bluuebunny/crossref_metadata_2025_split huggingface dataset:
II.—On the History and Antiquities of Paphos
Authors: James M. R. 
Published: June 2019

In this section of the Report it will be my object to present as complete a statement as I can of what is known and what has been written on the subject of Paphos; and this should include a short specification of the chief points on which the late excavations either have thrown, or may be expected to throw, more light. On large and general questions, such as the origin and history of the Aphrodite worship in general, or even its history in the whole of Cyprus, I cannot enter here.It is inevitable that the chapter must consist largely of quotations. The source of these is not far to seek. Meursius' ‘Cyprus’ in Creta, Cyprus, et Rhodos (Amsterdam, 1675, in 4to) contains a wonderfully comprehensive survey of the ancient literature of the subject. An essay by Frederick Münter, Bishop of Seeland, carries this survey a stage further, and makes some further additions to it. This essay is entitled, Der Tempel der Himmlischen Göttin zu Paphos (Copenhagen, 1824, 4to). It forms a supplement to his former tract, Religion der Karthager. It is illustrated with four plates, and supplemented by an architectural essay on the plan of the temple, from the pen of Gustav Friedrich Hetsch. These two books have assisted me to most of my quotations. I have added a few others from later books, and from my own reading.
Inscription on a Limestone Block
Authors: Hicks E. L. 
Published: June 2019

Letters Slight apices. Date about 200 B.C.; not earlier. Line 1: iota adscriptum possibly omitted in Line 21: for see I.B.M. 925 (Branchidae). In line 12 there is a space after indicating a stop, but Mr. Paton cannot find any trace of after Telmissos is described by Polemo (apud Suidam s.v.) as a town in Caria at a distance of sixty stadia from Halicarnassos [which answers very nearly to the distance between Budrum and the site above Ghiöl (J. L. M.)]. It has been frequently confused with its namesake, an important city in the west of Lycia. But we may take it for granted now that it was the little Carian town that was so famous in ancient times for its augury. Cicero is quite explicit on the point (De Divin. i. 41): Telmessus in Caria est, qua in urbe excellit haruspicum disciplina; and again in ch. 42: Turn Caria tota, praecipueque Telmesses, quos ante dixi, quod agros uberrimos maximeque fertiles incolunt, in quibus multa propter fecunditatem fingi gignique possunt, in ostentis animadvertendis diligentes fuerunt.
Inferences about Seeing
Authors: Alexander Peter 
Published: June 2019

In his book Attention, Professor Alan White says ‘When you see X, it follows that if X is Y, you see Y whether you realise it or not.’ If, in passing through Paris, I saw a tall complex iron structure and that structure is the Eiffel Tower, then I saw the Eiffel Tower whether I realised it or not. I accept this, but because recent philosophical writings and discussions have cast doubt on the validity of the inference-patternI saw x; x is y; so I saw yand certain related patterns, it is clear that we cannot be content with this unvarnished statement. Various entertaining examples are produced to show that some instances of this pattern are invalid and therefore that the pattern itself is invalid. If I saw Jones at noon and at noon Jones was bribing Smith then, it is alleged, I cannot conclude that I saw Jones bribing Smith. Similarly, it is said, from the facts that I saw a man in the far distance and that that man was my father, I cannot conclude that I saw my father in the far distance; from the facts that I saw a foot and that that foot was Lloyd George's I cannot conclude that I saw Lloyd George.
Internal Motions of Trapezium Systems
Authors: Allen Christine , Poveda Arcadio , Hernández-Alcántara Alejandro 
Published: June 2019

AbstractThe separations of the various components of 44 trapezia as a function of time are studied, taking advantage of many new, high precision observations for these objects. A previous study revealed that some systems have components moving with velocities larger than the escape velocity (Allen et al.1974). The present work updates our previous study, extending the observations by about 30 years, and thus allowing an improved determination of the relative transverse motions of the components. The analysis of the new data confirms the conclusions we reached in our previous work: most of the trapezia show the internal motions expected for bound, virialized small clusters, but a few have escaping components. The available observational material lends support to the concept that trapezia are unstable systems with lifetimes of the order of a few million years.
Modelling the Dust Emission of the L1551 IRS5 Binary System
Authors: Osorio M. , D’Alessio P. , Muzerolle J. , Calvet N. , Hartmann L. 
Published: June 2019

AbstractWe model the L1551 IRS5 source as a system containing two protostars, each surrounded by a circumstellar disk, both encircled by a circumbinary disk, and all disks surrounded by an extended infalling flattened envelope With this composite model, we can calculate self-consistently the spectral energy distribution of the source the shape of the ice and silicate features, and the spatial intensity distributions of the envelope and disks. We compare our model results with the observations, determining the physical parameters of the disks and the envelope. We find that flattened envelope collapse models are required in order to explain the observations and that the infall rate of the envelope is much larger than the accretion rates of the binary disks.
SN 1987A at Radio Wavelengths
Authors: Staveley-Smith L. , Manchester R.N. , Gaensler B.M. , Kesteven M.J. , Tzioumis A.K. , Bizunok N.S. , Wheaton V.C. 
Published: June 2019

SummarySN1987A has an intrinsic radio luminosity some four orders of magnitude less than SN1993J at maximum, largely a reflection of the tenuous wind . from the progenitor of SN1987A before explosion. Both remnants have an edge-brightened, ring-like morphology though, in the case of SN1987A, the expansion rate is currently only around 3500 km s−1. The flux density of the remnant of SN1987A continues to rise at all measured radio frequencies. Its spectral index is gradually flattening, indicating its transition into the supernova remnant phase. A campaign to increase the resolution of radio imaging by observing at higher frequencies is underway with the Australia Telescope Compact Array (ATCA).
Dynamical Evolution of v-cooled Disks Following Compact Binary Mergers
Authors: Lee William H. 
Published: June 2019

SummaryUnderstanding the dynamical evolution of post-merger accretion disks over a long timescale (comparable to their lifetimes) is essential to determine if these can power short GRBs. Here we present preliminary results of such a study, spanning 0.2 seconds, by using a realistic equation of state and taking into consideration the effects of neutrino cooling (the main agent, given the physical conditions in the disks).
Expected Changes of SNe with Redshift due to Evolution of Their Progenitors
Authors: Domínguez Inma , Höflich Peter , Straniero Oscar , Limongi Marco , Chieffi Alessandro 
Published: June 2019

SummaryWe have analyzed the influence of the stellar populations, from which SN progenitors come, on the observational outcome, including the metal free Pop. III. We use our models to study the evolution of the progenitor, the subsequent explosion and the light curves. For Type Ia, the variation of the main sequence mass of the progenitor of the exploding WD produces an offset in the maximum-decline relation of 0.2 mag. This effect is critical for the use of high redshift Type Ia SNe as cosmological standard candles. In contrast, the metallicity does not change the above relation (at maximum, ΔMV ≤0.06 mag). For Type II, we find a dependence of the light curve properties with both main sequence mass and metallicity of the progenitor, and we identify a rather homogeneous subclass, “Extreme II-P,” that may be used as a quasi-standard candle. Note that, although not as good as Type Ia for distance determinations, Type II are expected to have occurred since the first stars were formed.
Ultraprecise Photometry from Space: The MOST Microsat Mission
Authors: Matthews J. M. , Kuschnig R. , Walker G. A. H. , Pazder J. , Johnson R. , Skaret K. , Shkolnik E. , Lanting T. , Morgan J. P. , Sidhu S. 
Published: June 2019

AbstractMOST (Microvariability & Oscillations of STars / Microvariabilite et Oscillations STellaire) is a Canadian microsatellite mission intended to detect rapid photometric oscillations at theμmag level in stars brighter thanV∼ 6. This limit is set primarily by the 15-cm aperture of the MOST telescope. The small size and mass of the MOST bus (similar to a suitcase) sets a limit on the pointing accuracy of about ±10 arcsec. To achieve the required photometric precision under these conditions, the MOST focal plane features a set of Fabry microlenses which can spread the target starlight into a pupil image of the telescope onto a CCD. The large size (∼1600 pixels) and positional stability (±0.1 pixel) of these images makes MOST insensitive to CCD flat-fielding errors. MOST is currently on schedule to be launched in early 2002.
Short Period M Giant Stars in the Hipparcos Catalogue
Authors: Koen Chris , Laney Dave 
Published: June 2019

AbstractA number of M giant stars with periods of the order of a few days were discovered by the Hipparcos mission. Similar stars may also have been found by other large-scale surveys. Parallaxes and colour indices of a sample of these stars were used to estimate their radii, temperatures and luminosities. It is shown that it is very unlikely that they are ellipsoidal or spotted variables, and that they are most likely pulsating in high overtone modes.
Link between Mass-Loss and Variability Type for AGB Stars?
Authors: Ivezić Željko , Knapp Gillian R. 
Published: June 2019

AbstractWe discuss difficulties in explaining the distribution of AGB stars in the 25–12 vs. 12–K color–color diagram by steady-state radiatively driven models, and propose that the discrepancy may be due to changes of mass-loss rate with the time scales of ∼ 100 yr.
The Distance to the Large Magellanic Cloud
Authors: Popowski Piotr 
Published: June 2019

AbstractI demonstrate that the two unexpected results in the local Universe: anomalous intrinsic (V – I)0 colors of RR Lyrae stars and clump giants in the Galactic center, and very short distances to Magellanic Clouds inferred from clump giants, can be at least partially resolved with a modified coefficient of selective extinction AV/E(V – I). With this modification, I find a new clump-giant distance modulus to the Large Magellanic Cloud, μLMC = 18.27 ± 0.07, which is 0.09 larger than the Udalski (1998b) result. When distance estimates from the red clump, RR Lyrae stars and the eclipsing binary HV2274 are combined, one obtains μLMC = 18.31 ± 0.04 (internal).
The Distance to the Galactic Center
Authors: McNamara D. H. , Madsen J. B. , Barnes J. , Ericksen B. F. 
Published: June 2019

AbstractThe Optical Gravitational Lensing Experiment (OGLE) data on high-amplitude δ Scuti Stars (HADS) and RR Lyrae stars have been analyzed to determine the distance to the galactic bulge. We find a mean value of 14.47 ± 0.08 mag for the bulge distance modulus. A small additive correction leads to 7.9 ± 0.3 kpc as the best distance to the galactic center.
Cepheid Distance to the Virgo Cluster
Authors: Mazumdar Anwesh , Narasimha D. 
Published: June 2019

AbstractA reanalysis of the HST data on Cepheids in the Virgo cluster spiral M100 is presented, based on our study of the Galactic Cepheids. A distance modulus of 31.49 mag is derived, which is higher than the HST Key Project value of 31.04 mag obtained from the same data earlier (Ferrarese et al. 1996). The increase in the distance is caused by nearly equal contributions from a different calibration of the slope and the zero point of the period–luminosity relation and a correction for the flux-limited incompleteness bias.
Pulsational Amplitudes of Cepheids – Their Application to Reveal Companions
Authors: Szabados László 
Published: June 2019

AbstractTwo parameters are defined involving the observed (peak-to-peak) amplitudes in U, B, V, and R photometric bands as well as that of the radial velocity variation. They are used to detect companions to Cepheids for a sample about 300 Galactic Cepheids.
The Instability Strip of M3
Authors: Bakos G. Á. , Jurcsik J. 
Published: June 2019

AbstractWe present new multicolour CCD photometry of the central part of the globular cluster M3, mapping the precise position of ~ 120 RR Lyrae stars (RRab, RRd, RRc) on the horizontal branch (HB). The location of the double-mode variables (RRd) is in perfect agreement with recent theoretical results. We find a significant internal spread of metallicity amongst the RRab variables.
Theory of Amplitude Modulation II. The Resonant Mode Interaction Model
Authors: Van Hoolst Tim 
Published: June 2019

AbstractWith about one fourth of the RRab stars showing the Blazhko effect, amplitude modulation on long time scales is a common phenomenon in stellar pulsation. The role of nonradial oscillation modes is studied here, and it is proposed that the amplitude modulation is a result of a dynamical, nonlinear resonance between the observed radial mode and a low-degree nonradial mode. In this scenario, a nonradial mode is resonantly excited in Blazhko-type RR Lyrae stars. Degree one modes are found to have the highest probability of being excited and a crucial test of the model would be the observational determination of the degree of the proposed nonradial mode.
Mixing in the SMC Stars: Implication for Cepheids
Authors: Cordier D. , Lejeune T. , Lebreton Y. , Goupil M.-J. 
Published: June 2019

AbstractWe compare the recent OGLE 2 data of stars in the Small Magellanic Cloud (SMC) with stellar evolutionary models of low metallicity computed with the updated and numerically accurate code CESAM. The conversion between theoretical and observational data has been carefully done using the BaSel Library. This enables us to derive new observational constraints at SMC chemical composition: on the overshooting parameter αover during the main sequence, and on the mixing-length parameter αMLT for the red giant branch. The occurrence of an instability strip-crossing episode is strongly related to these mixing parameters.
Understanding Pulsations in OB Stars
Authors: Balona L. A. 
Published: June 2019

AbstractOur understanding of pulsations in β Cep, SPB and ζ Oph stars is discussed. We do not understand why there are no β Cep stars earlier than O9, though the models show that the instability strip extends to hotter stars. The main problem among the SPB stars is why rotation has a strong inhibiting effect on pulsation. The ζ Oph stars are an extension of the β Cep and SPB stars to higher spherical harmonic degrees. The pulsational stability of models of B stars to modes of high degree is discussed. Results are compared with two well observed ζ Oph stars. Although there is good agreement with ζ Oph itself, the periods of the high-degree modes in α Vir are incompatible with model predictions.
CCD Studies of δ Scuti Stars in Open Clusters
Authors: Kjeldsen Hans 
Published: June 2019

AbstractAsteroseismology on δ Scuti stars has until now produced very few convincing results – if we aim at doing strong tests of details of stellar modelling. The main reason for the lack of success is probably that these stars often rotate, which split nonradial oscillation frequencies into many more frequencies. These many frequencies and the fact that the more evolved δ Scuti stars contain a strong chemical composition gradient at the edge of the convective core, produce a very complicated eigenfrequency spectrum. In contrast to this, we expect, in principle, seismological studies of δ Scuti stars to be a very simple task: One has to compare theoretical oscillations in model stars with the observed oscillations. However, in order to produce convincing asteroseismological results, we need to do three things: (1) Detect as many eigenfrequencies as possible at high precision, (2) identify the eigenmodes and (3) improve the theoretical models. By observing δ Scuti stars in open clusters using CCDs, we have a possibility to improve on (1) and (2) as well as providing an opening for an improvement in the theoretical models by doing accurate calibrations of the basic cluster properties. In this paper I shall describe some of the results from CCD studies of δ Scuti stars in open clusters and identify some future prospects for this technique.
Optical Variability of the λ Eri Star HD 105382: Pulsation or Rotation?
Authors: Briquet M. , Aerts C. , De Cat P. 
Published: June 2019

AbstractHD 105382 is clearly a monoperiodic, very active λ Eri star with the frequency 0.7721 d−1. Its photometric behaviour and the moment variations are not typical for a standard pulsational model.
Time-Series CCD Photometry of Northern Open Clusters Using the BOAO 1.8-m Telescope: III. NGC 2301
Authors: Kim S.-L. , Park B.-G. , Chun M.-Y. , Sung H. , Jeon Y.-B. , Yuk I.-S. , Ann H. B. , Lee S. H. , Lee M. G. 
Published: June 2019

AbstractA time-series CCD photometric survey of variable stars in open clusters has been in progress using 1.8-m telescope at the Bohyunsan Optical Astronomy Observatory (BOAO) in Korea. We present preliminary results of time series photometry for the intermediate-age open cluster NGC 2301.
Pulsation Investigation of V647 Tau – Preliminary Results of STEPHI Campaign in 1997
Authors: Liu Y. Y. , Michel E. , Barban C. , Garrido R. , Alvarez M. , Hernández M. M. , Belmonte J. A. 
Published: June 2019

AbstractV647 Tau was observed during a 1997 STEPHI campaign; 228 hr of observations in v were obtained, together with another 50 hr of simultaneous data in y. The data were analyzed and main results are discussed in the text.
Time Scales for Period Change in Pulsating White Dwarf Stars
Authors: Kepler S. O. , Costa J. E. S. , Winget D. E. , Reed M. D. , Kawaler S. D. 
Published: June 2019

AbstractWe have used the rate of change of pulsation period for the hot (DOV) pre-white dwarf PG1159–035 and the cool (DAV) white dwarf G117–B15A to measure their evolutionary time scales. We show that, for any multiperiodic star, we must take into account the effect of all pulsations simultaneously on the times of maximum of the pulsations to get reliable measurements of periods and phases.
Absolute Spectrophotometry of Be Stars
Authors: Stiff T. , Jeffers S. 
Published: June 2019

AbstractAbsolute spectrophotometry data have been obtained for a sample of Be stars. These data were obtained with the York Observatory 60 cm telescope and vidicon spectrophotometer. The data have been corrected for differential atmospheric extinction, instrumental response, and interstellar extinction and calibrated in terms of absolute flux. Absolute Hα and Hβ fluxes have been determined.
The Far UV Spectrum of the Binary System AX Mon
Authors: Danezis E. 
Published: June 2019

AX Mon is early indicated in the literature as a double system (Merrill 1952). Cowley (1964) noted that the system consists of a rapidly rotating B3 star and a somewhat fainter K giant.We describe in this paper the main features of the far UV spectrum of HD 45910 observed with IUE at phase 0.5 (SWP 4762, LWR 4131). An analysis of this spectrum has been presented as part of a Ph.D. thesis (Danezis 1983). The far UV spectrum of AX Mon presents a large range of ionization stages going from CI, 01, NI, Mgl to SiIV, CIV, NV.
Reflections on Be Stars and the Be Phenomenon
Authors: Plavec Mirek J. 
Published: June 2019

AbstractAfter three specialized meetings on Be stars, it: appears that the Be phenomenon is more complicated than we have thought. Five fundamentally different models are now competing. All five are actually based on an assumption that the Be stars are only a specialized (perhaps more easily noticeable) case of a more general phenomenon. Carefully arranged observations may decide between competing concepts, for example between spheroidal and disk-shaped circumstellar envelopes, and they can decide on the location of the cool strata (emitting Balmer lines) and hot strata (N V, C IV, Si IV). Eclipsing interacting binaries provide valuable clues.
An Optical P – L Relation for LPVs
Authors: Pierce M.J. , Crabtree D.R. 
Published: June 2019

Supergiant Long-Period Variables (LPVs) are both more luminous and more common than Cepheids. The fact that a P – L relation exists at K (e.g. Wood et al. 1983 ApJ, 272, 99; Mould et al. 1990 ApJ, 349, 503) and not at visible wavelengths is usually attributed to the strong temperature sensitivity of TiO, which dominates the spectra of these stars in the visible. This has led us to apply a narrow bandpass (λ0 = 8250Å, BW = 350Å), avoiding TiO, in the hopes that an optical P – L relation can be found.The data for Per OB1, the LMC, and M 33 are shown in figure 1. The small dispersion (σLMC = 0.22 mag.) and flat slope are evident. Combining the data we find:(1)with the absolute calibration from the ten LPVs in Per OBI, assuming m – M = 11.8±0.2 (Garmany & Stencel 1992 AAS, 94, 211).
Seismology of Pulsating Ap Stars: Results From The Past Decade, Prospects For The Next
Authors: Matthews Jaymie M. 
Published: June 2019

AbstractSince the discovery of the first rapidly oscillating Ap (roAp) star in 1978 by Kurtz, this class of magnetic chemically-peculiar pulsators has grown to over two dozen. The eigenfrequency spectra of roAp stars (with periods of ∼ 6 – 15 min) are consistent with nonradialp-modes of low degreeand high overtonen, not unlike the Sun's five-minute oscillations seen in integrated light. However, unlike the Sun, the strong global dipole fields of roAp stars significantly affect the pulsations.Although much of the effort in the last decade has been towards detecting new roAp candidates and refining the frequencies of known variables, initial “seismic” analyses have already yielded important results. Measurements of fundamental frequency spacingsconstrain the luminosities and radii of some roAp stars. In addition, mode splitting provides: (1) an independent determination of rotation period, even in the absence of longer-term light variations; (2) limits on the rotational inclinationiand magnetic obliquityβ; and (3) an indication of the relativeinternalfield strengths of certain roAp stars. Very recently, the temperature - optical depth structure of the atmosphere of HR 3831 was inferred from optical and IR photometry of its oscillations.Judging from current developments, the next decade promises exciting results on both observational and theoretical fronts. Several roAp stars have now been monitored for over a decade, allowing us to investigate long-term period changes due to evolution, binarity, etc. Eigenfrequency models for stars in the mass and radius range appropriate for Ap stars are becoming available, as well as explicit treatments of the perturbations due to magnetic fields. Armed with these, we may be able to place some roAp stars on a theoretical(or “asteroseismological H-R“) diagram to derive independently their masses and main-sequence ages.