14,361 research outputs found

    Umbilic hypersurfaces of constant sigma-k curvature in the Heisenberg group

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    We study immersed, connected, umbilic hypersurfaces in the Heisenberg group HnH_{n} with nn ≥\geq 2.2. We show that such a hypersurface, if closed, must be rotationally invariant up to a Heisenberg translation. Moreover, we prove that, among others, Pansu spheres are the only such spheres with positive constant sigma-k curvature up to Heisenberg translations.Comment: 28 pages, 6 figure

    Umbilicity and characterization of Pansu spheres in the Heisenberg group

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    For n≥2n\geq 2 we define a notion of umbilicity for hypersurfaces in the Heisenberg group HnH_{n}. We classify umbilic hypersurfaces in some cases, and prove that Pansu spheres are the only umbilic spheres with positive constant pp(or horizontal)-mean curvature in HnH_{n} up to Heisenberg translations.Comment: 32 pages, 2 figures; in Crelle's journal, 201

    A Codazzi-like equation and the singular set for C1C^{1} smooth surfaces in the Heisenberg group

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    In this paper, we study the structure of the singular set for a C1C^{1} smooth surface in the 33-dimensional Heisenberg group H1\boldsymbol{H}_{1}. We discover a Codazzi-like equation for the pp-area element along the characteristic curves on the surface. Information obtained from this ordinary differential equation helps us to analyze the local configuration of the singular set and the characteristic curves. In particular, we can estimate the size and obtain the regularity of the singular set. We understand the global structure of the singular set through a Hopf-type index theorem. We also justify that Codazzi-like equation by proving a fundamental theorem for local surfaces in H1\boldsymbol{H}_{1}.Comment: 64 pages, 17 figure

    Bidirectional outflows as evidence of magnetic reconnection leading to a solar microflare

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    Magnetic reconnection is a rapid energy release process that is believed to be responsible for flares on the Sun and stars. Nevertheless, such flare-related reconnection is mostly detected to occur in the corona, while there have been few studies concerning the reconnection in the chromosphere or photosphere. Here we present both spectroscopic and imaging observations of magnetic reconnection in the chromosphere leading to a microflare. During the flare peak time, chromospheric line profiles show significant blueshifted/redshifted components on the two sides of the flaring site, corresponding to upflows and downflows with velocities of ±\pm(70--80) km s−1^{-1}, comparable with the local Alfv\'{e}n speed as expected by the reconnection in the chromosphere. The three-dimensional nonlinear force-free field configuration further discloses twisted field lines (a flux rope) at a low altitude, cospatial with the dark threads in He I 10830 \r{A} images. The instability of the flux rope may initiate the flare-related reconnection. These observations provide clear evidence of magnetic reconnection in the chromosphere and show the similar mechanisms of a microflare to those of major flares.Comment: 16 pages, 5 figures, accepted for publication in ApJ
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