TY - JOUR A1 - Hassanin, Alshaimaa A1 - Kliem, Bernhard A1 - Seehafer, Norbert T1 - Helical kink instability in the confined solar eruption on 2002 May 27 JF - Astronomische Nachrichten = Astronomical notes KW - instabilities KW - magnetohydrodynamics (MHD) KW - Sun: corona KW - Sun: coronal mass ejections (CMEs) KW - Sun: flares Y1 - 2016 U6 - https://doi.org/10.1002/asna.201612446 SN - 0004-6337 SN - 1521-3994 VL - 337 SP - 1082 EP - 1089 PB - Wiley-VCH CY - Weinheim ER - TY - JOUR A1 - Seehafer, Norbert A1 - Fuhrmann, M. A1 - Valori, Gherardo A1 - Kliem, Bernhard T1 - Force-free magnetic fields in the solar atmosphere Y1 - 2007 UR - http://www3.interscience.wiley.com/cgi-bin/abstract/117872628/ABSTRACT ER - TY - JOUR A1 - Kliem, Bernhard A1 - Seehafer, Norbert T1 - Helicity shedding by flux rope ejection JF - Astronomy and astrophysics : an international weekly journal N2 - We quantitatively address the conjecture that magnetic helicity must be shed from the Sun by eruptions launching coronal mass ejections in order to limit its accumulation in each hemisphere. By varying the ratio of guide and strapping field and the flux rope twist in a parametric simulation study of flux rope ejection from approximately marginally stable force-free equilibria, different ratios of self- and mutual helicity are set and the onset of the torus or helical kink instability is obtained. The helicity shed is found to vary over a broad range from a minor to a major part of the initial helicity, with self helicity being largely or completely shed and mutual helicity, which makes up the larger part of the initial helicity, being shed only partly. Torus-unstable configurations with subcritical twist and without a guide field shed up to about two-thirds of the initial helicity, while a highly twisted, kink-unstable configuration sheds only about one-quarter. The parametric study also yields stable force-free flux rope equilibria up to a total flux-normalized helicity of 0.25, with a ratio of self- to total helicity of 0.32 and a ratio of flux rope to external poloidal flux of 0.94. These results numerically demonstrate the conjecture of helicity shedding by coronal mass ejections and provide a first account of its parametric dependence. Both self- and mutual helicity are shed significantly; this reduces the total initial helicity by a fraction of ∼0.4--0.65 for typical source region parameters. KW - instabilities KW - magnetic fields KW - magnetohydrodynamics (MHD) KW - Sun KW - corona KW - coronal mass ejections (CMEs) KW - flares Y1 - 2022 U6 - https://doi.org/10.1051/0004-6361/202142422 SN - 0004-6361 SN - 1432-0746 VL - 659 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Schumacher, Jörg A1 - Kliem, Bernhard A1 - Seehafer, Norbert T1 - Three-dimensional spontaneous magnetic reconnection in neutral current sheets Y1 - 2000 ER - TY - BOOK A1 - Schumacher, Jörg A1 - Kliem, Bernhard A1 - Seehafer, Norbert T1 - Three-dimensional spontaneous magnetic reconnection in neutral current sheets T3 - Preprint series / Astrophysikalisches Institut Potsdam Y1 - 1999 VL - 99,42 PB - AIP CY - Potsdam ER - TY - JOUR A1 - Kliem, Bernhard A1 - Rust, S. A1 - Seehafer, Norbert T1 - Helicity transport in a simulated coronal mass ejection JF - Proceedings of the International Astronomical Union Y1 - 2010 U6 - https://doi.org/10.1017/S1743921311006715 SN - 1743-9213 SN - 1743-9221 SP - 125 EP - 128 PB - International Astronomical Union CY - Cambridge ER - TY - GEN A1 - Kliem, Bernhard A1 - Rust, S. A1 - Seehafer, Norbert T1 - Helicity transport in a simulated coronal mass ejection T2 - Postprints der Universität Potsdam : Mathematisch Naturwissenschaftliche Reihe N2 - It has been suggested that coronal mass ejections (CMEs) remove the magnetic he-licity of their coronal source region from the Sun. Such removal is often regarded to be necessary due to the hemispheric sign preference of the helicity, which inhibits a simple annihilation by reconnection between volumes of opposite chirality. Here we monitor the relative magnetic he-licity contained in the coronal volume of a simulated flux rope CME, as well as the upward flux of relative helicity through horizontal planes in the simulation box. The unstable and erupting flux rope carries away only a minor part of the initial relative helicity; the major part remains in the volume. This is a consequence of the requirement that the current through an expanding loop must decrease if the magnetic energy of the configuration is to decrease as the loop rises, to provide the kinetic energy of the CME. T3 - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 569 KW - magnetic fields KW - MHD KW - coronal mass ejections KW - magnetohydrodynamics KW - sun Y1 - 2019 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-412907 SN - 1866-8372 IS - 569 SP - 125 EP - 128 ER - TY - JOUR A1 - Hassanin, Alshaimaa A1 - Kliem, Bernhard A1 - Seehafer, Norbert A1 - Török, Tibor T1 - A model of homologous confined and ejective eruptions involving kink instability and flux cancellation JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - In this study, we model a sequence of a confined and a full eruption, employing the relaxed end state of the confined eruption of a kink-unstable flux rope as the initial condition for the ejective one. The full eruption, a model of a coronal mass ejection, develops as a result of converging motions imposed at the photospheric boundary, which drive flux cancellation. In this process, parts of the positive and negative external flux converge toward the polarity inversion line, reconnect, and cancel each other. Flux of the same amount as the canceled flux transfers to a flux rope, increasing the free magnetic energy of the coronal field. With sustained flux cancellation and the associated progressive weakening of the magnetic tension of the overlying flux, we find that a flux reduction of approximate to 11% initiates the torus instability of the flux rope, which leads to a full eruption. These results demonstrate that a homologous full eruption, following a confined one, can be driven by flux cancellation. Y1 - 2022 U6 - https://doi.org/10.3847/2041-8213/ac64a9 SN - 2041-8205 SN - 2041-8213 VL - 929 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER -