Waves in the Magnetized Solar Atmosphere. I. Basic Processes and Internetwork Oscillations

By C. Rosenthal, T. Bogdan, M. Carlsson, S. Dorch, V. Hansteen, S. McIntosh, A. McMurry, Å. Nordlund, Robert F. Stein. 2002

149 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/4f2545fe6798177a26c21a1de5479431fa883d6d

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

On the Generation, Propagation, and Reflection of Alfvén Waves from the Solar Photosphere to the Distant Heliosphere (2004, background): “Compressible MHD waves and shocks must also be considered alongside the incompressible waves modeled in this paper (for recent work, see Rosenthal et al. 2002; Bogdan et al. 2002, 2003; Hasan et al. 2003; Hasan & Ulmschneider 2004; Wedemeyer et al. 2004; Bloomfield et al. 2004; Suzuki 2004).”
Waves in the Magnetized Solar Atmosphere. II. Waves from Localized Sources in Magnetic Flux Concentrations (2003, background): “In the previous contribution (Rosenthal et al. 2002, hereafter Paper I) we outlined the basic equilibrium configurations and the underlying governing equations that form the basis for this series.”
Solar winds driven by nonlinear low‐frequency Alfvén waves from the photosphere: Parametric study for fast/slow winds and disappearance of solar winds (2005, methodology): “This is directly testable by in situ measurements of future missions, Solar Orbiter and Solar Pr obe, which will approach to∼45 and 4R⊙, respectively, corresponding to the inside of our computation domain. Our simulations show that the different types of the solar wi nds can be explained by the sing”
Dynamic Hydrogen Ionization (2002, background): “…waves propagate into the the region where the magnetic pressure equals the gas pressure (β = 1) and the magnetic field lines are curved, there is significant reflection and mode conversion into magneto-hydrodynamic waves propagating at approximately the Alfven speed (Rosenthal et al. 2002).”
Numerical Modeling of Magnetohydrodynamic Wave Propagation and Refraction in Sunspots (2006, background): “At the vicinity of this layer, the different wave modes can interact, and mode transformation takes place (see, e.g., Zhugzhda &Dzhalilov 1982, 1984; Bogdan et al. 2002, 2003; Rosenthal et al. 2002; Cally 2005, 2006).”
Solar Fine-Scale Structures. I. Spicules and Other Small-Scale, Jet-Like Events at the Chromospheric Level: Observations and Physical Parameters (2012, background): “…that propagate from the photosphere into the chromosphere, undergo mode conversion, refraction and reflection when they reach the canopy (see e.g. Rosenthal et al., 2002; Bogdan et al., 2003; Schunker and Cally, 2006; Cally, 2007; Khomenko et al., 2008b; Kuridze et al., 2009; Nutto et al., 2012).”