Revealing the Pattern of Solar Alfvénic Waves (RiPSAW)

This research proposal aims to advance our understanding of the physics of our closest star, the Sun, and other solar-like stars. The Sun displays a number of fascinating and dynamic phenomena such as powerful solar flares and giant, planet-sized concentrations of magnetic fields (sunspots). It also provides a unique opportunity to examine in detail how other stars behave.

The Sun is made of a plasma (ionised gas) threaded by a strong magnetic field. Such magnetised plasmas are common throughout the universe (e.g. active galaxy nuclei, nebula, interstellar medium), hence the research will also aid advances across multiple research communities.

Many stars possess their own weather systems, although these systems are extreme compared to those we experience on Earth. In our solar system, a hot, million degree wind blows off the Sun at colossal speeds reaching millions of miles per hour, washing over the planets. While we are under the protection of the Earth's magnetic field, that deflects the Sun's wind, other planetary bodies in the solar system have been exposed to its influence.

For example, the Sun's wind is known to have stripped Mars of its atmosphere. Scientists are also interested in how these winds will influence the habitability of exoplanets around other Sun-like stars. These winds also contribute to how the stars evolve, with the Sun losing over 10 trillion tonnes of material each year via its winds.

The objectives of the RiPSAW project are to examine the generation of the hot plasma and powerful winds, focusing on the role of magnetic waves. These magnetic (or Alfvén) waves can transfer energy through a star's atmosphere and are considered an important feature of any magnetic star. During the initial phase of RiPSAW, Dr Morton and his research team pioneered techniques for estimating properties of the magnetic waves.

The renewal of the RiPSAW project will see these tools advanced to examine if there is evidence for wave turbulence in the Sun's corona. Turbulence is one possible mechanism for explaining the heating and acceleration of the winds. Hence the proposed work may transform our understanding of how these hot winds behave.

To address the fundamental challenges, RiPSAW makes use of advanced mathematical techniques and cutting-edge computer simulations to create models of the Sun based on magnetohydrodynamics. We combine this theoretical effort with the highest quality data of the Sun available from state-of-the-art solar instruments (e.g. National Solar Observatory's DKIST - the world's newest and largest solar telescope); incorporating information from across the electromagnetic spectrum (e.g. infrared, EUV) and analysing this with modern methods drawn from statistics and machine learning.