ALFVÉN WAVE SOLAR MODEL (AWSoM): CORONAL HEATING

By B. Holst, Igor M. Sokolov, Xing Meng, M. Jin, IV WardB.Manchester, G. T'oth, Tamas I. Gombosi. 2013

308 citations recorded by the source corpus.

We present a new version of the Alfvén wave solar model, a global model from the upper chromosphere to the corona and the heliosphere. The coronal heating and solar wind acceleration are addressed with low-frequency Alfvén wave turbulence. The injection of Alfvén wave energy at the inner boundary is such that the Poynting flux is proportional to the magnetic field strength. The three-dimensional magnetic field topology is simulated using data from photospheric magnetic field measurements. This model does not impose open-closed magnetic field boundaries; those develop self-consistently. The physics include the following. (1) The model employs three different temperatures, namely the isotropic electron temperature and the parallel and perpendicular ion temperatures. The firehose, mirror, and ion–cyclotron instabilities due to the developing ion temperature anisotropy are accounted for. (2) The Alfvén waves are partially reflected by the Alfvén speed gradient and the vorticity along the field lines. The resulting counter-propagating waves are responsible for the nonlinear turbulent cascade. The balanced turbulence due to uncorrelated waves near the apex of the closed field lines and the resulting elevated temperatures are addressed. (3) To apportion the wave dissipation to the three temperatures, we employ the results of the theories of linear wave damping and nonlinear stochastic heating. (4) We have incorporated the collisional and collisionless electron heat conduction. We compare the simulated multi-wavelength extreme ultraviolet images of CR2107 with the observations from STEREO/EUVI and the Solar Dynamics Observatory/AIA instruments. We demonstrate that the reflection due to strong magnetic fields in the proximity of active regions sufficiently intensifies the dissipation and observable emission.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/141763adb0af7e40f783fa7736a9db6a8db39608

How researchers see this paper

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In Astronomy and Astrophysics

1. M. Temmer
2. W. Manchester IV
3. B. Vršnak
4. N. Lugaz
5. Tibor Török
6. C. Chen
7. C. Schrijver
8. C. Farrugia

In Geophysics

1. M. Temmer
2. C. Schrijver
3. John W. Bonnell
4. B. Vršnak

Citations in the corpus

• The Interaction of Successive Coronal Mass Ejections: A Review (2016, methodology): “With a full 3D MHD code under the Space SOLA: Review_v4.tex; 16 March 2017; 5:40; p. 12 Weather Modeling Framework (Tóth et al., 2012; van der Holst et al., 2014), Jin et al. (2016) numerically studied the long-distance magnetic impacts of CMEs.”
• The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere (2019, background): “The PSP results indicate that turbulencedriven models (e.g., Cranmer et al. 2007; Verdini et al. 2009; Chandran & Hollweg 2009; Chandran et al. 2011; van der Holst et al. 2014) remain a viable explanation for the acceleration of the solar wind from open field regions.”
• The Physical Processes of CME/ICME Evolution (2017, background): “Some models also allow for a separate treatment of the electron and ion temperatures (van der Holst et al. 2014).”
• Origins of the Ambient Solar Wind: Implications for Space Weather (2017, unknown): “Additional recent developments include solving multi-fluid energy equations instead of single-fluid MHD (Usmanov et al. 2012, 2016; van der Holst et al. 2014; Oran et al. 2015) and assimilating time-dependent photospheric data instead of using static synoptic maps (Feng et al. 2015; Linker et al.…”
• THERMAL DIAGNOSTICS WITH THE ATMOSPHERIC IMAGING ASSEMBLY ON BOARD THE SOLAR DYNAMICS OBSERVATORY: A VALIDATED METHOD FOR DIFFERENTIAL EMISSION MEASURE INVERSIONS (2015, methodology): “…in the thermal domain requires either DEM analysis and/or sophisticated MHD modeling with forward synthesis of observables (e.g., Peter et al. 2004; Gudiksen & Nordlund 2005; Mok et al. 2005; Hansteen et al. 2010; Peter & Bingert 2012; Jin et al. 2013; Chen et al. 2014; van der Holst et al. 2014).”
• Slow Solar Wind: Observations and Modeling (2016, unknown): “Most recently, global MHD models have attempted to incorporate self-consistent theories of coronal heating and solar wind acceleration using waves and turbulence (e.g., Lionello et al. 2013; van der Holst et al. 2014).”