Magnetic component

A magnetic component has a core (100) with a cavity (105) and a winding structure (21) accommodated in the cavity (105). The winding structure (21) has a height (27) in a direction transverse to its bottom (126) and top faces (125), and is provided with a number of turns (121) which extend from the bottom (126) to the top face (125). The core (100) has a magnetic gap area (24), which has an extension that is at least 50 % of the height (27) of the winding structure. Therewith, eddy currents are substantially limited

Thin-film magnetic head and method of manufacturing the magnetic head

Thin-film magnetic head having a head face (103) and comprising a magnetoresistive element (109) oriented transversely to the head face and a flux-guiding element (107) of a magnetically permeable material terminating in the head face. A peripheral area (109a) of the magnetoresistive element extending parallel to the head face is present opposite the flux-guiding element for forming a magnetic connection between the magnetoresistive element and the flux-guiding element. The flux-guiding element and the peripheral area of the magnetoresistive element constitute a common magnetic contact face (111), while the magnetically permeable material of the flux-guiding element is electrically insulating

Magneto-optical recording medium

A magneto optical recording medium (2) comprising a substrate (4) and a recording layer (6), the recording layer (6) comprising a bilayer structure consisting of a first layer (8) on which a magnetic second layer (10) is deposited, the second layer (10) demonstrating perpendicular magnetic anisotropy and a saturation remanence of at least 90 %, whereby the magnetic material of the second layer (10) comprises an oxide of iron, and the first layer (8) comprises an oxidic material whose in-plane lattice parameter differs from that of the magnetic material, the growth of the second layer (10) upon the first layer (8) being at least locally epitaxial

U, B and r band luminosity functions of galaxies in the Coma cluster

We present a deep multi-colour CCD mosaic of the Coma cluster (Abell 1656), covering 5.2 deg^2 in the B and r bands, and 1.3 deg^2 in the U band. This large, homogeneous data set provides a valuable low redshift comparison sample for studies of galaxies in distant clusters. In this paper we present our survey, and study the dependence of the galaxy luminosity function (LF) on passband and radial distance from the cluster centre. The U, B and r band LFs of the complete sample cannot be represented by single Schechter functions. For the central area, r<245 h_{100}^{-1} kpc, we find best-fitting Schechter parameters of M^{*}_U=-18.60^{+0.13}_{-0.18} and \alpha_U=-1.32^{+0.018}_{-0.028}, M^{*}_B=-19.79^{+0.18}_{-0.17} and \alpha_B=-1.37^{+0.024}_{-0.016} and M^{*}_r=-20.87^{+0.12}_{-0.17} and \alpha_r=-1.16^{+0.012}_{-0.019}. The LF becomes steeper at larger radial distance from the cluster centre. The effect is most pronounced in the U band. This result is consistent with the presence of a star forming dwarf population at large distance from the cluster centre, which may be in the process of being accreted by the cluster. The shapes of the LFs of the NGC 4839 group support a scenario in which the group has already passed through the centre.Comment: Accepted for publication in MNRA