the Creative Commons Attribution 4.0 License.

the Creative Commons Attribution 4.0 License.

# Quasi-separatrix layers induced by ballooning instability in the near-Earth magnetotail

### Zechen Wang

### Jun Chen

### Xingting Yan

Magnetic reconnection processes in the near-Earth magnetotail can be highly three-dimensional (3-D) in geometry and dynamics, even though the magnetotail configuration itself is nearly two-dimensional due to the symmetry in the dusk–dawn direction. Such reconnection processes can be induced by the 3-D dynamics of nonlinear ballooning instability. In this work, we explore the global 3-D geometry of the reconnection process induced by ballooning instability in the near-Earth magnetotail by examining the distribution of quasi-separatrix layers associated with plasmoid formation in the entire 3-D domain of magnetotail configuration, using an algorithm previously developed in the context of solar physics. The 3-D distribution of quasi-separatrix layers (QSLs) as well as their evolution directly follow the plasmoid formation during the nonlinear development of ballooning instability in both time and space. Such a close correlation demonstrates a strong coupling between the ballooning and the corresponding reconnection processes. It further confirms the intrinsic 3-D nature of the ballooning-induced plasmoid formation and reconnection processes, in both geometry and dynamics. In addition, the reconstruction of the 3-D QSL geometry may provide an alternative means of identifying the location and timing of 3-D reconnection sites in the magnetotail from both numerical simulations and satellite observations.

There has been a long-standing controversy over whether the magnetic reconnection or the ballooning instability in the magnetotail actually triggers the onset of substorms, since both mechanisms found support in observation and simulation (e.g., Baker et al., 1996; Lui, 1991; Angelopoulos et al., 2008; Panov et al., 2012). To resolve the controversy, it may be necessary to study and understand the evolution of the magnetotail in the substorm growth phase, and to identify and predict the signatures of magnetic reconnection and ballooning instability in the magnetotail, as well as their potential connections. In practice, the conventional two-dimensional reconnection models with spatial symmetries in both in-flow and out-flow regions are often used to identify and interpret the signatures of reconnection processes from observational data. However, one fundamental question that remains to be addressed is whether the magnetic reconnection in the magnetotail, when it does occur, can always be interpreted in the conventional two-dimensional picture, and if not, how one may characterize its intrinsically three-dimensional geometry.

The overall evolution of the magnetotail-like configuration has been studied for many years (Schindler, 2007, and references therein). In particular, the plasmoid formation process was investigated in detail in earlier 3-D resistive magnetohydrodynamic (MHD) simulations by Birn and Hones Jr. (1981) and by Hesse and Birn (1991), for example. Recently, our simulations based on the 3-D full MHD equations implemented in the NIMROD code (Sovinec et al., 2004) have found a plasmoid formation process in the generalized Harris sheet that is often used as an approximate configuration of the near-Earth magnetotail prior to a substorm onset (Zhu and Raeder, 2013, 2014). Those simulations demonstrate that the embedded thin current is unstable to ballooning-mode perturbations, and the nonlinear development of the ballooning instability is able to induce the onset of reconnection and the formation of plasmoids in the current sheet where there is no pre-existing X-point or X-line.

In comparison to the low-*S* (i.e., Lundquist number) regime, where *S*∼10^{2} considered in the earlier simulations by Birn and Hones Jr. (1981), our recent
simulations are in the higher-*S* regime, where *S*≥10^{4}, which may be
more relevant to the collisionless regime of plasmas in the magnetotail. In
the low-*S* regime, the magnetotail plasma is linearly unstable to resistive
tearing modes, and the associated reconnection process is initially a linear
process. In contrast, in the higher-*S* regime considered in our recent
work (Zhu and Raeder, 2013, 2014), the generalized Harris sheet is linearly stable
to resistive tearing modes. The onset of reconnection is a consequence of the
nonlinear development of ballooning instability, and the subsequent
reconnection is a nonlinear process. Thus, the reconnection processes in the
low-*S* regime reported in the earlier work by Birn and Hones Jr. (1981) and
by Hesse and Birn (1991) are essentially 2-D, whereas the reconnection process in
the higher-*S* regime in our simulations is an intrinsically 3-D process that
does not exist in the 2-D geometry. This key difference distinguishes our
recent work (Zhu and Raeder, 2013, 2014) from the previous work by Birn and Hones Jr. (1981)
and by Hesse and Birn (1991).

Although our previous work has demonstrated in MHD simulations the formation of plasmoids induced by ballooning instability in the generalized Harris sheet (Zhu and Raeder, 2013, 2014), the global 3-D structure of the ballooning-induced reconnection was not clear. In particular, the reconnection process in our simulations is no longer invariant along the equilibrium current direction, unlike in a conventional 2-D reconnection process. This leads to general questions as to where and how reconnection takes place in the 3-D configuration, as well as how the global structure of the 3-D reconnection process can be characterized and captured in ways different from the more familiar 2-D reconnection process. More fundamentally, it has remained unclear whether this 3-D reconnection process can be reducible to or interpretable in terms of the conventional 2-D reconnection processes.

Whereas the overall evolution of the magnetotail-like configuration has been studied in the space community for many years, the irreducible dimensionality of the reconnection process associated with the evolution of ballooning instability has never been addressed before in the literature, including the papers by, e.g., Birn and Hones Jr. (1981) and Hesse and Birn (1991) which were reviewed in the book by Schindler (2007). There is also a long history of work trying to identify the possible role of out-of-plane instabilities in reconnection (see, for example, Pritchett, 2013, and Sitnov et al., 2014). Different from those previous works, in this work we intend to identify the geometry features associated with the intrinsically 3-D reconnection process induced by the ballooning instability in the near-Earth magnetotail, in light of those questions raised in the previous paragraph.

Similarly to the magnetic island, the plasmoid presented in this work is
identified in the *x*−*z* plane as a finite region of closed magnetic flux
bounded by a separatrix with a single X-point (Otto et al., 1990; Zhu and Raeder, 2014). It is a
two-dimensional projection onto the *x*−*z* plane of three-dimensional magnetic
field lines in regions of magnetic reconnection. Whereas the plasmoid
structure itself appears out of a two-dimensional projection, its occurrence
in the *x*−*z* plane is periodic in the *y* direction in our simulations, which
indicates that the overall reconnecting field-line structure is intrinsically 3-D.
Such a relation between the 2-D plasmoid and the 3-D reconnection is indeed
possible, as demonstrated in our simulations, and may be more quantitatively
captured in the 3-D structure and distribution of quasi-separatrix layers
(QSLs).

The QSL has long been a powerful concept and method for the analysis and understanding of magnetic structures in the solar atmosphere (Titov and Démoulin, 1999; Titov et al., 2002). Recently the concept of QSLs has also been effectively applied to the analysis of laboratory reconnection experiments (Lawrence and Gekelman, 2009). Previously, we calculated the spatial distribution and the structure of the QSLs, as well as their temporal emergence and evolution, within the equatorial plane (Zhu et al., 2017), based on the earlier simulation results on the formation of plasmoids induced by ballooning instability in the magnetotail (Zhu and Raeder, 2013, 2014). There we found the QSL structures are not invariant along any direction within the 2-D equatorial plane; instead they are disconnected and isolated local structures. Those initial findings start to reveal the intrinsic 3-D nature of the reconnection induced by ballooning instability in the generalized Harris sheet, which is irreducible to 2-D reconnection processes in geometry and dynamics within the 2-D equatorial plane. In this work, we extend our previous study within the 2-D equatorial plane to the entire 3-D domain of the near-Earth magnetotail. Using a newly developed implementation for efficiently computing the squashing degree of magnetic field lines in any 3-D domain (Liu et al., 2016), we obtain the 3-D distribution of QSLs as well as their evolution in the near-tail plasma sheet. The intersection of the 3-D distribution of QSLs with the equatorial plane recovers results from our previous work. More importantly, the calculated 3-D distribution of QSLs provides a complete and global view of the geometric structure of the 3-D reconnections associated with the plasmoid formation induced by the nonlinear ballooning instability in the near-Earth magnetotail.

The rest of the paper is organized as follows. We first briefly review our previous simulation results for the plasmoid formation process induced by ballooning instability in Sect. 2. Next in Sect. 3 we describe the method we use for efficiently evaluating the squashing degrees of entire magnetic fields. Both 2-D and 3-D distributions of QSLs revealed from the squashing degree calculation are reported and analyzed in Sect. 4. Finally, summary and discussion are given in Sect. 5.

Our recent MHD simulations are developed to demonstrate the dynamic process
of plasmoid formation induced by nonlinear ballooning instability of the
near-Earth magnetotail. In these simulations, the magnetic configuration of
the near-Earth magnetotail is modeled using the generalized Harris sheet,
which can be defined in a Cartesian coordinate system as ${\mathit{B}}_{\mathrm{0}}(x,z)={\mathit{e}}_{y}\times \mathrm{\nabla}\mathrm{\Psi}(x,z)$,
$\mathrm{\Psi}(x,z)=-\mathit{\lambda}\mathrm{ln}\frac{\mathrm{cosh}\left[F\left(x\right)\frac{z}{\mathit{\lambda}}\right]}{F\left(x\right)}$,
$\mathrm{ln}F\left(x\right)=-\int {B}_{\mathrm{0}z}(x,\mathrm{0})\mathrm{d}x/\mathit{\lambda}$, and *λ* is the
characteristic width of the current sheet. The conventional Harris sheet is
recovered when *F*(*x*)=1. The configuration can be further specified with a
particular *B*_{z} profile that features a minimum region along the *x* axis,
corresponding to an embedded thin current sheet (Fig. 1),
such as those often found in global MHD simulations and inferred from
satellite observations in the near-Earth magnetotail.

For a sufficiently small magnitude of the *B*_{z} minimum, the magnetotail
becomes unstable to ballooning instability, whose nonlinear development leads
to the formation of tailward receding plasmoids in the magnetotail
(Fig. 2). The magnetic reconnection process in these
simulations is no longer invariant along the equilibrium current direction,
unlike in a conventional 2-D reconnection process. For example, at a time
after the formation of plasmoids, those field lines crossing the $y=-\mathrm{90}$ line
in the *z*=0 plane encounter a totally different plasmoid structure from the
field lines crossing the $y=-\mathrm{95}$ line in the *z*=0 plane
(Fig. 3). Questions arise as to where and how a
reconnection takes place in the 3-D configuration, as well as how the global
structure of the 3-D reconnection process can be characterized and captured
in ways different from the more familiar 2-D reconnection process. Further,
it remains unclear whether this 3-D reconnection process can be reducible to
or interpretable in terms of the conventional 2-D reconnection processes.

To address these questions in this work, we for the first time apply the
concept of a quasi-separatrix layer (QSL) to the analysis of the geometry of
magnetic reconnection induced by ballooning instability in a generalized
Harris sheet that represents the magnetotail. QSL has been adopted for the
analysis of the reconnection structures involved in the solar corona for a
long time (e.g., Titov and Démoulin, 1999; Titov et al., 2002). It has also been effectively
applied to the analysis of laboratory reconnection
experiments (Lawrence and Gekelman, 2009). A QSL is a 3-D structure defined by a steep
gradient in the field-line connectivity, which is quantified by mapping field
lines across a specified volume. A surface, *S*, must first be defined to
enclose this volume. Divide *S* into two subspaces, *S*_{0} and *S*_{1}, where
*S*_{0} and *S*_{1} represent the surfaces on which field lines enter and leave
the volume, respectively. The initial footpoint is defined as
${\mathit{r}}_{\mathrm{0}}=({u}_{\mathrm{0}},{v}_{\mathrm{0}})$ in *S*_{0}. One then traces the field line from the
initial footpoint through the enclosed volume until the field line leaves the
volume through *S*_{1} at the point ${\mathit{r}}_{\mathrm{1}}=({u}_{\mathrm{1}},{v}_{\mathrm{1}})$. The Jacobian
transformation matrix and the norm of the mapping from (*u*_{0},*v*_{0}) to
(*u*_{1},*v*_{1}) are defined as

A QSL is the region where the gradient of this mapping is large compared to
the average mapping, i.e., *N*≫1.

Mathematically, the squashing degree *Q* is defined as $Q={N}^{\mathrm{2}}/\left|\mathrm{\Delta}\right|$,
where Δ is the determinant of the Jacobian
matrix (Titov et al., 2002; Priest and Démoulin, 1995). The variation of *Q* among different field
lines reflects the deformation of the magnetic flux tubes. A high squashing
degree corresponds to a large variation in the cross-sectional area of an
elemental flux tube from one footpoint to another. Quasi-separatrix layers
turn into separatrices in the limit where the
layer thickness goes to zero or the corresponding squashing degree goes to
infinity. The physical significance of QSL is that current sheets
preferentially form on these layers for reconnection.

A newly developed implementation for efficiently computing the squashing degree of magnetic field lines in any 3-D domain has been successfully applied to investigating the evolution of magnetic flux ropes in a coronal magnetic field extrapolated from a photospheric magnetic field (Liu et al., 2016). The method utilizes the field-line mappings between a cutting plane and the footpoint planes to give optimal results for mapping the squashing factor in the cutting plane. In order to avoid spurious high squashing degree structures for field lines touching the cutting plane, a new plane perpendicular to the particular field line can be introduced and switched to using the same method. We adopt this new method to recover our previous results on 2-D QSL distribution based on the calculation of bald patches. We further use the new method to find the 3-D distribution of QSLs in the entire domain.

In this section, we compute the squashing degrees and analyze the 2-D and 3-D QSL distributions of the magnetic field configuration as well as its evolution in the near-Earth magnetotail, in an attempt to understand the global geometry of the magnetic field and the 3-D nature of the magnetic reconnection process in association with the plasmoid formation process induced by ballooning instability.

## 4.1 2-D spatial distribution of QSLs in equatorial plane

We first review the development of QSLs in the equatorial plane of the
magnetotail (i.e., the *z*=0 plane) based on the computation of squashing
degrees, as shown in Fig. 4, for the same time sequence of
nonlinear ballooning development that leads to the formation of tailward
receding plasmoids in the magnetotail (Fig. 2). Similar
results on QSLs are also obtained in our previous work, where the QSLs are
identified based on the computation of bald patches (Zhu et al., 2017). Here the
QSLs are identified as the boundaries of white patches in a plane, on which
the squashing degree becomes singularly large.

In the initial and early stages of ballooning instability evolution, QSLs are
absent in the *z*=0 plane (*t*=170) (Fig. 4, upper left). By
the time *t*=180 the first set of QSLs denoted as the white enclosed regions
starts to form periodically along the *y* direction within the *z*=0 plane
around the line of *x*=9.5 (Fig. 4, upper right). As the
ballooning instability continues to evolve, a second set of QSLs starts to
form in the equatorial plane near the radially extending fronts of ballooning
fingers around *x**≲*13.5 (*t*=190) (Fig. 4, middle
left). The circular shape of each of these QSLs is smaller in radius than the
first set of QSLs. Their spatial distribution pattern is similar to the first
set of QSLs, but their locations are shifted in the *y* direction from the
first set by one half distance between two adjacent QSLs. After reaching
their maximum sizes, the first set of QSLs begins to shrink into ellipses
squeezed in the *x* direction and eventually disappears (*t* = 220–260)
(Fig. 4, middle right, lower left, and lower right). In
addition, the locations of the QSLs also evolve, particularly those of the
second set. As the ballooning finger tips extend in the positive *x*
direction, the QSLs behind each finger tip in the second set move along in
the same tail direction. Furthermore, as the first set of QSLs nearly shrinks
into disappearance, a third set of QSLs starts to emerge at *x*=11 between
the first two sets around *t*=240 (Fig. 4, lower left). This
set of QSLs later becomes dominant in size after the first set disappears and
the second set also shrinks in size. Different from the first set, the third
set of QSL circles has the same locations in the *y* direction as those in
the second set. The timings and locations of the emergence of these QSL
structures correlate well with those of the plasmoid development as shown in
Fig. 2.

Even within the 2-D equatorial plane (*z*=0), the isolated and discrete
distribution of QSLs in both the *x* and *y* directions indicates the 3-D
feature of the corresponding reconnection process. In other words, the X-line
in conventional 2-D reconnection has broken into a group of disconnected
locations of reconnections as represented by QSLs. A close examination of one
of the QSLs centered around *x*=9.5, *y*=15 and another centered around
*x*=13.5, *y*=10 at *t*=190 finds that the variation of squashing degree at
the QSL on the boundary of an isolated region is rather spiky instead of
smooth (Fig. 5). Away from the QSL, the logarithms of
squashing degree are close to zero and their variation is flat and smooth.
The QSL structures are indeed located surrounding well-isolated regions,
which are the outcome of the irreducible 3-D nature of the corresponding
reconnection process.

## 4.2 3-D spatial distribution of QSLs

We further examine the 3-D distribution of QSLs in the entire simulation
domain of the magnetotail. Not only are QSLs located in isolated regions in
the 2-D plane, but they are also localized in isolated and confined regions
in the 3-D domain (Fig. 6). As shown in
Fig. 6, the circles representing QSLs in the 2-D plane are
extended to the iso-surfaces representing QSLs in 3-D space. Such regions of
QSLs are localized along the equilibrium field line near the equatorial
plane, such as those shown in Fig. 1 (lower panel). This is
consistent with field-line structure during the nonlinear development of
ballooning instability, where the plasmoids are centered around the
equatorial plane with north–south (*z*) symmetry. The distributions of the
QSL structures are periodic along the west–east (*y*) direction
(Figs. 7 and 8), same as the QSL
distribution within the 2-D equatorial plane. The 3-D distribution of QSLs
provides a global and complete view of where the reconnection takes place.
They further confirm the irreducible 3-D nature of the corresponding
reconnection process.

Another approach to characterizing the 3-D distribution of QSLs in the
near-Earth magnetotail is to examine the squashing degree contours on various
strategically selected 2-D slices parallel or perpendicular to coordinate
axes. For example, at an earlier time *t*=190, the squashing degree
distributions in the *y*−*z* planes show two elliptically shaped QSL regions
centered around $(y,z)=(\mathrm{5},\mathrm{0})$ at *x*=9.45 and $(y,z)=(\mathrm{10},\mathrm{0})$ at *x*=13.38,
respectively, which again are represented by the white space where the
squashing degree becomes singular (Fig. 9, upper
row). In the *x*−*z* plane, the corresponding two QSL regions manifest
themselves as two round areas of singular squashing degree located around
$(x,z)=(\mathrm{9.45},\mathrm{0})$ at *y*=5 and $(x,z)=(\mathrm{13.38},\mathrm{0})$ at *y*=10
(Fig. 9, middle row). In the *x*−*y* planes with equal
distance off the equatorial plane ($z=-\mathrm{0.03}$ and *z*=0.03), the QSL regions
are similar to those within the equatorial plane shown in
Fig. 4 in both location and shape, and the QSL distributions
in those two *x*−*y* plane are symmetric with respect to *z*=0
(Fig. 9, lower row). However, those QSL regions
disappear as the *x*−*y* planes move further away from the equatorial plane,
indicating the localized nature of the 3-D reconnection regions.

The above approach also helps in visualizing the development of 3-D
distribution of QSLs over time. At a later time *t*=240, three QSL regions
appear along the *x* axis at *x*=9.25, 11.0, and 14.3, which can be first
seen from the squashing degree contours within the *y*−*z* planes
(Fig. 10, upper row). This is in contrast with the
earlier time at *t*=190, when QSLs only appear in two *y*−*z* planes along the
*x* axis (Fig. 9, upper row). At the same time, the
three QSL regions also show up in the *x*−*z* planes, individually or together,
depending on where the plane is located in the *y* direction
(Fig. 10, middle row). For example, the two QSL
regions in the *x*−*z* plane around $(x,z)=(\mathrm{11.0},\mathrm{0})$ and $(x,z)=(\mathrm{14.3},\mathrm{0})$
(Fig. 10, middle row, right panel) correspond to the
two QSL regions in the *y*−*z* plane around $(y,z)=(\mathrm{10.0},\mathrm{0})$, but one in the
*x*=11.0 plane (Fig. 10, upper row, middle panel) and
another in the *x*=14.3 plane (Fig. 10, upper row,
right panel), respectively. Furthermore, the time development of QSL 3-D
distribution can also be viewed from the variation of squashing degree
contours in the *x*−*y* planes along the *z* direction
(Fig. 10, lower row). In particular, in comparison to
the earlier time at *t*=190, the dominant QSL regions have shifted from
around $(x,y)=(\mathrm{9},\mathrm{5})$ (Fig. 9, lower row) to about
$(x,y)=(\mathrm{14.3},\mathrm{10})$ near the *z*=0 equatorial plane by the time *t*=240
(Fig. 10, lower row). Together, and over time, these
slices with different but complementary orientations comprise a complete view
of the development of the global 3-D distribution of QSLs. In comparison with
the timings and locations of the emergence of the plasmoid development shown
in Fig. 2, one can see that 3-D distribution of QSLs as well
as their evolution directly follow the plasmoid formation during the
nonlinear development of ballooning instability in both time and space. More
importantly, the 3-D QSL distribution and evolution provide a more global and
complete view of the 3-D geometry of magnetic reconnection processes induced
by the nonlinear ballooning instability in the near-Earth magnetotail.

In summary, the 3-D distribution of quasi-separatrix layers (QSLs), as well
as its evolution directly following the nonlinear development of ballooning
instability in the near-Earth magnetotail, has been thoroughly evaluated and
examined based on previous resistive MHD simulation data on the plasmoid
formation process induced by the ballooning instability. The quasi-separatrix
layers have been identified by locating the regions of high squashing degree
throughout the entire 3-D domain of the model near-Earth magnetotail in
simulation. It is found that the 3-D distribution of QSLs correlates well not
only with the 2-D-mode structures of ballooning instability within the *x*−*y*
plane, but also with the 3-D ballooning-mode structures as projected onto the
*x*−*z* and *y*−*z* planes, both spatially and temporally during the evolution of
the magnetotail configuration. Such a close correlation demonstrates a strong
coupling between the ballooning and the corresponding reconnection processes.
It also further confirms the intrinsic 3-D nature of the ballooning-induced
plasmoid formation and reconnection processes, in both geometry and dynamics.
In addition, the reconstruction of the 3-D QSL geometry may provide an
alternative means for identifying the location and timing of 3-D reconnection
sites in the magnetotail from both numerical simulations and satellite
observations.

Whereas the near-Earth magnetotail can become ballooning unstable under substorm conditions, the nonlinear evolution of ballooning instabilities, by themselves, may not always lead to the near-explosive growth. The coupling between ballooning and reconnection could be an alternative, though not the necessary, route to substorm onset. Previous studies (Pritchett and Coroniti, 1999, 2010, 2013; Zhu et al., 2004) have demonstrated the persistent presence of ballooning instabilities in generalized Harris sheet and magnetotail configurations. The models have varied from the global scales in the ideal MHD models to the meso scales of two-fluid models, and eventually to the microscopic scales of kinetic models of plasmas. Since the intrinsic 3-D nature of the reconnection process reported in this work derives from the nature of ballooning instability, the global 3-D geometry structure of the ballooning-induced reconnection process is expected to persist in the presence of two-fluid and kinetic effects, particularly on the macroscopic scales where both MHD and kinetic models should agree. The QSL is purely a geometric feature of the magnetic field configuration. Thus the QSL method only relies on the magnetic field geometry in order to identify the reconnection sites. It is independent of how the plasma is modeled, be it fluid or particle. Therefore the QSL method should be applicable for particle-in-cell simulations of reconnection caused in the course of a kinetic ballooning instability.

Although this work was in part motivated by the substorm problem in magnetospheric physics, it should not be seen as one confined only to the space plasma physics community. Rather, with our first application of QSL to the magnetotail configuration represented by the generalized Harris sheet, this work provides new insight into the ubiquitous 3-D reconnections in nature and laboratory by identifying and characterizing 3-D reconnection induced by ballooning instability.

Because the 2-D perception of magnetic reconnection has been the conventional paradigm for interpreting and understanding most phenomena and processes associated with reconnection in both natural and laboratory plasmas since the beginning, our work and results provide a dramatically different and refreshing view on one of the most fundamental processes in all plasmas. It touches the core question as to what exactly defines a reconnection or whether reconnections in two dimensions and three dimensions are qualitatively different. Different answers to such a question can lead to vastly contrasting or contradicting interpretations and conclusions. These issues would continue to be addressed in future work.

The QSL method may potentially be applied to in situ observation data analysis as well, since it is the knowledge of the magnetic field lines' connectivity itself only that is required for the calculation of QSLs. The in situ observation data from both single-point and multi-point spacecraft measurements, with additional assumptions and modeling, have been used in various reconstruction methods for the magnetic field-line geometry in the magnetotail. These include the global MHD simulations of magnetotail evolution calibrated using the in situ observation data in general (e.g., Raeder et al., 2008), the Grad–Shafranov (GS) method for two-dimensional (2-D) magnetohydrostatic structure based on the single-spacecraft data analysis technique (e.g., Hasegawa et al., 2014), and the magnetic field rotation analysis (MRA) method based on four-point measurements of the magnetic field (e.g., Shen et al., 2007). The reconstructed region of interest using these methods and in situ observation data can then be subject to the calculation of QSL. We plan on exploring such a potential application of the QSL method to in situ observation analysis in the near future.

Data used in this study are available for download at http://plasma.ustc.edu.cn/publication/19/zhu19a/data/ (last access: 12 May 2019).

PZ was responsible for providing the simulation results and the original idea, the planning, coordinating, and executing of the overall QSL analyses, as well as the writing of the entire paper.

ZW performed the QSL calculations and plotted the corresponding results.

JC provided the Fortran and IDL programs for QSL calculations.

XY converted the simulation data into the format for QSL calculations and aided in figure revisions and paper preparation.

RL was responsible for the QSL algorithm implemented in the Fortran program used in the QSL calculation and contributed to paper writing, revisions, and responses to the referees.

The authors declare that they have no conflict of interest.

The computational work used the NSF XSEDE resources provided by TACC under grant no. TG-ATM070010 and the resources of NERSC, which is supported by the DOE under contract no. DE-AC02-05CH11231.

This research has been supported by the National Natural Science Foundation of China (grant no. 41474143) and the U.S. Department of Energy (grant nos. DE-FG02-86ER53218 and DE-SC0018001).

This paper was edited by Christopher Owen and reviewed by Andrei Runov and one anonymous referee.

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