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Sun corona hole 20163/5/2023 ![]() Surface Alfvén waves in solar flux tubes. On the nature of kink MHD waves in magnetic flux tubes. Goossens, M., Terradas, J., Andries, J., Arregui, I. The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO). An instrument to measure coronal emission line polarization. Asteroseismology of solar-type and red-giant stars. Estimating the “dark” energy content of the solar corona. Global conditions in the solar corona from 2010 to 2017. Alfvén wave heating of the solar chromosphere: 1.5D models. Overdamped Alfvén waves due to ion-neutral collisions in the solar chromosphere. Radial evolution of power spectra of interplanetary Alfvénic turbulence. Coronal heating by magnetohydrodynamic turbulence driven by reflected low-frequency waves. Magnetoacoustic portals and the basal heating of the solar chromosphere. Alfvén waves in the structured solar corona. Benchmarking fast-to-Alfvén mode conversion in a cold magnetohydrodynamic plasma. Three-dimensional MHD wave propagation and conversion to Alfvén waves near the solar surface. First direct measurements of transverse waves in solar polar plumes using SDO/AIA. Alfvénic waves with sufficient energy to power the quiet solar corona and fast solar wind. ![]() Detection of waves in the solar corona: kink or Alfvén? Astrophys. A global view of velocity fluctuations in the corona below 1.3 R ⊙ with CoMP. Investigating Alfvénic wave propagation in coronal open-field regions. Chromospheric Alfvénic waves strong enough to power the solar wind. Broadening of SI VIII lines observed in the solar polar coronal holes. The solar wind as a turbulence laboratory. Large-amplitude Alfvén waves in the interplanetary medium 2. Heating of the solar chromosphere and corona by Alfvén wave turbulence. On the generation, propagation, and reflection of Alfvén waves from the solar photosphere to the distant heliosphere. Alfvén waves and turbulence in the solar atmosphere and solar wind. 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. Chromospheric and coronal heating mechanisms II. Stellar activity and coronal heating: an overview of recent results. Observations of cool-star magnetic fields. Acknowledging that internal acoustic modes have a key role in injecting additional Poynting flux into the upper atmospheres of Sun-like stars has potentially significant consequences for the modelling of stellar coronae and winds. Alfvénic waves are thus a fundamental feature of the Sun’s corona. Here, we provide evidence that the Sun’s internal acoustic modes also contribute to the basal flux of Alfvénic waves, delivering a spatially ubiquitous input to the coronal energy balance that is sustained over the solar cycle. It is generally assumed that the associated Poynting flux is generated solely in the photosphere and propagates into the corona, typically through the continuous buffeting of magnetic fields by turbulent convective cells 4, 6, 7. ![]() Despite Alfvénic waves having been identified in the Sun’s atmosphere, the nature of the basal wave energy flux is poorly understood. Alfvénic waves are thought to make a critical contribution to energy transfer along these magnetic fields, with the potential to heat plasma and accelerate stellar winds 3, 4, 5. Many cool stars possess complex magnetic fields 1 that are considered to undertake a central role in the structuring and energizing of their atmospheres 2.
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