Making the Corona and the Fast Solar Wind: A Self-consistent Simulation for the Low-Frequency Alfvén Waves from the Photosphere to 0.3 AU

By T. Suzuki, S. Inutsuka. 2005

244 citations recorded by the source corpus.

By performing a one-dimensional magnetohydrodynamic simulation with radiative cooling and thermal conduction, we show that the coronal heating and the fast solar wind acceleration in the coronal holes are natural consequences of the footpoint fluctuations of the magnetic fields at the photosphere. We initially set up a static open flux tube with a temperature of 104 K rooted at the photosphere. We impose transverse photospheric motions corresponding to the granulations with a velocity ⟨dv⊥⟩ = 0.7 km s-1 and a period between 20 s and 30 minutes, which generate outgoing Alfvén waves. We self-consistently treat these waves and the plasma heating. After attenuation in the chromosphere by ≃85% of the initial energy flux, the outgoing Alfvén waves enter the corona and contribute to the heating and acceleration of the plasma mainly by the nonlinear generation of the compressive waves and shocks. Our result clearly shows that the initially cool and static atmosphere is naturally heated up to 106 K and accelerated to ≃800 km s-1.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/15b417b029b70698772bfb91124e40c8f5517715

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Citations in the corpus

Ultraviolet spectroscopy of the extended solar corona (2006, methodology): “…focus on the self-consistent computation of fast solar wind models using a simpler Kolmogorov version of the turbulent damping (e.g., Hu et al. 1999; Li 2003), and on the ability of various kinds of waves to steepen into shocks and heat open-field regions (Suzuki 2004; Suzuki & Inutsuka 2005).”
TIME–DISTANCE SEISMOLOGY OF THE SOLAR CORONA WITH CoMP (2009, background): “…large non-thermal line widths in the corona and exploit the developing self-consistent theories which involve the effective dissipation of low-frequency Alfvénic motions (e.g., Cranmer & van Ballegooijen 2005; Suzuki & Inutsuka 2005; Cranmer, van Ballegooijen & Edgar 2007; Verdini & Velli 2007).”
Alfvén Waves and Turbulence in the Solar Atmosphere and Solar Wind (2007, background): “Among the first are phenomena such as parametric decay (Pruneti & Velli 1997; Del Zanna et al. 2001) and wave steepening (Suzuki & Inutsuka 2005).”
MAGNETOHYDRODYNAMIC WAVES AND CORONAL HEATING: UNIFYING EMPIRICAL AND MHD TURBULENCE MODELS (2012, background): “The same criticism seems to be applicable to the more refined and physics-based Alfvén-wave-driven models of the solar wind Suzuki and Inutsuka (2005); Verdini et al. (2010); Osman et al. (2011).”
A TURBULENCE-DRIVEN MODEL FOR HEATING AND ACCELERATION OF THE FAST WIND IN CORONAL HOLES (2009, methodology): “In these ways, the present model differs from other recent models that incorporate turbulent heating (Suzuki & Inutsuka 2005; Cranmer et al. 2007).”
Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, methodology): “…that containboth a first-principles approach to coronal heating and a self-consistent chromosphere, transition region, and mass flux are those of Suzuki & Inutsuka (2005, 2006).1 The study of MHD turbulence as a potential source of heating for the solar wind goes back to Coleman (1968) and…”
PROPAGATING WAVES ALONG SPICULES (2011, background): “Many theoretical models have been developed for coronal heating based on waves that are excited in the photosphere or chromosphere (e.g., Hollweg et al. 1982; Tu & Marsch 1997; Axford et al. 1999; Suzuki & Inutsuka 2005; Cranmer et al. 2007; Antolin & Shibata 2010).”
Giant Chromospheric Anemone Jet Observed with Hinode and Comparison with Magnetohydrodynamic Simulations: Evidence of Propagating Alfvén Waves and Magnetic Reconnection (2008, background): “These Alfvén waves are generated by reconnection (Yokoyama 1998; Takeuchi & Shibata 2001), and may contribute to the heating and acceleration of solar wind when the magnetic field is open (Parker 1988; Suzuki & Inutsuka 2005).”
Multiwavelength Studies of MHD Waves in the Solar Chromosphere (2015, background): “…in the photosphere up into the upper chromosphere and corona, playing the role as the dominant energy carrier in many simulations that appear to be able to generate hot coronae (e.g., Cranmer and van Ballegooijen 2005; Suzuki and Inutsuka 2005; Verdini and Velli 2007; Matsumoto and Shibata 2010).”
A Semiempirical Magnetohydrodynamical Model of the Solar Wind (2007, background): “In order to obtain the correct solar wind solution, it is necessary to choose an appropriate inner boundary condition for the density (Hammer 1982; Suzuki & Inutsuka 2005).”
Alfvén Waves in the Solar Atmosphere (2012, background): “…Ofman & Davila 1995; Erdélyi and Goossens 1995; Ruderman and Roberts 2002; Goossens et al. 2011), phase mixing (Heyvaerts & Priest 1983; Ofman & Aschwanden 2002), Alfvén turbulence (Cranmer & van Ballegooigen 2005; van Ballegooijen et al. 2011) and/or mode conversion (Suzuki & Inutsuka 2005).”
INCORPORATING KINETIC PHYSICS INTO A TWO-FLUID SOLAR-WIND MODEL WITH TEMPERATURE ANISOTROPY AND LOW-FREQUENCY ALFVÉN-WAVE TURBULENCE (2011, background): “…Alfvén wave (AW), in part for simplicity and in part because the AW is the most promising wave type for transporting energy over large distances into the corona and solar wind (Barnes 1966; Velli et al. 1989; Matthaeus et al. 1999; Suzuki & Inutsuka 2005; Cranmer & van Ballegooijen 2005).”