Waves in the Magnetized Solar Atmosphere. II. Waves from Localized Sources in Magnetic Flux Concentrations

By T. Bogdan, M. Hansteen, A. McMurry, C. Rosenthal, M. Johnson, S. Petty-Powell, E. J. Zita, Robert F. Stein, S. McIntosh, Åke Nordlund. 2003

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Citations in the corpus

Oscillations and Waves in Solar Spicules (2009, background): “The Alfvén waves also can be generated near β = 1 region due to various wave coupling processes (Bogdan et al. (2002, 2003); Zaqarashvili and Roberts (2006)).”
Alfvén Waves in the Solar Atmosphere (2012, background): “Such studies will shed ample light into the true nature of Alfvén and other MHD wave dynamics and heating (Bogdan et al. 2003; Carlsson & Bogdan 2006; Erdélyi et al. 2007; Fedun et al. 2009; Khomenko et al. 2008; Fedun et al. 2011a).”
On Solving the Coronal Heating Problem (2005, background): “Mode coupling and other processes transfer energy between the different wave types, so the mix of waves changes as a function of height in the atmosphere (e.g., Stein and Nordlund, 1991; Bogdan et al., 2003).”
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).”
Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, background): “Time-dependent MHD models have the benefit of producing such effects naturally (e.g., Ofman & Davila 1998; Ofman 2005; Bogdan et al. 2002, 2003; Suzuki & Inutsuka 2005, 2006).”
Solar winds driven by nonlinear low‐frequency Alfvén waves from the photosphere: Parametric study for fast/slow winds and disappearance of solar winds (2005, background): “The compressive waves generated from the Alfve´n waves would suffer transit-time damping by interactions between magnetic mirrors and surfing particles [ Barnes, 1966; Suzuki et al., 2006].”
How to Channel Photospheric Oscillations into the Corona (2005, background): “Under such lowb conditions, the high magnetic field provides a strong waveguide to slow MHD waves and shocks (Bogdan et al. 2003), so that our hydrodynamic approach properly describes the leaking p-modes.”
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).”
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).”
Magnetic field inclination and atmospheric oscillations above solar active regions (2006, background): “The significance of attack angle has been noticed in numerical simulations previously (Bogdan et al 2003).”