Description
Organiser: Jesse Coburn; co organisers: Deborah Baker, Luca Franci, Alexander James, Pauline Simon, Stephanie Yardley
The Solar Orbiter and Parker Solar Probe missions have both been operating for several years now providing state-of-the-art in situ measurements of the solar wind and remote sensing observations of its source regions on the Sun. They have ventured closer to the Sun than ever before providing new insights into the mechanisms that heat the corona and accelerate the solar wind. This unprecedented view of the solar corona-wind connection with the aid of advanced magnetic field modelling permits precise identification of the solar wind source regions (such as coronal holes and active region boundaries). In particular, we are able to put observational constraints on theories that invoke magnetic field reconnection and energisation by plasma turbulence and waves to explain coronal heating and solar wind acceleration. In this session, we will celebrate and discuss the latest advances in solar wind and solar corona research. We encourage observations from Solar Orbiter, Parker Solar Probe, Daniel K. Inouye Solar Telescope (DKIST), Advanced Composition Explorer, Swedish 1-m Solar Telescope, Solar Dynamics Observatory, Hinode and other Heliospheric observatories.
Since the middle of the last century, it has been known that the atmosphere of the Sun is orders of magnitudes hotter than its surface. Over the years, many studies have looked at the potential role of MHD waves in sustaining these high temperatures. Using 3D MHD simulations of transverse, Alfvenic waves, we look at the role of the complexity of the magnetic field and the power spectrum of the...
A primary characteristic of solar flares is the efficient acceleration
of electrons to nonthermal deka-keV energies. While hard X-Ray (HXR)
observation of bremsstrahlung emission serves as the key diagnostic of
these electrons. In this study, we investigate the time evolution of
flare-accelerated electrons using the warm-target model. This model,
unlike the commonly used cold-target...
Many space weather forecasting and scientific applications would benefit from improved extrapolation of the solar coronal magnetic field, since this acts as the main โboundary conditionโ for models of the heliospheric magnetic field and solar wind. I will present a practical extension to the PFSS (potential field source surface) model to incorporate an axisymmetric solar wind. A steady state...
Magnetohydrodynamic (MHD) waves are ubiquitous in the solar atmosphere and are key in many models for seismological or energy conversion processes. Coronagraphs such as Metis on board Solar Orbiter have already detected wave-like disturbances and other such instruments on board Aditya-L1 and PROBA-3 are likely to follow observing them at unprecedented spatial and temporal resolutions, opening...
Parker Solar Probe was launched nearly 7 years ago and within a few months became the first spacecraft to study the inner heliosphere twice as close to the Sun than ever before. Each year, PSPโs perihelion has been moving closer to the Sun, last year reaching a distance of less than 10 solar radii, nearly 7 times closer than any other spacecraft. An important milestone was reached in 2021 when...
Switchbacks are large Alfvรฉnic deflections , or even reversals, of the magnetic field in the solar wind. Many authors have suggested that switchbacks are linked to processes low in the solar atmosphere such as interchange reconnection, but the manner of this connection remains unclear. Torsional Alfvรฉn waves are known to be naturally produced by impulsive interchange reconnection events such...
Low-latitude coronal holes can produce fast solar wind characterized by rapid fluctuations rather than a steady flow. Despite significant advances in solar physics, the precise mechanisms behind the formation of this fast solar wind remain elusive. In this study, we analyze multiple sources of such wind. By linking in-situ measurements from the Solar Orbiter's instruments to their potential...
The study of solar turbulence and density fluctuations is essential for understanding the physical processes governing the heliosphere, particularly the behavior of the solar wind and its role in space weather. These turbulent structures can significantly influence the observed propertiesโsuch as angular size and positionโof compact extra-solar radio sources. In this work, we utilize the...
The dissipation and heating of collisionless plasma in the inner heliosphere is a significant unresolved problem in space physics. The helicity barrier theory suggests a possible mechanism for these processes, but it requires validation through analysis of spacecraft data. We assess the validity of the parameter regime associated with the helicity barrier in the solar wind over a range of...
The slow solar wind has long been believed to be driven by interchange reconnection between open and closed flux at pseudo and helmet streamers. While recent work now suggests that the Alfvรฉnic fast wind may also be the result of interchange reconnection occurring at a multitude of small, network bipoles inside coronal holes. Here, we present observations of the post-eruption relaxation phase...
Abstract
Understanding the evolution of the solar wind, including solar large-scale structures such as interplanetary coronal mass ejections, stream interaction regions, and high-speed streams, requires tracking the solar plasma starting from its references and active regions on the solar surface through interplanetary space. Multi-spacecraft can introduce new thoughts about these features'...
Solar radio bursts, produced by electrons travelling along magnetic field lines from the Sun through the heliosphere, are a unique diagnostic of the solar atmosphere. Remote radio observations from spacecraft, including Parker Solar Probe and Solar Orbiter, now offer a multi-vantage point view of radio bursts at different longitudes around the Sun. By analysing variations in the received peak...
The open flux problem relates to the inconsistencies between the in-situ measurements of the magnetic flux at 1 AU and the estimated magnetic flux propagated from near the Sun surface (typically 2-3 solar radii) to 1 AU. The estimate measure of the flux at 1 AU is larger than the flux estimated from solar modelling, which is not compatible with our understanding of the interplanetary magnetic...
