The solar corona is comprised of a hot, ≥1 MK plasma that expands outward into the solar system, carrying magnetic field with it, and reaching flow speeds greater than the Alfvén speed. This flow is the solar wind, and defines the heliosphere. The solar wind is not laminar, but is dynamic and filled with structures on many spatial and temporal scales, from the large down through kinetic dissipation scales. The largest scales are directly imposed onto or injected into the solar wind, and include the timescale of solar rotation, the spatial scales associated with the global coronal magnetic field, and phenomena such as coronal mass ejections (CMEs). At the other end of the size spectrum are the smallest scales, those where electron- and ion-scale kinetic physics and dissipation occur, which are all formed through evolution en route. There is a many-orders-of magnitude spread in scale sizes between the large-scale structure and the kinetic dissipation scales of the solar wind (Verscharen et al., 2019). Neither observations nor simulations are currently capable of spanning the mesoscales. We define mesoscales to include this multiple-decade size range that is larger than the dissipation scale and similar plasma scales, and smaller than the largest-scale structures. Unlike the large scale structures, which are always imposed/injected, and the small scale structures, which evolve en route, mesoscale structures can be created through either mechanism. At 1 AU, mesoscales occur between approximately 5–10,000 Mm, or 10 s to 7 h under the assumption that the structures are strictly advecting. For in situ measurements, which measure the solar wind at a single point, the spatial scale is related to the measured temporal scale by L = V _sw ∗ duration, while in images both spatial and temporal scales can be directly measured.

In Figure 1 we show a conceptual view of the full range of scales in the solar wind, and highlight representative examples of solar wind phenomena observed at the different scales. The y-axis shows the range of scale sizes from large-scale to kinetic. From left to right, we provide representative cartoon examples of each scale, example spectral slopes of the measured plasma variations, the corresponding turbulence regime, whether the scales’ creation is dominated by injected/imposed versus evolution, the ability of current observations to measure them, and the ability of current simulations to model them.

At the smallest scale lies the kinetic scale, where plasma dynamics and structure are dictated by the motion of individual particles. The transition between the kinetic and the mesoscale is generally considered to be related to the ion inertial length, d _i , or the ion gyroradius. At 1 AU, the observed break in the spectra of magnetic field fluctuations from the inertial range to the dissipation scales typically is observed to occur at advected time scales of several seconds (Leamon et al., 1999), or equivalently on spatial scales on the order of hundreds of km through a few Mm via the Taylor hypothesis (that spatial crossing time dominates temporal behavior of the solar wind as measured in situ). This scale is close to the proton cyclotron frequency (Verscharen et al., 2019) though multiple mechanisms have been suggested to explain this spectral break (Leamon et al., 1999). Note also that the Taylor hypothesis has limitations in the context of turbulence (Treumann et al., 2019; Bourouaine and Perez, 2020; Perez et al., 2021). At these small scales, all of the structure and dynamics are created as a result of processing and evolution en route to 1 AU. Any injected or imposed structure from the corona begins to evolve on timescales as rapid as the wave-particle interaction time scale (Bruno and Carbone, 2013); structural evolution on small scales has been observed both in-situ (Elliott et al., 2016) and (on larger scales) remotely (DeForest et al., 2015).

The largest scale solar wind structures are all imposed/injected from the Sun. For example, the traditional solar wind separation by speed into “fast” and “slow” wind (Neugebauer and Snyder, 1962; Neugebauer and Snyder, 1966; McComas et al., 1998), are empirically associated with and imposed by the large scale solar structures coronal holes and coronal streamers, respectively. Co-rotating interaction regions (CIR) and stream interaction regions (SIR) form due to adjacent faster and slower wind regions in combination with solar rotation, producing compression regions where the fast wind catches up with the slow, and rarefaction regions behind (Gosling and Pizzo, 1999). This is an example of directly imposed structures that have been observed in white light and tracked to 1 AU using combined STEREO SECCHI Heliospheric imager data and L1 in situ observations (Rouillard et al., 2009; Rouillard et al., 2010a; Rouillard et al., 2010b), and evidence of them survives out to 10 AU (Richardson, 2018).

The transition from the large scale to the mesoscale range is more ambiguous than the transition from small scale to mesoscales. For the purposes of this paper, we define the mesoscales to be the scales at 1 AU at which structures can be both imposed/injected from the Sun as well as generated en route. The upper end is roughly 10,000 Mm (or 7 h), based on observational and theoretical evidence for mesoscale structures that were created in both ways. These sources of mesoscale structure are not mutually exclusive, as structures from the solar atmosphere will also evolve as they advect. Thus, the complexity in this mesoscale regime is a result of the presence of both imposed/injected and evolved structures, and the interplay between them. Determining the fractional amount of mesoscale structures formed through imposed/injected versus evolved is important for understanding both solar wind formation and turbulent evolution, and the answer is likely dependent on solar wind type and radial distance (evolution time) from the Sun.

Mesoscale solar wind structures are important to study for at least three reasons. First, like the solar wind, the Sun is also dynamic and filled with structures of many scales. Many of the spatial structures are imposed directly onto the heliosphere, and many of the transient dynamics are injected directly into the solar wind as it is formed. Thus, the solar wind and its structures contain imprints of the physical processes that heat the corona and that release and accelerate the solar wind (Viall and Borovsky, 2020). In particular, the traditional bimodal solar wind classification by speed overly simplifies the inherent nature and mesoscale structure of the solar wind. Furthermore, the bimodal classification does not account for solar wind observed to be of other “types” with distinct properties (Roberts et al., 2020a), e.g., slow wind that is highly Alfvénic (Roberts et al., 1987; D’Amicis and Bruno, 2015). Rather than only two types of solar wind, solar wind formation can occur via many different pathways, or combinations of physical mechanisms and source locations (Viall and Borovsky, 2020), each of which injects and imposes different structures with unique properties into the solar wind. Some pathways to solar wind formation result in solar wind plasma with properties and mesoscale structures that cannot be interpreted with the simple bimodal classification.

A key aspect of the new framework that allows for many pathways to solar wind formation is that it considers the time history of the solar plasma as it becomes the solar wind. This oft-ignored time history of solar wind formation imparts unique, observable imprints of the physical regime and processes that dominate each step; mesoscale structures can be one of the results. Observations of collisionality (Kasper et al., 2008; Kasper et al., 2017) and composition (Zurbuchen et al., 2002) are also examples where the solar wind exhibits a continuum of states rather than bimodality, and are examples where the time history of the plasma likely influences the resulting solar wind characteristics. The three steps of solar wind formation time history are source, release, and acceleration. The first step is the source of the plasma–i.e., whether it originates from a coronal hole (CH), which are tenuous and cooler, an active region (AR), which are dense and hot, or from the quiet sun (QS), which are of medium temperatures and densities. Separating the solar wind source into these three types of locations in the corona, which themselves are associated with different solar magnetic field configurations and plasma conditions, is essentially an empirical proxy for coronal heating (Viall et al., 2021). The second step is the release of plasma–whether the plasma is on open magnetic field lines, with one footpoint rooted in the Sun and the other already open to the heliosphere, or whether the plasma is on closed magnetic field lines, with both magnetic footpoints rooted in the Sun, requiring reconnection for the plasma to be released into solar wind. The third step is plasma acceleration, a process that continues through the high corona. All three steps can occur through a single physical process, such as turbulence; in such cases, the coronal heating mechanism, solar wind release, and solar wind acceleration all result from the same process (Cranmer et al., 2017). However, whenever the second step is reconnection, then steps one and three are necessarily separate processes because they occur in different physical regimes, thus leaving distinct plasma observables and structures in that parcel of solar wind. This time history of solar wind formation provides the seeding for eventual turbulence, and can also lead to the direct creation of mesoscale structures.

The second reason for studying mesoscales is that as the solar wind advects outward, these structures evolve, decay, and generate new mesoscale structures through turbulence, and thus represent a “laboratory” for studying this fundamental process (Bruno and Carbone, 2013).

The third reason for studying mesoscales is that dynamic solar wind and embedded mesoscale structures continually buffet all of the planets in our solar system, and are the medium through which larger structures and energetic particles propagate. Mesoscale structures and dynamics provide a fundamental transfer of energy from the Sun to Geospace, and constitute the ground-state of space weather–the every-day driving of Geospace that happens even during ambient conditions.

In the next three sections we delve into further detail on structures in the solar wind, represented in Figure 1, and elaborate on the three above-mentioned reasons that understanding mesoscale structures in the solar wind is critical for advancing our understanding of solar wind formation and evolution. In Section 2, we describe evidence of imposed and injected structures that leave imprints of coronal heating, and of the solar wind release and acceleration mechanisms. In Section 3 we describe evidence of turbulent evolution destroying and creating structures. In Section 4 we describe how these different types of mesoscale structures drive dynamics in the magnetosphere. Finally, in Section 5 we discuss the interplay and ambiguity between evolution vs. injection/imposing of these structures, when and under what conditions each mechanism may dominate, and outline potential paths forward for scientific understanding of this complex interconnection.

Much of the mesoscale structure and variability in the solar wind, especially observed within 1 AU, is imposed and injected from the Sun. For decades, researchers have speculated that many in-situ detected solar wind structures have a solar origin (Crooker et al., 1993; Crooker et al., 1996b), predating observations that were capable of conclusively and routinely differentiating between possible sources. Some fraction of the injected or imposed structures provide the energy for the turbulent cascade, or otherwise evolve as they advect, which we will describe in Section 3. In this section we focus on identifiable structures that are unambiguously of solar origin.

There exist two main observational methods for unambiguously identifying structures that were injected/imposed from the Sun. The first and most direct method is through remote imaging. This is typically done in white light, which is sensitive to electron density and location relative to the Thomson Surface (Vourlidas and Howard, 2006; Howard and DeForest, 2012), or extreme ultraviolet (EUV) emission, which is sensitive to electron density squared and is a function of temperature. When remote images exist with sufficient cadence and coverage, structures can be tracked in time from the solar corona as they accelerate outward into the solar wind (Sheeley et al., 1999; Viall et al., 2010; Viall and Vourlidas, 2015-07; DeForest et al., 2016; Alzate and Morgan, 2017; Rouillard et al., 2020; Alzate et al., 2021).

The second method is to use in situ observations of ionic and charge state composition. These quantities are frozen into the plasma at heights in the corona at which the collisional ionization and recombination rates are small. Therefore, above these heights these properties do not evolve, thus compositional changes observed in situ indicate that the structure was formed in the chromosphere and/or corona. The ionic charge states are generally frozen in by 1.5–3 solar radii, but some elements are not frozen in until as high as four or five solar radii (Landi et al., 2012). The relative abundance of elements with low first ionization potential (FIP) are set lower down in the chromosphere and a relative enhancement of the abundance of low FIP elements is an indicator of plasma release from the closed field corona (Peter, 1998; Laming, 2015). Recent theoretical work argues that the relative abundance of the element sulfur may be a unique indicator of the release of plasma from previously closed-magnetic field lines (Laming et al., 2019). The relative amount of ions as a function of mass can also change in the corona through gravitational effects (Raymond et al., 1997; Weberg et al., 2012-11). This could be the result of closed magnetic field lines with flows that are small enough such that gravitational settling occurs (Feldman et al., 1998). The relative amount of He 2++, or alpha/proton (AHe) ratio is also set in the solar atmosphere, but it is currently unknown which physical mechanism(s) determines the final ratio observed in the solar wind. AHe could be the result of mass dependent processes, particularly when closed field lines open to the solar wind, and lighter protons escape faster than alpha particles (Endeve et al., 2005-05). Currently, observations indicate that AHe is largely the result of FIP fractionation through the chromosphere (Rakowski and Laming, 2012), with an AHe “shutoff” (a rapid depletion in AHe) occurring prior to solar cycle onset that is likely the result of a mechanism near or below the photosphere (Alterman et al., 2021). In summary, the nature of the compositional change are linked to the physical processes involved in creating the solar wind and mesoscale structures that are injected/imposed from the Sun. Thus, such mesoscale structures contain imprints of the physical mechanisms that heat the solar corona and release and accelerate the solar wind.

Related, although specific entropy (T/n ^γ ) is not a conserved quantity, as it evolves with distance from the Sun, it is anticorrelated with the conserved quantity of charge state and therefore it can also be used as a proxy indicator of imposed or injected structures (Pagel et al., 2004). Likewise, temperature changes, which are not conserved, can be used when observed close to the Sun as a tracer of solar-created structures by the release of hotter plasma from closed-magnetic field lines on the sun through reconnection (Stansby and Horbury, 2018; DiMatteo et al., 2019). For example, in recent work on mesoscale-sized patches of switchbacks using data from Parker Solar Probe, (Woodham et al., 2020) argued that, based on enhanced T _‖ in the patches relative to their surroundings, the patches themselves could be structure injected from reconnection in the solar corona.

In a few isolated cases, which we describe in the examples below, it has been possible to directly link remote observations with in situ measurements of injected and imposed mesoscale structures and follow them from their creation at the Sun out into the Heliosphere. However, in most cases it is unknown how far out into the heliosphere the remotely observed structures survive. Likewise, even when compositional changes observed in situ indicate a solar creation mechanism, it is usually not known precisely which solar structures created the in situ-determined structures. When mesoscale structures are observed without compositional variations, their source is ambiguous, and could have been due to evolution en route, or imposed/injected structure. Thus, most connections between specific in situ phenomena and remote phenomena are qualitative.

The largest structure that the Sun imposes on the Heliosphere is that of its magnetic field, in which the global magnetic polarity inversion line in the corona results in the structure of the Heliospheric Current Sheet (HCS). As the solar cycle progresses, the Sun’s magnetic field becomes more complex, and can even form multiple HCSs. The HCS as a structure imposed from the Sun was confirmed through predictions using the magnetic field extrapolated from the photospheric measurements (Hoeksema et al., 1983) as well as with the AHe changes associated with the HCS (Gosling et al., 1981). There is evidence that the Sun also imposes spatial structures on mesoscales that survive at least through the inner heliosphere, and possibly out as far as Ulysses measurements (1–5 AU). The complexity of the photospheric magnetic field produces a web of separatrices, the S-web, (Antiochos et al., 2011; Linker et al., 2011; Titov et al., 2011; Pontin and Wyper, 2015) in the solar corona on mesoscales. Separatrices in the corona are regions where reconnection-released solar wind is most likely to occur. Thus, the imprint of the spatial structure of the S-web is predicted to impose boundaries between reconnection-released wind and open-field wind in the heliosphere on mesoscales (Crooker et al., 2004; Crooker and McPherron, 2012; Aslanyan et al., 2021). Recent simulations of interchange reconnection, which is induced at the lanes between cells of magnetic footpoint driving, predict that remnants of the scale size and pattern of photospheric driving by supergranular flows should be imposed along S-web corridors and into the solar wind (Aslanyan et al., 2021).

Another example of imposed mesoscale structure may be a type of pressure balance structure (PBS) observed by Ulysses, in which the changes in plasma pressure are approximately balanced by the changes in magnetic pressure and have a timescale of less than a day (McComas et al., 1995). There is evidence that polar plumes observed in polar coronal holes may be imposing these heliospheric counterparts as imprints in the polar solar wind (Poletto, 2015). Even in the ecliptic, fast speed streams observed by Helios also showed evidence of PBSs that were correlated with those expected from a superradial expansion of plumes into the heliosphere (Thieme et al., 1989; Thieme et al., 1990). Though PBSs can also be created through mechanisms en route such as slow mode waves (Yao et al., 2013a; Yao et al., 2013b), the high beta portion of the type of PBSs observed by Ulysses were highly correlated with AHe, and therefore likely of solar origin (Reisenfeld et al., 1999). Given the association of the observations with high latitudes during solar minimum (and therefore likely polar coronal holes), and the association with the high beta portion of the structures, (Reisenfeld et al., 1999) suggested that the structures were polar plume extensions. However, the structures’ observed frequency did not follow the expected frequency vs. latitude distribution for co-rotating features, and PBS signatures may also be susceptible to instability and mixing (Parhi et al., 1999).

Towards the middle range of the mesoscales, (Borovsky, 2008) studied the scale size of flux tubes observed at 1 AU and found a median scale size of ∼440 Mm, and suggested that they were fossilized structures imposed by structures from the Sun. (Borovsky, 2016) examined what they classified as “unperturbed coronal hole plasma” between 0.3 and 2.3 AU and found the plasma to be structured in many of its components, including in AHe and proton specific entropy variations, confirming a solar source to much of the coronal hole wind variability. They argued the radial size scales measured at the spacecraft correspond to longitudinal scales at the Sun as a result of solar rotation. Assuming this geometry, they concluded that the longitudinal scales of the corresponding structures at the Sun would be a significant fraction of a supergranule (which are 30–35 Mm diameter in the photosphere). Thus, they could be due to open magnetic field funnels imposing structure on the solar wind. Examining the boundaries between these mesoscale structures, (Borovsky, 2020b) showed that discontinuous changes in AHe are correlated with discontinuities in the magnetic field direction, i.e., current sheets. They showed that this correlation applies to all types of solar wind, and that the discontinuities are weaker away from the changes in AHe. Lastly, they showed that sharp changes in electron strahl intensity also corresponded to larger discontinuities in the magnetic field direction. Together, these observations support the interpretation that much of the mesoscale structure in the solar wind is likely imposed flux-tube structure from the solar corona.

There are also time-dynamic processes in the solar atmosphere that inject structure into the solar wind and heliosphere. The largest injected transient structures are CMEs. These are explosive events that can have speeds of up to thousands of km/s. They involve the buildup and release of magnetic energy at a magnetic polarity inversion line. Though large CMEs are generally considered to be created by different phenomena than the ambient solar wind, the same mechanism of magnetic energy build up at a polarity inversion line and subsequent release that creates CMEs is likely also responsible for a spectrum of mesoscale structures in the solar corona from pseudostreamer jets (Kumar et al., 2021) down to small X-ray and EUV jets (Sterling et al., 2015; Wyper et al., 2017). It is predicted that such jets in polar coronal holes could inject mesoscale structures into the solar wind that could be observed in the near-Sun environment with Parker Solar Probe (Roberts et al., 2018). However, based on empirically-determined jet rates and filling factors (Savcheva et al., 2007; Sako et al., 2013), (Roberts et al., 2018) estimated that Parker Solar Probe would only encounter an average coronal hole jet about once in 50–100 days of observations. While it is currently unknown how far out into the heliosphere distinguishable jet signatures survive, it has long been thought that microstreams observed in Ulysses could be remnants of x-ray or EUV jets. Microstreams have velocities ± 35 km/s relative to background, last 6 h or longer, and occur in conjunction with large angle magnetic discontinuities. They have higher kinetic temperatures, proton flux, and a slight enhancement of low FIP elements compared to the average fast solar wind. The compositional changes associated with microstreams indicate a solar origin (Neugebauer et al., 1995; Neugebauer et al., 1997). (Neugebauer, 2012) argued specifically for coronal x-ray jets as the solar source, but polar plumes are also a possibility due to their association with x-ray jets (Neugebauer et al., 1997; Poletto, 2015). Using simulations of jets, (Karpen et al., 2016) demonstrated that the associated Alfvén wave and density and velocity enhancements produced by jets are sustained through the outer corona, and are consistent with in situ observations of microstreams. Similarly, (Velli et al., 2011) simulated polar plumes and demonstrated that the observed velocity increase in microstreams could be explained by different heat deposition in plumes. Evidence suggests that plumes are driven by jetting activity at their base (Raouafi et al., 2016), thus for progress it is likely necessary to treat x-ray jets and plumes as different observable manifestations of a common process.

At the large scales, but at slower speeds, are slow helmet streamer blowout CMEs, a subset of which are the so-called “stealth” CMEs, that do not have an obvious signature in the low corona (Howard and Tappin, 2008; Robbrecht et al., 2009). Stealth CMEs originate higher up in the corona, are slow (about 300 km/s) (Ma et al., 2010; Howard and Harrison, 2013), and, though “stealthy,” their connection through the global-scale coronal magnetic field to the low corona can be identified through advanced image processing (Alzate and Morgan, 2017). (Lynch et al., 2016) modeled a stealth CME by imposing a large scale global shear meant to represent the effects of differential rotation on the global coronal magnetic field. They showed that the footpoint energization in such driving takes place across the polarity inversion line associated with the HCS and helmet streamers, as opposed to a polarity inversion line in an active region.

As with explosive CMEs, streamer blowout CMEs likely also represent the large end of a continuum of structures created through a common physical mechanism. There is an abundance of mesoscale structures that are also associated with the HCS. (Crooker et al., 1993; Crooker et al., 1996a) identified mesoscale structures within the HCS in situ at L1, which they demonstrated could not be due to a wavy HCS traversed by the spacecraft. Instead, they suggested a solar source to the structures because the observed structures were consistent with tangled flux ropes, and flux ropes are generally considered a signature of reconnection. (Suess et al., 2009) expanded on prior in situ studies of the AHe depletions occurring at the HCS, and showed that the AHe changes are not centered on the HCS. The offset AHe changes are consistent with solar reconnection-injected structure near the HCS, rather than a static HCS. Thus, the imposed large scale structure of the HCS is also comprised of injected structures at mesoscales; this picture is most recently confirmed by Parker Solar Probe in situ observations close to the Sun (Lavraud et al., 2020). Also consistent with this picture, mesoscale plasma blobs are observed in remote white light imaging to be released from the tips of helmet streamers on scales of many hours (Sheeley et al., 1997; Wang et al., 1998; Wang et al., 2000; Harrison et al., 2009; Rouillard et al., 2009; Sheeley and Rouillard, 2010). Their continued acceleration is observed out to 30 solar radii, where they reach typical speeds of around 300 km/s. In some cases, streamer blobs have been tracked from their helmet streamer release out to their observation in situ at 1 AU (Rouillard et al., 2010a; Rouillard et al., 2010b), and Parker Solar Probe in situ data taken around 30 solar radii (Rouillard et al., 2020). Reconnection at the helmet streamer seems to be fundamental to the release of blobs. Observations in white light of raining inflows (Sheeley et al., 1997; Wang et al., 2000) and the dipolarizations associated with blobs (Sanchez-Diaz et al., 2017), suggests that the reconnection often occurs around four to five solar radii. MHD models (Higginson and Lynch, 2018; Lynch, 2020) and 2D thermal models (Allred and MacNeice, 2015; Endeve et al., 2005-05) also show that helmet streamer tips are dynamic and prone to reconnection. This general picture of streamer reconnection led (Lynch et al., 2016) to argue that stealth CMEs represents the middle of the continuum between fast CMEs and mesoscale helmet streamer blobs, wherein the same universal process of shear across a polarity inversion line leads to reconnection-released plasma into the heliosphere.

On mesoscales of tens of minutes to a couple of hours are puffs and periodic density structures. Some of these have been observed in white light images to originate at the Sun as low as 2.5 solar radii, and can be followed out to about 50 solar radii (Sheeley et al., 1997; Viall et al., 2010; Viall and Vourlidas, 2015-07; DeForest et al., 2016; DeForest et al., 2018). As with helmet streamer blobs, periodic density structures occur preferentially near the HCS (Viall and Vourlidas, 2015-07). They occur at several characteristic scales, including 90 min (Viall and Vourlidas, 2015-07) and shorter (DeForest et al., 2018). In a simulation of reconnection at the helmet streamer, (Réville et al., 2020) demonstrated that periodic density structures at the HCS could be the result of the tearing mode. On the other hand, (Allred and MacNeice, 2015) and (Schlenker et al., 2021) argued that the periodicity was determined by the interplay between heating and expansion of the last closed field lines, and the retraction of field lines after reconnection. (Pylaev et al., 2017) argued for a third mechanism, wherein a standing shock at the 90 min acoustic cutoff frequency of the corona drives reconnection. Regardless of the precise mechanism, the timescale of the resulting density structures is a constraint on how magnetic reconnection occurs at the helmet streamers. With limitations of current remote white light instruments in terms of sensitivity, and temporal and spatial resolution, periodic density structures are too small and faint to see in more tenuous wind outside of streamers, or beyond about 50 Rsun where the density and associated signal is too weak. However, (DiMatteo et al., 2019) identified several instances of 90 min periodic density structures at the HCS close to the Sun in Helios data. They were associated with temperature changes, and thus determined to be of solar origin. At 1 AU, (Kepko et al., 2016) showed an example of 90 min periodic density structures associated with compositional changes, and (Viall et al., 2009b) showed an example of 30 min periodic density structures associated with AHe changes. Thus, at least some periodic density structures survive through the inner heliosphere. Both (Kepko et al., 2016) and (DiMatteo et al., 2019) showed evidence that at least one of the structures in the periodic density train was a flux rope, and so consistent with reconnection as their formation mechanism.

More generally, mesoscale structures in the heliosphere away from the HCS are expected as a result of interchange reconnection at the boundaries between open and closed fields or S-web arcs (Higginson et al., 2017a; Higginson et al., 2017b). Indeed, (Mason et al., 2019) observed evidence of interchange reconnection at a null-point topology (i.e., a distinct closed magnetic field structure from the helmet streamer) in the corona. With current sensitivity limitations in EUV data, it was not possible to see the solar wind outflows associated with the reconnection. In one event of periodic density structures observed close to the Sun by Helios, the solar coronal source was confirmed via concurrent temperature changes, and the location was determined to be far from the HCS, an important test of the S-web theory of reconnection-released solar wind (DiMatteo et al., 2019). Analyzing 25 years of Wind solar wind density data, (Kepko et al., 2020) identified periodic density structures in all types of solar wind, including fast, ecliptic wind. They occurred at particular timescales, or equivalent radial length scales, that were associated with the solar cycle, and the terminator (McIntosh et al., 2019). Since the 25 years Wind study used all periodic density structures that were identified, without testing for associated compositional changes, it is possible that not all of those were created at the Sun. Even for those that are, further investigation is required to determine if their properties are a function of different types of solar wind sources, e.g. reconnection at the HCS versus other S-web arcs.

Structuring and/or destruction of mesoscale solar wind structures can also occur through turbulence. As Figure 1 shows, the scales of observed solar wind mesoscales also correspond to the energy containing and inertial range scales expected from turbulence. Both fluid and MHD turbulence are driven by nonlinearities represented by the underlying equations of motion. These nonlinearities lead to cross-scale cascades of energy first described by Kolmogorov (1941) and Kraichnan (1967) and treated by many authors (Frisch, 1995; Bruno and Carbone, 2013). The turbulent cascade carries energy and structure from the large energy-containing scale through a very broad inertial range of scales (roughly encompassing the mesoscales defined above) that are dominated by the turbulent cascade, to a dissipation scale where the energy becomes a source of heat (Leamon et al., 1998). In the case of the solar wind, the energy containing scales are determined by dynamics and structure of the corona itself (Tu and Marsch, 1995; Chae et al., 1998; Cranmer et al., 1999). A large variety of mechanisms including hydrodynamics, MHD modes, and magnetic reconnection, can give rise to turbulent cascades; once the system develops a cross-scale energy cascade and characteristic spectral power-law signature, it is considered “turbulent” regardless of the specific mechanism. The importance of a cross-scale cascade is that it gives rise to perturbations in all major measurable parameters of the flow, including density, velocity and magnetic fields, and other structural identifiers. The specific relationship between different types of perturbation depends on the mechanism itself.

There are many lines of evidence indicating that the solar wind is processed by turbulence as it moves through the solar system, e.g., see review by (Matthaeus and Velli, 2011). To measure the turbulence properties using in situ data requires the inclusion of the Taylor approximation that the dominant source of variability is spatial structures sweeping over the spacecraft. Therefore, time spectra yield equivalent spatial spectra of perturbations in all major wind parameters (Matthaeus and Velli, 2011); the validity of the Taylor approximation is also corroborated by multi-spacecraft measurements of at least some coherence parameters (e.g., Matthaeus et al. (2005)). That corroboration is important, because the Taylor approximation is known to be limited in the context of turbulence (Klein et al., 2014; Bandyopadhyay et al., 2020).

The presence of a turbulent cascade at 1 AU has long been inferred from time spectra of in situ measurements (Coleman, 1966; Horbury et al., 2005). Comparisons of the magnetic field spectra measurements show that the break point between the energy containing scales and the inertial range evolves with distance from the Sun. In the fast wind, this break point occurs near 10 mHz at 0.3 AU and steadily evolves to lower frequencies at larger distances of less than 0.1 mHz at 4.8 AU (Bruno et al., 2009; Bruno and Carbone, 2013). Those results also showed that the slow wind is not observed to have a corresponding break between the inertial and energy containing scales, but more recent results with Parker Solar Probe show that the slow wind has a break to energy containing scales, but at a lower frequency than the fast wind (Chen et al., 2021).

The correlation length is often used to define the large end of the inertial range of scale, under the assumption that it represents the largest scale of turbulent eddies. Multi-spacecraft measurements have yielded 1,000–2000 Mm as the correlation scale at 1 AU (Matthaeus et al., 2005), corresponding to 1–2 h crossing time, although the measurement itself is sensitive to analysis technique (Isaacs et al., 2015) and may be longer. While in-situ measurements are limited to statistical analyses of the overall character of the solar wind, imaging measurements afford direct detection of individual features. The coherence length result is corroborated by test particle analysis using features in comet Encke’s tail (DeForest et al., 2015), which also identified an eddy size scale of approximately 1,000–2000 Mm (i.e., with roughly 90 min crossing time) at 1AU. However, the comet tail result may be affected by a turbulent “vortex street” from interaction between the solar wind and the comet (Nisticò et al., 2018), and therefore may differ from the turbulent field of the bulk solar wind itself. This uncertainty associated with the characteristic coherence length is reflective of the difficulty of measuring the “native” solar wind flow. While ample spectral signatures indicate the presence of a turbulent cascade, definitively measuring the spectral limits of the cascade - and therefore the dominant processes affecting solar wind variability at different scales - remains an open problem, in part because different solar wind parameters yield different spectral characteristics (Bruno and Carbone, 2013).

In addition to direct spectral measurements and correlation lengths, several other key results demonstrate that the statistical characteristics of the solar wind evolve with propagation, approaching a state consistent with turbulent processing. Tracing of the cross-helicity evolution with distance from the Sun provided one of the first clear lines of evidence that nonlinear dynamical evolution occurs in the solar wind (Roberts et al., 1987). More recently (Telloni et al., 2021) measured a stream of solar wind at 0.1 and 1.0 AU and showed that the magnetic spectral density, flatness, and higher order moment scaling laws were consistent with Alfvénic fluctuations near the Sun evolving into fully developed turbulence. Similarly, (Chen et al., 2020) showed that turbulence evolves between 0.17 and 1 AU: at 0.17 AU the data showed increased energy spectral density, a slope of −3/2, lower magnetic compressibility, and increased relative amount of outward propagating Alfvénic fluctuations compared to inward. Close to the Sun, both the magnetic field and velocity spectra have a slope of −3/2, but only the magnetic spectra is observed to steepen with distance, and the outward dominance of the Alfvénic fluctuations is observed to decrease with distance (Chen et al., 2021; Shi et al., 2021). The evolution of the outward wave dominance as well as the evolution of the spectral break point with distance is supported by MHD simulations of turbulence (Roberts et al., 1991). As physics-based models of turbulence become more complex, they are able to reproduce many of the observed characteristics of the solar wind (Roberts and Ofman, 2019; Adhikari et al., 2021).

The dissipation scale, which defines the small-scale end of the turbulent inertial range of scales, varies with plasma condition and with distance from the Sun; a useful benchmark at 1 AU is 2 s (Leamon et al., 1998), or approximately 600 km. At scales much smaller than this, the spectrum steepens as kinetic phenomena convert the perturbations to fully randomized heat. More recent work has demonstrated that the relationship between temperature and velocity evolves with distance in a way that is consistent with turbulent processing (Elliott et al., 2012; Lionello et al., 2014). Entropy also increases and has less variability with distance, indicating heating and turbulent processing (Roberts et al., 2005). The so-called switchbacks observed by Parker Solar Probe exhibit different break scales between inertial and dissipation scales and increased level of intermittency than the surrounding wind, perhaps contributing to the turbulent heating in the inner heliosphere (Martinović et al., 2021).

Importantly for the purposes of this paper, active turbulence would process any injected or imposed mesoscale structures from the Sun. A general trend of processing and statistical modification is observed to continue to over 30 AU as solar wind features are “worn down” by dynamic interaction with other parcels of wind (Elliott et al., 2016). The solar wind at 0.33 AU was observed with the Helios spacecraft to contain more and sharper spikes in velocity (Horbury et al., 2018) than further away from the Sun, and the trend continues inward to the corona itself in the form of switchbacks observed by Parker Solar Probe (Bale et al., 2019; Kasper et al., 2019). Indeed, the microstreams observed by Ulysses - likely related to the larger of the switchbacks that do survive - are themselves observed to evolve in distance from the Sun (Reisenfeld et al., 1999). This corroborates the picture of a solar wind whose structure evolves from the “young” state with spatial and temporal structure injected by coronal processes, to a more processed state that reflects the observed turbulent spectrum further from the Sun.

There is also evidence that turbulence generates new structures in the solar wind on mesoscales. As one example, there is an active debate as to whether the switchbacks observed by Parker Solar Probe (and described above) are created through turbulence or not, with many arguing that their observed characteristics are consistent with turbulent formation (Squire et al., 2020; Tenerani et al., 2020; Shoda et al., 2021). In another example, work by (DeForest et al., 2016) showed that at least some compact bright features in the images form in the solar wind as it propagates. They identified “flocculae” that are observed to “fade in” to the overall flow between 20 and 80 solar radii from the Sun (see Figure 1). Typical flocculae are oblong: about the same size as streamer puffs (∼1 solar radius at 30 solar radii altitude) but 3x–10x wider. These have been interpreted as signs of the isotropization of shear-driven turbulence (Chhiber et al., 2019), which may arise locally or be excited as anisotropic magnetically-guided turbulence carried from the outer corona itself (Cranmer, 2012; Cranmer and Woolsey, 2015; Oughton et al., 2015). Similarly, analysis of Helios data showed that the heliospheric current sheet becomes more complex with distance, as indicated by more current-sheet crossings (Roberts et al., 2005). In contrast, a statistical analysis of Helios, IMP8, Wind, ACE and Ulysses data also showed that the occurrence rate of flux ropes in the HCS decreases in frequency and and flux ropes are larger in size with distance from the Sun (Cartwright and Moldwin, 2008; Cartwright and Moldwin, 2010), indicating that they likely merge.

Taken as a whole, these results indicate that solar wind is turbulent. Structure at or below 1,000 Mm observed at 1 AU are well within the turbulent cascade, in a sequence that begins with both spatial and temporal driving in the corona and processes the imprinted structure through turbulent evolution of shear flows and eddies. Large-scale turbulent eddies appear to form and be isotropized at or shortly above the transition from the low-β corona to moderate-β solar wind, likely about 0.3 AU from the Sun (DeForest et al., 2016), and the cascade appears to fully develop between this distance and 1 AU although the turbulence may remain anisotropic toward the smaller-scale end of the inertial range (Bruno and Carbone, 2013). However, many injected and imposed structures observed on scales of tens of minutes and scales of hundreds to several thousand Mm have been observed to survive to at least 1 AU. We return to the inherent ambiguity of these results and its interpretation in the context of mesoscale structures in Section 5.

The structured solar wind impacts the magnetosphere in several ways. The solar wind dynamic pressure, p d y n = n i m i v i 2 , is the primary driver of the magnetopause standoff distance and the size of the magnetosphere. Any mesoscale solar wind structures that are comprised of changes in density and/or velocity will alter the magnetic field magnitude inside the magnetosphere. The interaction between the solar wind dynamic pressure and magnetosphere can be considered quasi-stationary in the response to any solar wind structures that have scales larger than the dayside magnetosphere. As shown in Figure 1 even the small end of the mesoscales (down to about 100 Mm) in the solar wind are as large as Earth’s magnetosphere and, therefore, can drive dynamics in a quasi-stationary way. At ∼100 Mm, equivalent to a 4 min duration structure advecting at 400 km/s, the scale size of the structure is approximately similar to the size of the dayside magnetosphere. The temporal scale of the interaction is also near the timescale that information propagates across the magnetosphere, the so-called Alfvénic travel time. Therefore, the quasi-static assumption breaks down for solar wind structures on scales smaller than 100 Mm and/or shorter than 4 min, and propagation effects through the magnetosphere need to be considered. Regardless of the exact timescale of the interaction, solar wind dynamic pressure variability injects compressional energy into the Earth’s magnetosphere, where it can affect particle energization, diffusion, and transport.

Large scale solar wind structures, such as CIRs or SIRs that form when a faster wind overtakes a slower wind, are important drivers of magnetospheric activity (Gosling and Pizzo, 1999; Tsurutani et al., 2006; Kilpua et al., 2017). In particular, for Earth’s radiation belts it has been recognized for decades that there is a strong correlation between solar wind speed and the flux of relativistic electrons, particularly in the outer zone and for V _sw > 500 km/s (Paulikas and Blake, 1979; Miyoshi and Kataoka, 2005; Borovsky and Denton, 2006; Bortnik et al., 2006; Yuan and Zong, 2012). While CMEs are often considered to be large drivers of space weather, SIR-driven geomagnetic storms often exhibit higher fluxes of radiation belt electrons compared to CME-driven storms (Borovsky and Denton, 2006; Kataoka and Miyoshi, 2006; Kilpua et al., 2015; Turner et al., 2019), especially at larger radial distances (>4.5 R _E ) and during the declining phase of the solar cycle. The general process of radiation belt enhancements is energization via local chorus waves combined with radial diffusion (see review by Li and Hudson (2019)). While the comparatively long overall SIR scale is important for radiation belt flux enhancements, the mesoscale structures embedded within that large scale structure appear to be an important contributor as well. The compression region between the fast and slow wind is filled with dynamic pressure fluctuations that provide a source of broadband compressional power that drives magnetospheric ultra low frequency (ULF) waves (Kilpua et al., 2013; Kepko and Viall, 2019). ULF waves are known to be an important magnetospheric process that can lead to enhanced radial diffusion, energization, or even loss to atmospheric precipitation. When combined with high solar wind dynamic pressure, this externally driven ULF wave activity can scatter electrons to large radial distances where they can fill a broad region of the radiation belts, or can be lost due to magnetopause shadowing (Turner et al., 2012; Hietala et al., 2014). The entire SIR driving of the magnetosphere can take several days, with the loss of outer zone electrons apparently more dominant during the early part of the SIR, and a net increase in the flux of energetic electrons over the course of the entire SIR event. This highlights the importance of understanding all of the mesoscale aspects of solar wind driving within large scale events.

The subset of mesoscale structure that manifest as periodic density structures are of particular interest for magnetospheric dynamics, because they can drive magnetospheric ULF pulsations at discrete periodicities for extended intervals. There is now a substantial body of research demonstrating magnetospheric pulsations that are directly-driven by solar wind periodic density structures (Kepko et al., 2002; Stephenson and Walker, 2002; Kepko and Spence, 2003; Viall et al., 2009a; Villante et al., 2013; DiMatteo and Villante, 2017). This includes observations of solar wind-driven pulsations in ground magnetometer data (Villante and Tiberi, 2016), high latitude ionospheric radar observations (Fenrich and Waters, 2008), polar UV imaging data (Liou et al., 2008), and even the equatorial ionosphere (Dyrud et al., 2008). MHD simulations have confirmed that cyclic solar wind dynamic pressure structures directly drive magnetospheric oscillations, and locations of field line resonance will even amplify the waves (Claudepierre et al., 2010; Hartinger et al., 2014). The apparent frequencies of periodic density structures in the frame of the magnetosphere is often between 0.5 and 4 mHz (Viall et al., 2009a; Kepko et al., 2020), which is similar to the drift period of radiation belt particles. Kepko and Viall (2019) showed an event where radiation belt particles were precipitating to the atmosphere with a periodicity determined by the solar wind periodic density driver. Recent work utilizing Balloon Array for Radiation-belt Relativistic Electron Losses (BARREL) measurements of particle precipitation suggests an association between solar wind periodic density structures and electromagnetic ion cyclotron (EMIC) wave power enhancements, which scatters energetic electrons into the loss cone where they are then lost to Earth’s atmosphere (Breneman et al., 2020).

An additional mesoscale solar wind structure-magnetosphere interaction that needs to be considered are intervals of large interplanetary magnetic field (IMF) that could lead to enhanced reconnection at the dayside magnetopause. Earth’s magnetic field points northward at the magnetopause, and therefore when the IMF has a large southward component (B _south ), magnetic reconnection is likely to occur. Dayside magnetic reconnection is the primary mechanism by which solar wind energy enters the magnetosphere, and is the ultimate source of much of the dynamics that occur, including geomagnetic storms and substorms. High speed solar wind (>750 km/s) is known to be dominated by large amplitude Alfvén waves (Tsurutani et al., 1994). Within SIRs, these Alfvén waves are compressed and increase in amplitude as the high speed flow impinges upon the slower flow ahead, leading to a pile-up of large amplitude fluctuations in solar wind IMF B _south . The combination of high solar wind speed, density, and B _south often leads to intense geomagnetic activity. The auroral activity driven by this solar wind interaction has been termed High Intensity Long Duration Continuous AE Activity (HILDCAA) (Tsurutani and Gonzalez, 1987). The relationship between these large amplitude Alfvén waves and the mesocale density structures that are also inherent to SIRs is an area ripe for study.

In some ways, the magnetospheric impact of solar wind structures is independent of whether the solar wind structures are injected/imposed versus formed en route through turbulence. On the other hand, while turbulence and coronal processes can both produce mesoscale structures in the geoeffective size scale range of 100 Mm and greater, coronal processes may produce mesoscale structures with different properties. For example, it seems that unique processes in the corona make them periodic (Kepko et al., 2016; Viall et al., 2009b; Viall and Vourlidas, 2015-07). In another example, (Kepko and Viall, 2019) demonstrated that SIRs compress and amplify existing periodic density structures in the slow wind, thereby increasing their impact on Earth’s magnetosphere. This is a clear example of where both the injection mechanisms and evolution impacted Earth’s response. In summary, for full predictability of space weather at Earth and the nature of the magnetospheric driving, it is important to understand how much and which types of mesoscale structures are formed through turbulence, or injected/imposed from the solar corona.

Figure 1 describes the phenomenological structure in the solar wind, from kinetic through mesoscale to large-scale. The turbulence regimes discussed in Section 3, and the injected and imposed structures from the Sun discussed in Section 2, both produce solar wind structures at mesoscales. There is a clear interplay between imposed and injected structure, the evolution of such structure en route to 1 AU, and turbulence creating new structures, all of which comprise the zoo of mesoscale structures at 1 AU. The goal is to understand this interplay and to determine which type of structures dominate the solar wind under which conditions.

The solar wind contains structures that are injected and imposed directly by the Sun and structures that are generated and evolve en route due to turbulence. At the extremes of the spatial scales, it is simple to differentiate these creation mechanisms. Yet there exists a several orders of magnitude gap between these two scales, the mesoscale. In this regime, with a size scale at 1 AU of ∼5–10,000 Mm and time scales of 10 s–7 h, both injected/imposed and structures generated en route co-exist, and it is often difficult to disentangle the two. Competition between the imposed and injected structures with turbulent and other evolution leads to complex structuring and dynamics. Injected mesoscales carry imprints of the processes that release solar plasma and heats and accelerates the solar wind, and therefore studying them can provide insight into the generation of the solar wind. The mesoscale regime is also the region of observation space that is grossly under-sampled. Sparse in situ measurements are limited to radial profiles of the solar wind as the wind advects past the spacecraft, and remote imaging currently cannot resolve many mesoscales. There is very limited azimuthal coverage, and even less out of the ecliptic coverage. Understanding mesoscale structures is important as they are drivers of Earth’s magnetosphere, and important upstream conditions for the structuring of CMEs, CIRs, and the propagation of energetic particles.