TY - JOUR A1 - Teriaca, Luca A1 - Andretta, Vincenzo A1 - Auchere, Frederic A1 - Brown, Charles M. A1 - Buchlin, Eric A1 - Cauzzi, Gianna A1 - Culhane, J. Len A1 - Curdt, Werner A1 - Davila, Joseph M. A1 - Del Zanna, Giulio A1 - Doschek, George A. A1 - Fineschi, Silvano A1 - Fludra, Andrzej A1 - Gallagher, Peter T. A1 - Green, Lucie A1 - Harra, Louise K. A1 - Imada, Shinsuke A1 - Innes, Davina A1 - Kliem, Bernhard A1 - Korendyke, Clarence A1 - Mariska, John T. A1 - Martinez-Pillet, Valentin A1 - Parenti, Susanna A1 - Patsourakos, Spiros A1 - Peter, Hardi A1 - Poletto, Luca A1 - Rutten, Robert J. A1 - Schuehle, Udo A1 - Siemer, Martin A1 - Shimizu, Toshifumi A1 - Socas-Navarro, Hector A1 - Solanki, Sami K. A1 - Spadaro, Daniele A1 - Trujillo-Bueno, Javier A1 - Tsuneta, Saku A1 - Dominguez, Santiago Vargas A1 - Vial, Jean-Claude A1 - Walsh, Robert A1 - Warren, Harry P. A1 - Wiegelmann, Thomas A1 - Winter, Berend A1 - Young, Peter T1 - LEMUR large european module for solar ultraviolet research JF - Experimental astronomy : an international journal on astronomical instrumentation and data analysis N2 - The solar outer atmosphere is an extremely dynamic environment characterized by the continuous interplay between the plasma and the magnetic field that generates and permeates it. Such interactions play a fundamental role in hugely diverse astrophysical systems, but occur at scales that cannot be studied outside the solar system. Understanding this complex system requires concerted, simultaneous solar observations from the visible to the vacuum ultraviolet (VUV) and soft X-rays, at high spatial resolution (between 0.1'' and 0.3''), at high temporal resolution (on the order of 10 s, i.e., the time scale of chromospheric dynamics), with a wide temperature coverage (0.01 MK to 20 MK, from the chromosphere to the flaring corona), and the capability of measuring magnetic fields through spectropolarimetry at visible and near-infrared wavelengths. Simultaneous spectroscopic measurements sampling the entire temperature range are particularly important. These requirements are fulfilled by the Japanese Solar-C mission (Plan B), composed of a spacecraft in a geosynchronous orbit with a payload providing a significant improvement of imaging and spectropolarimetric capabilities in the UV, visible, and near-infrared with respect to what is available today and foreseen in the near future. The Large European Module for solar Ultraviolet Research (LEMUR), described in this paper, is a large VUV telescope feeding a scientific payload of high-resolution imaging spectrographs and cameras. LEMUR consists of two major components: a VUV solar telescope with a 30 cm diameter mirror and a focal length of 3.6 m, and a focal-plane package composed of VUV spectrometers covering six carefully chosen wavelength ranges between 170 and 1270 . The LEMUR slit covers 280'' on the Sun with 0.14'' per pixel sampling. In addition, LEMUR is capable of measuring mass flows velocities (line shifts) down to 2 km s (-aEuro parts per thousand 1) or better. LEMUR has been proposed to ESA as the European contribution to the Solar C mission. KW - Sun: atmosphere KW - Space vehicles: instruments KW - Techniques: spectroscopy KW - ESA cosmic vision Y1 - 2012 U6 - https://doi.org/10.1007/s10686-011-9274-x SN - 0922-6435 VL - 34 IS - 2 SP - 273 EP - 309 PB - Springer CY - Dordrecht ER - TY - JOUR A1 - Fuhrmann, Marcel A1 - Seehafer, Norbert A1 - Valori, Gherardo A1 - Wiegelmann, T. T1 - A comparison of preprocessing methods for solar force-free magnetic field extrapolation JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Extrapolations of solar photospheric vector magnetograms into three-dimensional magnetic fields in the chromosphere and corona are usually done under the assumption that the fields are force-free. This condition is violated in the photosphere itself and a thin layer in the lower atmosphere above. The field calculations can be improved by preprocessing the photospheric magnetograms. The intention here is to remove a non-force-free component from the data. Aims. We compare two preprocessing methods presently in use, namely the methods of Wiegelmann et al. (2006, Sol. Phys., 233, 215) and Fuhrmann et al. (2007, A&A, 476, 349). Methods. The two preprocessing methods were applied to a vector magnetogram of the recently observed active region NOAA AR 10 953. We examine the changes in the magnetogram effected by the two preprocessing algorithms. Furthermore, the original magnetogram and the two preprocessed magnetograms were each used as input data for nonlinear force-free field extrapolations by means of two different methods, and we analyze the resulting fields. Results. Both preprocessing methods managed to significantly decrease the magnetic forces and magnetic torques that act through the magnetogram area and that can cause incompatibilities with the assumption of force-freeness in the solution domain. The force and torque decrease is stronger for the Fuhrmann et al. method. Both methods also reduced the amount of small-scale irregularities in the observed photospheric field, which can sharply worsen the quality of the solutions. For the chosen parameter set, the Wiegelmann et al. method led to greater changes in strong-field areas, leaving weak-field areas mostly unchanged, and thus providing an approximation of the magnetic field vector in the chromosphere, while the Fuhrmann et al. method weakly changed the whole magnetogram, thereby better preserving patterns present in the original magnetogram. Both preprocessing methods raised the magnetic energy content of the extrapolated fields to values above the minimum energy, corresponding to the potential field. Also, the fields calculated from the preprocessed magnetograms fulfill the solenoidal condition better than those calculated without preprocessing. KW - Sun: magnetic topology KW - Sun: atmosphere KW - magnetohydrodynamics (MHD) Y1 - 2011 U6 - https://doi.org/10.1051/0004-6361/201015453 SN - 0004-6361 VL - 526 PB - EDP Sciences CY - Les Ulis ER -