bluuebunny/crossref_metadata_2025_split huggingface dataset:
The 6dF Galaxy Survey: Mass and Motions in the Local Universe
Authors: Colless Matthew , Jones Heath , Campbell Lachlan , Burkey Daniel , Taylor Andy , Saunders Will 
Published: June 2019

The 6dF Galaxy Survey will provide 167 000 redshifts and about 15000 peculiar velocities for galaxies over most of the southern sky out to about cz = 30000 km s--1. The survey is currently almost half complete, with the final observations due in mid-2005. An initial data release was made public in December 2002; the first third of the dataset will be released at the end of 2003, with the remaining thirds being released at the end of 2004 and 2005. The status of the survey, the survey database and other relevant information can be obtained from the 6dFGS web site at http://www.mso.anu.edu.au/6dFGS.In terms of constraining cosmological parameters, combining the 6dFGS redshift and peculiar velocity surveys will allow us to: (1) break the degeneracy between the redshift-space distortion parameter β = Ω0.6m/b and the galaxy-mass correlation parameter rg; (2) measure the four parameters Ag, Γ, β and rg with precisions of between 1% and 3%; (3) measure the variation of rg and b with scale to within a few percent over a wide range of scales.
Diffuse molecular clouds at high galactic latitude
Authors: Stark Ronald 
Published: June 2019

The IRAS 60 and 100 μm flux from cirrus clouds are commonly explained by dust continuum emission. But this explanation in some cases requires unexpectedly high dust temperatures.We argue that the contribution of fine structure emission of neutral oxygen, O°(63 μm), can be significant in the IRAS 60 μm band. The 0°(63 μm) line emission together with the dust continuum emission offers a plausible explanation of the observed flux ratio I(60)/I(100), as well as of its variation across individual clouds. We also discuss the clumpy/filamentary structure of these clouds.
Bright-rimmed clouds with IRAS point sources: candidates for star formation by radiation-driven implosion
Authors: Sugitani Koji , Fukui Yasuo , Ogura Katsuo 
Published: June 2019

We present preliminary results of a survey of bright-rimmed clouds associated with IRAS point sources.Bright-rimmed globules associated with old HII regions have long been suspected as a potential site for star formation. Physical conditions of such clouds seem to well match to models of radiation-driven implosion, which have been studied as an effective process for induced star formation (e.g. Klein et al. 1985, Bertoldi 1989). Bright-rimmed globules associated with IRAS point sources are good candidates for the sites of induced star formation. Three well-established cases of radiation-driven implosions in bright-rimmed globules (Ori I-2, IC1396-n, and L1206) were reported (Sugitani et al. 1989). Similar examples were also reported in HH46/47 (Olberg et al. 1989) and in GN21.38.9 (Duvert et al. 1990). However, the samples are still not numerous enough to establish comprehensive understanding of star formation by such implosion process.
Old and New Tools for Understanding the Evolution of Stars in Clusters
Authors: D'Antona Francesca 
Published: June 2019

The uncertainties in the modelling of some important inputs of stellar evolution must be taken into account for a correct interpretation, both of the HR diagrams of individual stars, and of the integrated colors, of stellar clusters. After a short discussion of Globular Cluster ages, we focus on the problem of convection and discuss the parametrization of convection efficiency and overshooting.Convective efficiency affects the reliability of the giants colors, especially for high metallicity: age - metallicity relations found from integrated colors of clusters must be regarded with caution.Non-instantaneous mixing, both in the formal convective region and in the overshooting region must be taken into account: this is necessary to compute nucleosynthesis in ‘hot bottom burning’ envelopes, but it may also affect the color distribution in clump (core helium burning) stars, as shown here for the case of the LMC cluster NGC 1866.
On the Problem of the Mechanism of the Origin of Stars in Stellar Associations
Authors: Ambartsumian V. A. 
Published: June 2019

Almost ten years have passed since the idea of stellar associations as nonstable stellar systems was formulated. The complex of observational data obtained during this time indicates that stars contained in the associations are young objects of some million years of age. We would like to stress here that this concerns both the O and T associations. It is also known that those O associations which could be sufficiently investigated in this respect, contain, as a rule, T Tauri type stars and are consequently T associations as well. There are, on the other hand, T associations which do not contain hot giants. But apparently the mechanisms of stellar formations must be similar in O and T associations. This means that any theory of stellar origin for a given type of association must permit variations, which will provide an explanation of the origin of stars in associations of other type.Two hypotheses on the origin of stellar associations have been thus far discussed. One of them, suggested by the author at the initial stage of the idea about associations, supposes that each association has originated as a result of an expansion from a body or a system, the volume of which was initially very small. The dimensions of the latter was in any case less than one parsec. According to this point of view, these initial bodies (protostars) have either not been observed up to the present, or have not yet been identified with any known object. This point of view does not give any indication about a concrete mechanism of stellar origin, postponing its explanation to the time, when the earliest stages of the expansion of the association may be studied in detail.
Non-Radial Oscillations
Authors: Ledoux P. 
Published: June 2019

The problem of the adiabatic non-radial oscillations of spherical stars is reviewed and results recalled for a variety of models. The anomalous behaviour of the eigenfunctions for highly condensed models is related to the apparent mobile singularities depending on the eigenvalues. Tables of Q-values are provided to facilitate possible applications to variable stars.In the case of the gravity modes, the existence of multiple spectra some stable (g+ modes) some unstable (g− modes) if superadiabatic and subadiabatic regions alternate is discussed and the interest of further investigations underlined.As far as vibrational stability (effects of the non adiabatic terms) is concerned, a general expression is given for the ‘damping coefficient’. The attention is drawn to the possibility for g+ modes of becoming vibrationally unstable under the effect of various factors and in various models, including the Sun where this was advocated as a possibility of relieving the neutrinos difficulty.Finally the present status of the most obvious candidates among variable stars for non-radial oscillations, the β Canis Majoris stars and the rapid blue variables (white dwarfs) is briefly reviewed.
The Sun as a Pulsating Rotating Star
Authors: Schatten Kenneth H. 
Published: June 2019

Physical arguments are provided which suggest the following:(a) The Sun rotates rapidly internally, with a period near one day. The arguments are based upon a low ‘effective’ plasma dynamic viscosity associated with a negative ‘effective’ magnetic density, ϱM = −B2/4πν2. This low (near zero) viscosity allows several calculations of the angular velocity of the solar core to be made. A fluid dynamical argument based upon the inviscous Navier-Stokes relation shows that for objects seated in a non-expanding magnetohydrodynamic fluid, the usual Kepler law should be replaced by T2 ∝ r4.(b) The rapid rotation suggests that the solar magnetic field is deeply buried and, furthermore, that the Sun violates the Ferraro theorem. This violation results from a radial electric field necessary to support the solar plasma. This radial field requires the Sun to be charged with a charge q = + 2 × 1011 esu. Thus the Sun's differential rotation may be viewed as arising from B']θ=0 in the rest frame of the fluid where Er ≠ 0 or alternatively as a polar spin down by the solar wind flow. Thús in the fluid frame, the solar activity cycle may be viewed as an Alfvén wave, with T= Ω/vA = 20 yr. The velocity of material along the field is such that (G−1 cm−2 s−1), governed by the collapse of mass in the solar core; (4H + 4e → 1He + + 2e) results in a reduction of gas pressure unless ~7 × 1014 gm s−1 of material continually collapse so as to conserve the particle number in the solar interior.(c) This requires the Sun to emit gravity waves with an energy comparable to its luminosity. The virial of the nuclear reactions in the core governs whether the energy goes into gravity waves or heat. A variable positron-electron core allows this.
Data for Probing the Sun
Authors: Elsworth Yvonne 
Published: June 2019

The observations of solar oscillations provide an unrivalled, precise way of probing the solar interior. In this paper, I consider the observations and their interpretation in terms of the physics of the Sun. The oscillations that we are concerned with here are the so-called p modes, i.e. oscillations for which pressure is the restoring force. The modes for which gravity is the restoring force have yet to be unambiguously detected on the Sun. The observations are made either as Doppler velocity or as intensity and are, in general, very small effects. To get an impression of the precision required, consider that in integrated velocity the total signal is ~ 1 m s−1 with the strongest individual modes being about 15-20 cm s−1. The weakest, detected modes are of order a few mm s−1. When this signal is measured as a Doppler shift, v/c is a few parts in 1011. The observations are made by a variety of instruments on Earth or in Space which can be simply divided into those which observe the Sun as a star and those which image the solar surface into many pixels Although there are many different observers using many different techniques, in all cases one is analysing light emitted from a region relatively high in the atmosphere of the Sun. When one considers how these measurements can be interpreted in terms of the solar oscillations, two issues arise:
1.Roughly where in the solar atmosphere are the lines formed?2.How different are the heights of formation for different lines?
Low-Degree P-Mode Solar Cycle Trends from Bison Data
Authors: Chaplin W.J. , Elsworth Y. , Isaak G.R. , McLeod C.P. , Miller B.A. , New R. 
Published: June 2019

An in-depth discussion of the analysis presented here can be found in an up-coming paper (Chaplin et al., 1997).In order to investigate the solar-cycle dependence of the low-degree p-mode frequencies, we have analysed eighteen 4-month frequency spectra generated from BiSON Doppler velocity residuals collected between 1991 January 01 and 1997 January 05. These data cover the falling phase of solar activity cycle 22. up to the cycle 22/23 boundary. Fig. 1(a) shows frequency shifts, averaged over two orders in n. up to ~ 3900 μHz - as derived from the analysis of the 4-month spectra - normalised to unit change in the 10.7-cm radio flux. The dashed line lying above the BiSON data is a fit to the BBSO 1989-minus-1986 frequency shifts, for 4 ≤ ℓ ≤ 140 (Libbrecht k Woodard. 1991). The dotted line passing through the data corresponds to the bestscaled fit of the BBSO data to the BiSON data - the best-fit requires the BBSO data to be scaled by 0.71 ± 0.03. This is reasonably consistent - as expected - with the mean, overall ratio of the inverse mode masses of those data used in the BiSON and BBSO analyses (≈ 0.67). Fig. 1(b) shows the BiSON activity-normalised frequency shifts, plotted as a function of inverse mode mass - here, as anticipated, there is a clear correlation between the variables.
Acoustic Imaging and Subsurface Absorption Structure of Sunspots
Authors: Chang H.-K. , Chou D.-Y. , Labonte B. 
Published: June 2019

Recently, Chang et al. (1997, hereafter Paper I) developed a new method, based on time-distance curves (Duvall et al. 1993), to construct a three-dimensional acoustic intensity image of the solar interior. Here we report results from another data set.Solar p-mode waves, which are continually generated and dissipated stochastically by the turbulent convection, are scattered and absorbed by local inhomogeneities. If we appropriately add p-mode waves observed at the surface, based on the knowledge of how the waves propagate (time-distance curves), such that acoustic signals emanating from a particular point at a particular time are collected in phase, we can reconstruct the p-mode amplitude at the target point at the target time. The scheme of adding signals from a target point in phase plays the same role as a lens in optics. Thus we call it the “computational acoustic lens” (Paper I). This imaging technique can be used to construct acoustic amplitudes at any point in the solar interior based on the time-distance curve between that depth and the surface, which can be computed from a standard solar model based on the ray theory. The time series of constructed a plitudes provides information of both the intensity and the phase of the wavetrain. The intensity can be used to study p-mode absorption regions, and the phase can be used to probe other properties of local inhomogeneities, such as flow and change in wave speed.
High-energy Galactic phenomena and the interstellar medium
Authors: Cesarsky Catherine J. 
Published: June 2019

Gamma rays of energy in the range 30 MeV-several GeV, observed by the satellites SAS-2 and COS-B, are emitted in the interstellar medium as a result of interactions with gas of cosmic-ray nuclei in the GeV range (π° decay γ rays) and cosmic-ray electrons of energy > 30 MeV (bremsstrahlung γ rays). W. Hermsen has presented at this conference the γ ray maps of the Galaxy in three “colours” constructed by the COS-B collaboration; the information in such maps is supplemented by radio-continuum studies (see lecture by R. Beck), and is a useful tool for studying the distribution of gas, cosmic rays (c.r.) and magnetic fields in the Galaxy. The variables in this problem are many:large-scale (~ 1 kpc) and small-scale (~10 pc) distributions of c.r. nuclei, of c.r. electrons, of atomic and molecular hydrogen, of magnetic fields, fraction of the observed radiation due to localized sources, etc. Of these, only the distribution - or at least the column densities - of atomic hydrogen are determined in a reliable way. Estimates of the amount of molecular hydrogen can be derived from CO observations or from galaxy counts. The radio and gamma-ray data are not sufficient to disentangle all the other variables in a unique fashion, unless a number of assumptions are made (e.g. Paul et al. 1976). Still, the COS-B team has been able to show that :a) there is a correlation between the gamma-ray emission from local regions, as observed at intermediate latitudes, and the total column density of dust, as measured by galaxy counts. The simplest interpretation is that the density of c.r. nuclei and electrons is uniform within 500 pc of the sun, and that dust and gas are well mixed. Then, γ rays can be used as excellent tracers of local gas complexes (Lebrun et al. 1982, Strong et al. 1982).b) In the same way, the simplest interpretation of the γ-ray emission at energy > 300 MeV from the inner Galaxy, is that c.r. nuclei and electrons are distributed uniformly as well : there is no need for an enhanced density of c.r. in the 3–6 kpc ring; on the contrary, even assuming a uniform density of c.r., the γ-ray data are in conflict with the highest estimates of molecular hydrogen in the radio-astronomy literature (Mayer-Hasselwander et al. 1982).c) In the outer Galaxy, the gradient of c.r. which had become apparent in the early SAS-2 data can now, with COS-B data, be studied in three energy ranges. A gradient in the c.r. distribution is only required to explain the low-energy radiation, which is dominated by bremsstrahlung from relativistic electrons (Bloemen et al., in preparation).
III / Summary of Mogollon Branches and Sites
Authors: Wheat Joe Ben 
Published: June 2019

The first Mogollon branch defined was the Mimbres. Here, sites have been excavated in the southern part of the Mimbres drainage and in the adjacent part of the Gila drainage.Harris Village (Haury 1936b) is located about a quarter of a mile east of the Mimbres, New Mexico post office, on a large, flat terrace which rises abruptly some 20 m. above the east bank of the Mimbres River. It is about 1,850 m. above sea level. The village occupied several acres, part of which was not explored. Easily approached from all sides, defense does not seem to have been a factor in selecting the village site. The surrounding countryside is rugged and hilly, but agricultural land is available in small fields along the stream. The area is in the lower part of the pinyon-juniper belt, and a few trees occur on the site. Cottonwood, poplar, and walnut grow along the valley.
VI / Mogollon Pottery
Authors: Wheat Joe Ben 
Published: June 2019

The Mogollon Culture begins with the addition of pottery to the last phase of the Cochise Culture. Pottery was the last distinctive element to be added, for architecture and agriculture had been a functioning part of the culture for perhaps a thousand years or more. There can be little doubt that pottery was introduced from outside the area, for the earliest ceramic complex appears as a thriving industry with well established techniques. Technically this pottery is well made, and although only a limited number of shapes occur, it is by no means primitive.The main outline of Mogollon pottery development can be summarized briefly. The earliest horizon yet known contains polished brown and polished red wares. These wares, or variations of them, continue as basic wares of the ceramic complex throughout Mogollon history.
Prevalence of depression and burden among informal care-givers of people with dementia: a meta-analysis
Authors: Collins Rebecca N. , Kishita Naoko 
Published: June 2019

AbstractThis meta-analysis examined the prevalence of depression and burden among informal care-givers of people with dementia (PwD) and compared the prevalence of depression between male and female, and spousal and non-spousal, care-givers. The quality of studies was evaluated and moderator variables explored. A search of six electronic databases (PsycARTICLES, PsycINFO, MEDLINE Complete, SCOPUS, Web of Science and ProQuest) was conducted from the first available date to the 31 October 2017. Inclusion criteria involved observational studies on the prevalence of burden or depression among informal care-givers of PwD. Forty-three studies were examined with a total of 16,911 participants. The adjusted pooled prevalence of depression was 31.24 per cent (95% confidence interval (CI) = 27.70, 35.01) and burden was 49.26 per cent (95% CI = 37.15, 61.46), although heterogeneity among prevalence estimates was high. Depression prevalence estimates differed according to the instrument used and the continent where the study was conducted. The odds of having depression were almost one and a half times higher in female compared to male care-givers. No significant difference was observed between spouses and non-spouses. Most studies had a medium risk of bias. Results suggest a great need within this population for interventions that are effective at reducing burden and depressive symptoms. It therefore appears imperative for dementia services that are not providing such interventions to do so.
COMERCIO DE MERCANCÍAS LOCALES EN SANTIAGO DE CHILE, 1773–1778
Authors: Martínez Barraza Juan José 
Published: June 2019

ABSTRACTThis article deals with the trade of local merchandise in Santiago's district (Corregimiento) from 1773 to 1778, based on tributary sources. It contributes to the debate on the organization of the colonial internal market. The main traded merchandise, which represented about 80% of Chilean exports, came from the cattle exploitation that was developed in the haciendas around Santiago, whose cattle stocks were complemented from neighboring provinces in the Andes. The largest destination of this trade, in which big merchants acted together with a thousand minor merchants, were the retail channels and the artisan sectors supplying the population of Santiago. The impulse of this demand on the domestic market was so dynamic that it shows a degree of regional autonomy higher than what it is traditionally assumed for the Chilean economy in the late colonial period.
Current Status of the Microlensing Surveys
Authors: Paczyński Bohdan 
Published: June 2019

AbstractThe ongoing microlensing searches have generated more photometric measurements of pulsating stars than all previous observing projects combined. In particular, OGLE has made ∼ 340,000 B, V, and I-band measurements of ∼ 1,300 Cepheids in the Large Magellanic Clouds accessible over Internet. Microlensing searches contributed to the development of very efficient image subtraction software which works best in crowded fields. This suggests the use of a period – flux amplitude rather than period – luminosity relation for the Cepheids for distance determination, as the flux amplitude is directly measurable with the image subtraction, and it is not biased by crowding. Future projects will dramatically increase the data rate, will provide all-sky coverage and a complete census of variables, including pulsating stars, to the ever fainter limits. Time will show which approach, a small number of large teams or a large number of small teams, will be more productive.
Photometry of Pulsating Stars in the Magellanic Clouds as Observed in the MOA Project
Authors: Hearnshaw J. B. , Bond I. A. , Rattenbury N. J. , Noda S. , Takeuti M. , Abe F. , Carter B. S. , Dodd R. J. , Honda M. , Jugaku J. , Kabe S. , Kilmartin P. M. , Koribalski B. S. , Matsubara Y. , Masuda K. , Muraki Y. , Nakamura T. , Nankivell G. R. , Reid M. , Rumsey N. J. , Saito To. , Sato H. , Sekiguchi M. , Sullivan D. J. , Sumi T. , Watase Y. , Yanagisawa T. , Yock P. C. M. , Yoshizawa M. 
Published: June 2019

AbstractA review of the MOA (Microlensing Observations in Astrophysics) project is presented. MOA is a collaboration of approximately 30 astronomers from New Zealand and Japan established with the aim of finding and detecting microlensing events towards the Magellanic Clouds and the Galactic bulge, which may be indicative of either dark matter or of planetary companions. The observing program commenced in 1995, using very wide band blue and red filters and a nine-chip mosaic CCD camera.As a by-product of these observations a large database of CCD photometry for 1.4 million stars towards both LMC and SMC has been established. In one preliminary analysis 576 bright variable stars were confirmed, nearly half of them being Cepheids. Another analysis has identified large numbers of blue variables, and 205 eclipsing binaries are included in this sample. In addition 351 red variables (AGB stars) have been found. Light curves have been obtained for all these stars. The observations are carried out on a 61-cm f/6.25 telescope at Mt John University Observatory where a new larger CCD camera was installed in 1998 July. From this latitude (44° S) the Magellanic Clouds can be monitored throughout the year.
Blue Variables from the MOA Database
Authors: Noda Sachiyo , Takeuti Mine , Bond I. A. , Rattenbury N. J. , Abe F. , Carter B. S. , Dodd R. J. , Hearnshaw J. B. , Honda M. , Jugaku J. , Kabe S. , Kilmartin P. M. , Masuda K. , Matsubara Y. , Muraki Y. , Nakamura T. , Reid M. , Rumsey N. J. , Saito To. , Sato H. , Sekiguchi M. , Sullivan D. J. , Sumi T. , Watase Y. , Yanagisawa T. , Yock P. C. M. , Yoshizawa M. 
Published: June 2019

AbstractA large database of CCD photometry for 1.4 million stars towards both the LMC and the SMC, which has been established by the MOA project, is a useful resource to study variable stars. In our preliminary study, variables identified as β Lyrae type stars and Herbig Ae/Be stars have been found amongst blue stars.