Role of Longitudinal Waves in Alfvén-wave-driven Solar Wind

Abstract

We revisit the role of longitudinal waves in driving the solar wind. We study how the the $p$-mode-like vertical oscillation on the photosphere affects the properties of solar winds under the framework of Alfvén-wave-driven winds. We perform a series of one-dimensional magnetohydrodynamical numerical simulations from the photosphere to beyond several tens of solar radii. We find that the mass-loss rate drastically increases with the longitudinal wave amplitude at the photosphere up to $\sim 4$ times, in contrast to the classical understanding that the acoustic wave hardly affects the energetics of the solar wind. The addition of the longitudinal fluctuation induces the longitudinal-to-transverse wave mode conversion in the chromosphere, which results in the enhanced Alfvénic Poynting flux in the corona. Consequently, the coronal heating is promoted to give higher coronal density by the chromospheric evaporation, leading to the increased mass-loss rate. This study clearly shows the importance of the longnitudinal oscillation in the photosphere and the mode conversion in the chromosphere in determining the basic properties of the wind from solar-like stars.

22 pages, 14 figures, Resubmitted to ApJ after referee comments

References in corpus (26)

• Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence
• The Evolution and Role of Solar Wind Turbulence in the Inner Heliosphere
• Magnetic Landscape of Sun's Polar Region
• On the generation of solar spicules and Alfvénic waves
• New Observational Constraints on the Winds of M Dwarf Stars
• Three Dimensional MHD Wave Propagation and Conversion to Alfven Waves near the Solar Surface. I. Direct Numerical Solution
• The evolution of the solar wind
• First direct measurements of transverse waves in solar polar plumes using SDO/AIA
• A basal contribution from p-modes to the Alfvénic wave flux in the Sun's corona
• Dynamics of the Solar Magnetic Network. II. Heating the Magnetized Chromosphere
• Three-dimensional simulation of the fast solar wind driven by compressible magnetohydrodynamic turbulence
• Three-dimensional Magnetohydrodynamic Simulation of the Formation of Solar Chromospheric Jets with Twisted Magnetic Field Lines
• Damping of Alfven waves by Turbulence and its Consequences: from Cosmic-Rays Streaming to Launching Winds
• Density Fluctuations in the Solar Wind Based on Type III Radio Bursts Observed by Parker Solar Probe
• Turbulence Transport Modeling and First Orbit Parker Solar Probe (PSP) Observations
• Direct and Inverse Cascades in the Acceleration Region of the Fast Solar Wind
• Alfvén-wave driven magnetic rotator winds from low-mass stars I: rotation dependences of magnetic braking and mass-loss rate
• The parametric instability of Alfvén waves: effects of temperature anisotropy
• Radiating Current Sheets in the Solar Chromosphere
• Corona and XUV emission modelling of the Sun and Sun-like stars
• Full compressible 3D magnetohydrodynamic simulation of solar wind
• Height-dependent velocity structure of photospheric convection in granules and intergranular lanes with Hinode/SOT
• IRIS Mg II Observations and Non-LTE Modeling of Off-limb Spicules in a Solar Polar Coronal Hole
• M-dwarf's Chromosphere, Corona and Wind Connection via the Nonlinear Alfvén Wave
• The small-scale structure of photospheric convection retrieved by a deconvolution technique applied to Hinode/SP data
• Astrophysical Conditions for Planetary Habitability

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