The individual investigations, which are briefly introduced above, are united in highlightingseveral specific advances in our understanding of the Sun’s atmosphere facilitated by the ad-ĭition of Parker Solar Probe to humanity’s suite of heliospheric instrumentation. The Sun and as other advances in space based instrumentation are made, such as the gradualĮscape of the Solar Orbiter to higher latitudes. We close with a summary of these results and the outlook for further improvement of ourunderstanding of the coupled corona and inner heliosphere ans PSP continues to approach The future prospects of using this localisation to constrain magnetic connectivity and density Potential to act as passive tracers of coronal and heliospheric structure. Further, it allows disambiguation of spatial and temporalįinally, we present recent work using observations by Parker Solar Probe and other 1 auspacecraft to localise type III radio bursts, an impulsive solar ejection of electron beams,įrom emission at the solar surface out into the inner heliosphere. Understanding other peculiar plasma physics observed as PSP as it has explored new re. Modelling and PSP data shows how making these connections is a vital building block for PSP, and therefore contextualises its measurements. Nation of specific locations on the Sun which emit solar wind plasma later measured by Third, we present a study in which we determine Parker Solar Probe’s magnetic connectivityback to specific coronal sources for its first solar encounter. We also compare the meanĭirection of the heliospheric magnetic field to the expectation of the Parker spiral model,įinding very good agreement which is tending to improve with closing distance from the sunĪs the ratio of average field strength to random fluctuations increases. To coronal models with typically accepted model parameters. This conservation implies a deficit in open magnetic flux according ![]() We measure the open magnetic flux and confirm it is conserved between 1 au and PSP’sĬlosest approach to date. Isotropic, indicating the coronal field has already relaxed to this state within this radius. We present evidence that at 0.13 au the heliospheric magnetic field remains latitudinally Next, we use the full data set of the heliospheric magnetic field taken by Parker Solar Probein its first four years on orbit to directly measure the heliospheric magnetic field down toĠ.13 au and compare directly to the large scale expectations of the Parker magnetic field. Specific metrics can lead to different conclusions about optimum model parameters. We illustrate how models must be constrainedĪt multiple boundaries to give an accurate representation and that focusing on individual The topology of the coronal streamer belt. To constrain the sizes of coronal holes and the locations of high plasma density indicating To new PSP data which provides direct boundary conditions on the magnetic skeleton of theĬorona, we show how it is important to make use of pre-existing observational capabilities Specifically, we first introduce a framework for evaluating models of the coronal magneticfield, which sets how the solar wind emerges and shapes the inner heliosphere. Global structure and further derive novel constraints on plasma models of the corona and Of work we use new data from PSP to improve our knowledge and understanding of this Heliosphere which had hitherto could only be accessed with global modelling. This has presented an opportunity to directly probe regions of the Solar Probe (PSP) was launched into an orbit taking it closer to the Sun than any human. ![]() ![]() Our most complete understanding of the corona and heliosphere comes from large scalephysical models which can fill in information about a plasma on a 3D grid. Influence which extends out to 1 au and therefore is most relevant to the Earth and humanity. By inner heliosphere, we focus on the portion of the Sun’s sphere of Where the dynamic pressure of the outflowing solar wind overcomes the magnetic pressure of These two regimesĪre strongly coupled together but their mutual boundary may be regarded as the location Of particular importance to making Sun-EarthĬonnections are the regions called the corona and the inner heliosphere. All interactions between the Sun and life onĮarth are channelled through this medium. Stellar medium which is called the heliosphere. The Sun’s atmosphere is a complex and dynamic magnetized plasma and extends all theway from its visible surface out into interplanetary space, carving out a bubble in the inter.
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