The solar dynamo

By Mathieu Ossendrijver. 2003

372 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/a73b073f60a4942fbbcb33a6ca65a666fc7a5ec3

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Citations in the corpus

Simulations of the Small-Scale Turbulent Dynamo (2003, background): “…Heiles 1997; Vallée 1997, 1998; Balbus & Hawley 1998; Kulsrud 1999; Weiss & Tobias 2000; Title 2000; Beck 2000, 2001; Ferrière 2001; Kronberg et al. 2001; Carilli & Taylor 2002; Han & Wielebinski 2002; Widrow 2002; Tobias 2002; Ossendrijver 2003; Han et al. 2004; Brandenburg & Subramanian 2004).”
Chromospheric activity catalogue of 4454 cool stars (2018, methodology): “Together with the Ω effect, which is differential rotation, it has been successful in reproducing different aspects of the solar magnetic cycle under the mean-field dynamo models (see e.g. Ossendrijver 2003; Charbonneau 2010, for a detailed review on the solar dynamo).”
Solar Dynamo Theory (2014, background): “…review focuses on a few areas where significant advances have been made in the past two decades in a manner such as to complement, rather than duplicate, other recent reviews on the topic, notably Ossendrijver (2003), Brandenburg & Subramanian (2005), Miesch & Toomre (2009), and Charbonneau (2010).”
PERSISTENT MAGNETIC WREATHS IN A RAPIDLY ROTATING SUN (2010, background): “…stars like the Sun, the global-scale dynamo is generally thought to be seated in the tachocline, an interface of shear between the differentially rotating convection zonea d the radiative interior which is in solid body rotation (e.g., Parker 1993; Charbonneau & MacGregor 1997; Ossendrijver 2003).”
Toroidal versus poloidal magnetic fields in Sun-like stars: a rotation threshold (2008, background): “…progress in this field since the very first solar dynamo model proposed by Parker (1955), there are still many aspects of solar magnetism that the current models cannot reproduce or did not thoroughly explore (see, e.g. the reviews of Ossendrijver 2003 or Brandenburg & Subramanian 2005).”
A VOLUME-LIMITED SAMPLE OF 63 M7–M9.5 DWARFS. II. ACTIVITY, MAGNETISM, AND THE FADE OF THE ROTATION-DOMINATED DYNAMO (2009, background): “At masses lower than 0.3M⊙ (Burrows et al. 1997), ultracool dwarfs are fully convective (Baraffe et al. 1998) and cannot harbor a dynamo that requires a tachocline, as is believed to be the case at least for the cyclic part of the solar dynamo (e.g., Ossendrijver 2003).”
Hemispheric sunspot numbers R~n and R~s from 1945-2004: catalogue and N-S asymmetry analysis for solar cycles 18-23 (2006, background): “…be explained by the interference between the dominant dipolar mode and modes with quadrupolar symmetry with respect to the solar equator (excitation could be reached through nonlinear or stochastic effects) that may strongly enhance the N-S asymmetry between the hemispheres (Ossendrijver 2003).”
CONSTRAINING THE AGE–ACTIVITY RELATION FOR COOL STARS: THE SLOAN DIGITAL SKY SURVEY DATA RELEASE 5 LOW-MASS STAR SPECTROSCOPIC SAMPLE (2007, background): “…MD 21218 7 Department of Physics & Astronomy, Vanderbilt University, Nashville, TN 37235 the tachocline) creates a rotational sheer; the convective zone undergoes differential rotation, while the radiative zone rotates like a solid body (Parker 1993; Ossendrijver 2003; Thompson et al. 2003).”
A CATALOG OF ROTATION AND ACTIVITY IN EARLY-M STARS (2012, background): “Rotational shear at this interface can amplify magnetic fields and sustain a cyclic magnetic dynamo (Parker 1993; Ossendrijver 2003).”
Does the butterfly diagram indicate a solar flux-transport dynamo? (2004, methodology): “…physical transport of magnetic flux is not used in the more ‘traditional’ type of dynamo models, which explain the equatorward drift by a latitudinally propagating dynamo wave and thus do not require a material flow (for a recent comprehensive review of solar dynamo theory, see Ossendrijver, 2003).”
The Case for a Distributed Solar Dynamo Shaped by Near-Surface Shear (2005, background): “…being comparable with the typical eddy scale at the bottom of the convection zone (Galloway & Weiss 1981), as well as the observed fidelity of Hale’s polarity law; see Fisher et al. (2000), Tobias (2002), Schüssler (2002), Ossendrijver (2003), Fan (2004), and Weiss (2005) for recent reviews.”
Asteroseismology of Solar-Type and Red-Giant Stars (2013, background): “…region in the stably stratified layer just beneath the base of the convective envelope which mediates the transition from differential rotation in the envelope to a solid-body-like profile in the radiative interior and is believed to play an integral rôle in dynamo action (Ossendrijver 2003).”
The Origin of T Tauri X-Ray Emission: New Insights from the Chandra Orion Ultradeep Project (2005, background): “The third problem is our lack of a sound understanding of the dynamo processes, which are the ultimate origin of the magnetic activity in the Sun and in stars (e.g., Ossendrijver 2003).”
Fluctuation dynamo and turbulent induction at low magnetic Prandtl numbers (2007, background): “…physical mechanism most likely to be responsible for the ubiquitous presence of dynamically strong magnetic fields in the Universe — from planets and stars to galaxies and galaxy clusters (e.g., Moffatt 1978, Childress & Gilbert 1995, Roberts & Glatzmaier 2000, Ossendrijver 2003, Widrow 2002).”
CYCLIC MAGNETIC ACTIVITY DUE TO TURBULENT CONVECTION IN SPHERICAL WEDGE GEOMETRY (2012, background): “…turbulent effects are parameterized (e.g. Krause & Rädler 1980), have reproduced many aspects of the solar cycle, but with broadly varying assumptions for the various parameterizations (see, e.g. Dikpati & Charbonneau 1999; Ossendrijver 2003; Käpylä et al. 2006; Kitchatinov & Olemskoy 2012).”
Exploring the Physical Basis of Solar Cycle Predictions: Flux Transport Dynamics and Persistence of Memory in Advection- versus Diffusion-dominated Solar Convection Zones (2007, background): “While there is now a concensus that the Sun’s magnetic field is generated by a hydromagnetic dynamo (Ossendrijver 2003; Charbonneau 2005), the origin of fluctuations in the basic cycle is yet to be conclusively determined.”
Dynamo Action in the Solar Convection Zone and Tachocline: Pumping and Organization of Toroidal Fields (2006, background): “…the elements have now begun to be studied singly with reasonable fidelity using three-dimensional numerical modeling, often turning to localized planar domains to obtain sufficient spatial resolution within the simulations (see reviews by Ossendrijver 2003; Fan 2004; Charbonneau 2005; Miesch 2005).”
Simulations of Dynamo Action in Fully Convective Stars (2007, background): “…poloidal poloidal magnetic fields generated within the convection zone, giving rise to organized toroidal field structures (e.g., Parker 1993; Charbonneau & MacGre- 1 present address: Dept of Astronomy & Astrophysics, U. Chicago, 5640 S. Ellis Ave, Chicago, IL 60637 gor 1997; Ossendrijver 2003).”