TY - JOUR A1 - Dineva, Ekaterina Ivanova A1 - Pearson, Jeniveve A1 - Ilyin, Ilya A1 - Verma, Meetu A1 - Diercke, Andrea A1 - Strassmeier, Klaus A1 - Denker, Carsten T1 - Characterization of chromospheric activity based on Sun-as-a-star spectral and disk-resolved activity indices JF - Astronomische Nachrichten = Astronomical notes N2 - The strong chromospheric absorption lines Ca ii H & K are tightly connected to stellar surface magnetic fields. Only for the Sun, spectral activity indices can be related to evolving magnetic features on the solar disk. The Solar Disk-Integrated (SDI) telescope feeds the Potsdam Echelle Polarimetric and Spectroscopic Instrument (PEPSI) of the Large Binocular Telescope (LBT) at Mt. Graham International Observatory, Arizona, U.S.A. We present high-resolution, high-fidelity spectra that were recorded on 184 & 82 days in 2018 & 2019 and derive the Ca ii H & K emission ratio, that is, the S-index. In addition, we compile excess brightness and area indices based on full-disk Ca ii K-line-core filtergrams of the Chromospheric Telescope (ChroTel) at Observatorio del Teide, Tenerife, Spain and full-disk ultraviolet (UV) 1600 angstrom images of the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO). Thus, Sun-as-a-star spectral indices are related to their counterparts derived from resolved images of the solar chromosphere. All indices display signatures of rotational modulation, even during the very low magnetic activity in the minimum of Solar Cycle 24. Bringing together different types of activity indices has the potential to join disparate chromospheric datasets yielding a comprehensive description of chromospheric activity across many solar cycles. KW - astronomical databases KW - miscellaneous KW - methods KW - data analysis KW - activity KW - Sun KW - atmosphere KW - chromosphere KW - techniques KW - spectroscopic Y1 - 2022 U6 - https://doi.org/10.1002/asna.20223996 SN - 0004-6337 SN - 1521-3994 VL - 343 IS - 5 PB - Wiley-VCH CY - Weinheim 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 - Rüdiger, Günther A1 - Küker, Manfred T1 - Angular momentum transport by magnetoconvection and the magnetic modulation of the solar differential rotation JF - Astronomy and astrophysics : an international weekly journal / European Southern Observatory (ESO) N2 - In order to explain the variance of the solar rotation law during the activity minima and maxima, the angular momentum transport by rotating magnetoconvection is simulated in a convective box penetrated by an inclined azimuthal magnetic field. Turbulence-induced kinetic and magnetic stresses and the Lorentz force of the large-scale magnetic background field are the basic transporters of angular momentum. Without rotation, the sign of the magnetic stresses naturally depends on the signs of the field components as positive (negative) B theta B phi transport the angular momentum poleward (equatorward). For fast enough rotation, however, the turbulence-originated Reynolds stresses start to dominate the transport of the angular momentum flux. The simulations show that positive ratios of the two meridional magnetic field components to the azimuthal field reduce the inward radial as well as the equatorward latitudinal transport, which result from hydrodynamic calculations. Only for B theta B phi>0 (generated by solar-type rotation laws with an accelerated equator) does the magnetic-influenced rotation at the solar surface prove to be flatter than the nonmagnetic profile together with the observed slight spin-down of the equator. The latter phenomenon does not appear for antisolar rotation with polar vortex as well as for rotation laws with prevailing radial shear. KW - magnetic fields KW - Sun KW - rotation KW - convection Y1 - 2021 U6 - https://doi.org/10.1051/0004-6361/202039912 SN - 1432-0746 VL - 649 PB - EDP Sciences CY - Les Ulis ER - TY - THES A1 - Sule, Aniket T1 - Formation and stability of the solar tachocline in MHD simulations T1 - Entstehung und Stabilität der solaren Tachokline in MHD Simulationen N2 - The solar tachocline is a thin transition layer between the solar radiative zone rotating uniformly and the solar convection zone, which has a mainly latitudinal differential rotation profile. This layer has a thickness of less than $0.05R_{\sun}$ and is subject to extreme radial as well as latitudinal shears. Helioseismological estimates put this layer at roughly $0.7R_{\sun}$. The tachocline mostly resides in the sub-adiabatic, non-turbulent radiative interior, except for a small overlap with the convection zone on the top. Many proposed dynamo mechanisms involve strong toroidal magnetic fields in this transition region. The exact mechanisms behind the formation of such a thin layer is still disputed. A very plausible mechanism is the one involving a weak, relic poloidal magnetic field trapped inside the radiative zone, which is responsible for expelling differential rotation outwards. This was first proposed by \citet{RK97}. The present work develops this idea with numerical simulations including additional effects like meridional circulation. It is shown that a relic field of 1~Gauss or smaller would be sufficient to explain the observed thickness of the tachocline. The stability of the solar tachocline is addressed as the next part of the problem. It is shown that the tachocline is stable up to a differential rotation of 52\% in the absence of magnetic fields. This is a new finding as compared to the earlier two dimensional models which estimated the solar differential rotation (about 28\%) to be marginally stable or even unstable. The changed stability limit is attributed to the changed stability criterion of the 3-dimensional model which also involves radial gradients of the angular velocity. In the presence of toroidal magnetic field belts, the lowest non-axisymmetric mode is shown to be the most unstable one for the radiative part of the tachocline. It is estimated that the tachocline would become unstable for toroidal fields exceeding about 100~Gauss. With both formation and stability questions satisfactorily addressed, this work presents the most comprehensive analysis of the physical processes in the solar tachocline to date. N2 - Die Sonne besteht aus verschiedenen Zonen, die durch die Art des Energietransports von innen nach aussen unterschieden werden. Der innere Teil heißt Strahlungs-, der äußere Teil Konvektionszone. Die Grenzschicht zwischen den beiden Regionen liegt bei etwa 70% des Sonnenradius. Beide Zonen rotieren in ausgezeichneter Weise um die Sonnenachse. In der konvektiven Zone ändert sich die Rotationsrate mit dem Breitengrad und ist nur schwach von der radialen Position abhängig. Dies wird als latitudinale differentielle Rotation bezeichnet. Im Gegensatz dazu rotiert ein Großteil der Strahlungszone gleichförmig. Der Übergang von gleichförmiger Rotation im Inneren zu differentieller Rotation außen geschieht innerhalb einer sehr dünnen Schicht, die ungefähr mit der Grenzschicht zwischen den beiden Zonen übereinstimmt. Diese Schicht hat eine Ausdehnung von etwa 5% des Sonnenradius und wird als “Tachokline” bezeichnet. Die Existenz der Tachokline wurde vor etwa zwei Jahrzehnten bestätigt. Seit ihrer Entdeckung wurden verschiedenste Modelle vorgeschlagen, um die Existenz einer solchen Schicht zu erklären. Diese Arbeit wendet das bislang beliebteste und erfolgreichste dieser Modelle an, das zuerst von Rüdiger & Kitchatinov (1997) vorgeschlagen wurde. Darin wird angenommen, dass während ihrer Entstehung ein schwaches Magnetfeld im Inneren der Sonne eingeschlossen wurde. Ein solches Feld verdrängt die differentielle Rotation erfolgreich in den äußeren Randbereich der Strahlungszone und erzeugt so die Tachokline. Die Theorie nimmt weiter an, dass die Tachokline aktiv mit der darunterliegenden strahlungsdominierten Zone verbunden ist, gemäß der Beobachtung, dass ein Großteil der Tachokline unterhalb des Fußes der Konvektionszone liegt. Diese Arbeit legt verbesserte numerische Simulationen vor, die dem früheren Modell zwei neue physikalische Effekte hinzufügt: schwache radiale und horizontale Strömungen (“meridionale Strömungen” genannt) und Temperaturgradienten. Es wird gezeigt, dass ein eingeschlossenes Feld von weniger als einem Gauß ausreichend wäre, die beobachtete Dicke der Tachokline zu erkären. In einem weiteren Schritt wird versucht zu ergründen, ob die Tachokline eine stabile Schicht innerhalb der Sonne ist. Es wird gezeigt, dass sie, in Abwesenheit eines Magnetfeldes, stabil bleibt, solange die Winkelgeschwindigkeit am Pol nicht unter 52% derer am Äquator fällt. Da sekundäre Strömungen hauptsächlich horizontal verlaufen, haben Temperaturgradienten wenig Einfluss auf die Stabilität der Tachokline. In Gegenwart eines Magnetfeldes wird die Grenzschicht für Felder stärker als 100 Gauß instabil. Indem sowohl Fragen zur Entstehung als auch zur Stabilität zufriedenstellend angesprochen werden, stellt diese Arbeit die derzeit umfassendste Analyse der physikalischen Vorgänge in der Tachokline dar. KW - Sonne KW - Tachokline KW - Magnetohydrodynamik KW - Sun KW - Tachocline KW - Magnetohydrodynamics Y1 - 2007 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-14612 ER -