130,648 research outputs found
Aegus fukiensis Bomans 1989
No full textAegus fukiensis Bomans, 1989 Aegus fukiensis Bomans, 1989. Nouv. Rev. Ent. (N. S.), 6(1): 21. TL: China, Fujian, Mt. Wuyishan. TD: BMNH. Distribution. China (Zhejiang, Fujian).Published as part of Cao, Yuyan, Webb, Michael D., Bai, Ming & Wan, Xia, 2016, New synonymies and records of the stag-beetle genus Aegus MacLeay from Chinese fauna (Coleoptera: Lucanidae), pp. 261-272 in Zoological Systematics 41 (3) on page 270, DOI: 10.11865/zs.201627, http://zenodo.org/record/461758
Aegus angustus Bomans 1989
No full textAegus angustus Bomans, 1989 Aegus angustus Bomans, 1989. Nouv. Rev. Ent. (N. S.), 6(1): 17. TL: China, Fujian, Mt. Wuyishan. TD: BMNH. Distribution. China (Zhejiang, Fujian, Hubei, Guangdong, Sichuan).Published as part of Cao, Yuyan, Webb, Michael D., Bai, Ming & Wan, Xia, 2016, New synonymies and records of the stag-beetle genus Aegus MacLeay from Chinese fauna (Coleoptera: Lucanidae), pp. 261-272 in Zoological Systematics 41 (3) on page 268, DOI: 10.11865/zs.201627, http://zenodo.org/record/461758
Aegus callosilatus Bomans 1989
No full text<i>Aegus callosilatus</i> Bomans, 1989 <p> <i>Aegus callosilatus</i> Bomans, 1989. <i>Nouv. Rev. Ent. (N. S.)</i>, 6(1): 20. TL: China, Fujian, Mt. Wuyishan. TD: BMNH.</p> <p>Distribution. China (Fujian).</p>Published as part of <i>Cao, Yuyan, Webb, Michael D., Bai, Ming & Wan, Xia, 2016, New synonymies and records of the stag-beetle genus Aegus MacLeay from Chinese fauna (Coleoptera: Lucanidae), pp. 261-272 in Zoological Systematics 41 (3)</i> on pages 268-270, DOI: 10.11865/zs.201627, <a href="http://zenodo.org/record/4617586">http://zenodo.org/record/4617586</a>
Aegognathus soulai Arnaud and Bomans 2004
No full text<i>Aegognathus soulai</i> Arnaud and Bomans, 2004 <p>(Figure 4a–d: paratypes, 3J)</p> <p> <i>Aegognathus soulai</i>, 2004: 5 (original combination and description)</p>Published as part of <i>Cáceres, Juan Sebastián D. & Grossi, Paschoal Coelho, 2023, Taxonomic revision of Aegognathus Leuthner, 1883 (Coleoptera: Lucanidae), pp. 557-595 in Journal of Natural History 57 (9 - 12)</i> on page 573, DOI: 10.1080/00222933.2023.2198736, <a href="http://zenodo.org/record/7975445">http://zenodo.org/record/7975445</a>
Bubble instability of mIIA on AdS4 × S6
No full textWe consider compactifications of massive IIA supergravity on a six-sphere. This setup
is known to give rise to non-supersymmetric AdS4 vacua preserving SO(7) as well as
G2 residual symmetry. Both solutions have a round S
6 metric and are supported by
the Romans’ mass and internal F6 flux. While the SO(7) invariant vacuum is known to
be perturbatively unstable, the G2 invariant one has been found to have a fully stable
Kaluza-Klein spectrum. Moreover, it has been shown to be protected against brane-jet
instabilities. Motivated by these results, we study possible bubbling solutions connected
to the G2 vacuum, representing non-perturbative instabilities of the latter. We indeed
find an instability channel represented by the nucleation of a bubble of nothing dressed
up with a homogeneous D2 brane charge distribution in the internal space. Our solu tion generalizes to the case where S
6
is replaced by any six-dimensional nearly-Kähler
manifold
Spherical branes and the BMN matrix quantum mechanics
No full textWe study the maximally supersymmetric Yang-Mills theory on Sd using supersymmetric localisation and holography. We argue that the analytic continuation in dimension to d = 1 yields a Euclidean version of the BMN matrix quantum mechanics. This system can be analysed at large N using supersymmetric localisation and leads to explicit results for the free energy on Sd and the expectation value of supersymmetric Wilson loops. We show how these results can be reproduced at strong gauge coupling using holography by employing spherical D-brane solutions. We construct these solutions for any value of d using an effective supergravity description and pay particular attention to the subtleties arising in the d → 1 limit. Our results have implications for the BMN matrix quantum mechanics and the physics of circular D0-branes
To see or not to see a bow shock. Identifying bow shocks with Ha allsky surveys
No full textOB-stars have the highest luminosities and strongest stellar winds of all stars, which enables them to interact strongly with their surrounding ISM, thus creating bow shocks. These offer us an ideal opportunity to learn more about the ISM. They were first detected and analysed around runaway OB-stars using the IRAS allsky survey by van Buren et al. (1995, AJ, 110, 2614). Using the geometry of such bow shocks information concerning the ISM density and its fluctuations can be gained from such infrared observations. As to help to improve the bow shock models, additional observations at other wavelengths, e.g. H, are most welcome. However due to their low velocity these bow shocks have a size of 1°, and could only be observed as a whole with great difficulties. In the light of the new H allsky surveys (SHASSA/VTSS) this is no problem any more. We developed different methods to detect bow shocks, e.g. the improved determination of their symmetry axis with radial distance profiles. Using two H-allsky surveys (SHASSA/VTSS), we searched for bow shocks and compared the different methods. From our sample we conclude, that the correlation between the direction of both proper motion and the symmetry axis determined with radial distance profile is the most promising detection method. We found eight bow shocks around HD 17505 , HD 24430 , HD 48099 , HD 57061 , HD 92206 , HD 135240 , HD 149757 , and HD 158186 from 37 candidates taken from van Buren et al. (1995, AJ, 110, 2614)
MeSH term explosion and author rank improve expert recommendations
No full textInformation overload is an often-cited phenomenon that reduces the productivity, efficiency and efficacy of scientists. One challenge for scientists is to find appropriate collaborators in their research. The literature describes various solutions to the problem of expertise location, but most current approaches do not appear to be very suitable for expert recommendations in biomedical research. In this study, we present the development and initial evaluation of a vector space model-based algorithm to calculate researcher similarity using four inputs: 1) MeSH terms of publications; 2) MeSH terms and author rank; 3) exploded MeSH terms; and 4) exploded MeSH terms and author rank. We developed and evaluated the algorithm using a data set of 17,525 authors and their 22,542 papers. On average, our algorithms correctly predicted 2.5 of the top 5/10 coauthors of individual scientists. Exploded MeSH and author rank outperformed all other algorithms in accuracy, followed closely by MeSH and author rank. Our results show that the accuracy of MeSH term-based matching can be enhanced with other metadata such as author rank
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
Single Star-Forming Galaxies and Star-Forming Galaxies in SF+SF and Mixed Pairs
No full textWe compare the SFR of single star-forming galaxies with the SFR of star-forming galaxies in pairs. Volume limited samples are compared selected from the 2dFGRS applying a maximum magnitude difference criterion. We show that SF galaxies in SF+SF pairs typically increase teir SFR as they get fainter, whereas this does not happen for SF galaxies in mixed (SF+passive) pairs. And we provide evidence that differences between single SF and SF in pairs get more significant when SF galaxies in mixed pairs are excluded from the pair sample. Our analysis confirms that enhanced SFR and the presence of a companion galaxies (on 0.5 h^-1 Mpc scale) are correlated quantities, provided the galaxy is neither too luminous nor too faint and the triggering galaxy is ikteself a SF galaxy
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