857 research outputs found

    Reorientation in Antiferromagnetic Multilayers: Spin-Flop Transition and Surface Effects

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    Nanoscale superlattices with uniaxial ferromagnetic layers antiferromagnetically coupled through non-magnetic spacers are recently used as components of magnetoresistive and recording devices. In the last years intensive experimental investigations of these artificial antiferromagnets have revealed a large variety of surface induced reorientational effects and other remarkable phenomena unknown in other magnetic materials. In this paper we review and generalize theoretical results, which enable a consistent description of the complex magnetization processes in antiferromagnetic multilayers, and we explain the responsible physical mechanism. The general structure of phase diagrams for magnetic states in these systems is discussed. In particular, our results resolve the long standing problem of a ``surface spin-flop'' in antiferromagnetic layers. This explains the different appearance of field-driven reorientation transitions in systems like Fe/Cr (001) and (211) superlattices, and in [CoPt]/Ru multilayers with strong perpendicular anisotropy.Comment: Companion paper for talk at Second Seeheim Conference on Magnetism, June 27- July 1, 2004; 8 pages included 7 figure

    Linear-Time Algorithms for Computing Maximum-Density Sequence Segments with Bioinformatics Applications

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    We study an abstract optimization problem arising from biomolecular sequence analysis. For a sequence A of pairs (a_i,w_i) for i = 1,..,n and w_i>0, a segment A(i,j) is a consecutive subsequence of A starting with index i and ending with index j. The width of A(i,j) is w(i,j) = sum_{i <= k <= j} w_k, and the density is (sum_{i<= k <= j} a_k)/ w(i,j). The maximum-density segment problem takes A and two values L and U as input and asks for a segment of A with the largest possible density among those of width at least L and at most U. When U is unbounded, we provide a relatively simple, O(n)-time algorithm, improving upon the O(n \log L)-time algorithm by Lin, Jiang and Chao. When both L and U are specified, there are no previous nontrivial results. We solve the problem in O(n) time if w_i=1 for all i, and more generally in O(n+n\log(U-L+1)) time when w_i>=1 for all i.Comment: 23 pages, 13 figures. A significant portion of these results appeared under the title, "Fast Algorithms for Finding Maximum-Density Segments of a Sequence with Applications to Bioinformatics," in Proceedings of the Second Workshop on Algorithms in Bioinformatics (WABI), volume 2452 of Lecture Notes in Computer Science (Springer-Verlag, Berlin), R. Guigo and D. Gusfield editors, 2002, pp. 157--17

    A photoionization model of the compact HII region G29.96-0.02

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    We present a detailed photoionization model of G29.96-0.02 (hereafter G29.96), one of the brightest Galactic Ultra Compact HII (UCHII) regions in the Galaxy. This source has been observed extensively at radio and infrared wavelengths. The most recent data include a complete ISO (SWS and LWS) spectrum, which displays a remarkable richness in atomic fine-structure lines. The number of observables is twice as much as the number available in previous studies. In addition, most atomic species are now observed in two ionization stages. The radio and infrared data on G29.96 are best reproduced using a nebular model with two density components: a diffuse (n_e~680cm-3) extended (~1 pc) component surrounding a compact (~0.1 pc) dense (n_e~57000cm-3) core. The properties of the ionizing star were derived using state-of-the-art stellar atmosphere models. CoStar models yield an effective temperature of \~30^{+2}_{-1} kK whereas more recent non-LTE line blanketed atmospheres with stellar winds indicate somewhat higher values, Teff~32--38 kK. This range in Teff is compatible with all observational constraints, including near-infrared photometry and bolometric luminosity. The range 33-36 kK is also compatible with the spectral type O5-O8 determined by Watson and Hanson (97) when recent downward revisions of the effective temperature scale of O stars are taken into account. The age of the ionizing star of G29.96 is found to be a few 10^6 yr, much older than the expected lifetime of UCHII regions. Accurate gas phase abundances are derived with the most robust results being Ne/S=7.5 and N/O=0.43 (1.3 and 3.5 times the solar values, respectively).Comment: Accepted in Astronomy and Astrophysic

    The effects of loyalty programs on customer satisfaction, trust, and loyalty toward high- and low-end fashion retailers

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    This study examines the differential effects of the benefits customers receive from a loyalty program (LP) on satisfaction with the LP, trust in the LP, and store loyalty for high- and low-end fashion retailers. With survey data from U.S. LP subscribers, the study tests the relationships using multiple regressions and analysis of covariance. The results show that symbolic benefits are more important for high-end fashion store consumers' satisfaction with the LP; conversely, utilitarian benefits increase consumers' satisfaction with the LP more in low-end fashion retailing, whereas hedonic benefits increase consumers' satisfaction with the LP in both types of retailers. All benefits in both types of retailers affect trust in the LP. Finally, satisfaction with and trust in the LP are important drivers of loyalty to the retailer. The findings have important implications on how managers of high- and low-end fashion retailing can effectively design their LP rewards to maximize loyalty
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