts. The critical role of students and volunteer effort will be highlighted. The psychological and cultural aspect and its role in the development of astronomy in the Caribbean is also explored. The outlook for the next decade will be highlighted with a brief proposal of having a node for TWAN (Third World Astronomy Network) in Trinidad in the Caribbean.
Developing astronomy in Cuba
Authors: Taboada Ramón E. Rodríguez 
Published: August 2007

AbstractThe development process of astronomy in Cuba is analysed from the point of view of a person actually working in astrophysics. It is concluded that the key word for astronomy development is “engagement” between a mature partner and the new developing group. It can not be forgotten that only astronomers do astronomy and that should be the main goal: to develop people working in astronomy.
New facilities for astronomy education and popularization in Guanajuato, Mexico
Authors: Bravo–Alfaro Hector 
Published: August 2007

AbstractWith relatively low funds, the Departamento de Astronomía de la Universidad de Guanajuato, in Mexico, has successfully carried out the modernization of a rustic astronomical observatory. At this site, once it is fully refurbished, it is planned to hold not only public observations, but also to have an ambitious programme of science popularization devoted to scholars.
Observing programmes of the Observatorio Astronómico Los Molinos, Uruguay
Authors: Tancredi Gonzalo , Roland S. , Salvo R. , Benitez F. , Bruzzone S. , Ceretta A. , Acosta E. 
Published: August 2007

AbstractThe Observatorio Astronómico Los Molinos (OALM) is the only professional observatory in Uruguay. Its research activity is dedicated to the study of Small Bodies of the Solar System, i.e. comets and asteroids. It is one of the few observatories in the southern hemisphere dedicated to this topic. The observational programmes that we are conducting at present are described, putting especial emphasis in the results obtained last year.
Astronomical extinction over the ELT Moroccan sites from aerosol satellite data
Authors: Siher El Arbi , Benkhaldoun Zouhair , Bounhir Aziza 
Published: August 2007

AbstractTwo Moroccan sites have been selected to be characterized for the ELT telescopes. Those sites are in the Atlas, between Oukaïmeden (where the national observatory is situated) and the Canary Islands. For this preliminary study, we have used the Nimbus-7 TOMS aerosol index to derive the astronomical extinction. This work builds on the findings of an earlier study which established the link between these two parameters over the Canary Islands.
Astronomy in Thailand
Authors: Kramer Busaba 
Published: August 2007

AbstractDuring the last few years, Thailand has seen a significant change in the way astronomical research and education is pursued in the country. The government has approved the establishment of the National Astronomical Research Institute of Thailand (NARIT) which aims to develop not only astronomical research but also astronomy education at all levels, both in formal and informal education. A framework of national key projects exists which includes national facilities, national collaborative research networks, teacher training and public outreach programmes. Examples of these programmes will be presented in this paper.