1,725,930 research outputs found
Southern Pacific (SP) 3766
No full textA photograph postcard showing the Southern Pacific (SP) 3766, 2-10-2, Ogden, UT
Santa Fe (ATSF) 3766
No full textA photograph print showing Santa Fe 3766, 4-8-4, taking on water, Topeka, KS
Santa Fe (ATSF) 3766
No full textA photograph print showing Santa Fe 3766, 4-8-4, on passenger train with angular metal box attached to front end, Pasadena, CA. Box was a platform for test engineers
Santa Fe (ATSF) 3766 on "Chief"
No full textA photograph print showing Santa Fe 3766, 4-8-4, on No. 20 "Chief", meeting No. 3 east of Glorietta, NM
Block Card 3766 Schneider Road
No full textThis image was produced by the Auditor's Office in Lucas County, Ohio for tax assessment purposes. Associated dates are approximate. Descriptive terms related to this photograph include: Garrison Colonial Style | 3766 Schneider Road (Toledo, Ohio) | Dwelling | Crossgates Plat (Toledo, Ohio) | South Toledo Area (Toledo, Ohio
Light curves of the Be stars of NGC 3766
No full textAbstractNonradial pulsations (NRPs) are a possible formation mechanism for the equatorial disks surrounding Be stars. The open cluster NGC 3766 has a high fraction of transient Be stars, Be stars that have been observed with both emission due to a circumstellar disk and a non-emitting B-type spectrum. Because of the large fraction of transient Be stars, this cluster is a prime location for studying the formation mechanisms of Be star disks. We observed NGC 3766 for more than 25 nights over three years to generate Strömgren uvby light curves of the Be population. We present the results of a period search to investigate the presence of NRPs.</jats:p
The B and Be star population of NGC 3766
No full textWe present multiple epochs of Hα spectroscopy for 47 members of the open cluster NGC 3766 to investigate the long-term variability of its Be stars. Sixteen of the stars in this sample are Be stars, including one new discovery. Of these, we observe an unprecedented 11 Be stars that undergo disk appearances and/or near disappearances in our Hα spectra, making this the most variable population of Be stars known to date. NGC 3766 is therefore an excellent location to study the formation mechanism of Be star disks. From blue optical spectra of 38 cluster members and existing Strömgren photometry of the cluster, we also measure rotational velocities, effective temperatures, and polar surface gravities to investigate the physical and evolutionary factors that may contribute to the Be phenomenon. Our analysis also provides improvements to the reddening and distance of NGC 3766, and we find E(B - V ) = 0.22 ± 0.03 and (V - MV )₀ = 11.6 ± 0.2, respectively. The Be stars are not associated with a particular stage of main-sequence evolution, but they are a population of rapidly rotating stars with a velocity distribution generally consistent with rotation at 70%-80% of the critical velocity, although systematic effects probably underestimate the true rotational velocities, so that the rotation is much closer to critical. Our measurements of the changing disk sizes are consistent with the idea that transitory, nonradial pulsations contribute to the formation of these highly variable disks
Going Beyond Counting First Authors in Author Co-citation Analysis
No full textThe present study examines one of the fundamental aspects of author co-citation analysis (ACA) - the way co-citation
counts are defined. Co-citation counting provides the data on which all subsequent statistical analyses and mappings
are based, and we compare ACA results based on two different types of co-citation counting - the traditional type that
only counts the first one among a cited work's authors on the one hand and a non-traditional type that takes into
account the first 5 authors of a cited work on the other hand. Results indicate that the picture produced through this non-traditional author co-citation counting contains more coherent author groups and is therefore considerably clearer. However, this picture represents fewer specialties in the research field being studied than that produced through the traditional first-author co-citation counting when the same number of top-ranked authors is selected and analyzed. Reasons for these effects are discussed
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