3D hard sphere Boltzmann equation: explicit
structure and the transition process from polynomial tail to Gaussian tail
Yu-Chu Lin
Yu-Chu Lin, Department of Mathematics, National Cheng Kung
University, Tainan, Taiwan
yuchu@mail.ncku.edu.tw , Haitao Wang
Haitao Wang, School of Mathematical Sciences, Institute of Natural
Sciences, MOE-LSC, IMA-Shanghai, Shanghai Jiao Tong University, Shanghai,
China
haitallica@sjtu.edu.cn and Kung-Chien Wu
Kung-Chien Wu, Department of Mathematics, National Cheng Kung
University, Tainan, Taiwan and National Center for Theoretical Sciences,
National Taiwan University, Taipei, Taiwan
kungchienwu@gmail.com
Abstract.
We study the Boltzmann equation with hard sphere in a near-equilibrium
setting. The initial data is compactly supported in the space variable and
has a polynomial tail in the microscopic velocity. We show that the solution
can be decomposed into a particle-like part (polynomial tail) and a
fluid-like part (Gaussian tail). The particle-like part decays exponentially
in both space and time, while the fluid-like part corresponds to the behavior of the compressible Navier-Stokes equation, which dominates the long time
behavior and exhibits rich wave motion. The nonlinear wave interactions in
the fluid-like part are precisely characterized and therefore we are able to distinguish the linear and nonlinear wave of the solution. It is notable that although the solution has polynomial tail in the velocity initially, the transition process from the polynomial to the Gaussian tail can be
quantitatively revealed due to the collision with the background global Maxwellian.
The Boltzmann equation is a fundamental model in the collisional kinetic
theory, which describes the evolution of a phase space distribution function
of moderately dilute gas. Precisely, the Boltzmann equation reads
(1)
where is the distribution function for particles
at time , position and microscopic velocity , and initial data is given. Here the Boltzmann collision
operator is given by
where is the relative velocity and the
post-collisional velocities satisfy
It is well known that the global Maxwellians are the steady solutions to the
Boltzmann equation. In the perturbation regime near the Maxwellian, we look
for the solution in the form of
(2)
where sufficiently small, with a perturbation function to . Here the global Maxwellian is normalized as
Substituting (2) into (1), the perturbation function
satisfies the equation
(3)
where
In fact, can be split into
with
Note that this kind of perturbation (2) allows the initial data to
have a polynomial tail in the microscopic velocity, which is different from
the standard perturbation, , where
initial data is assumed to have a Gaussian tail.
It is known that there are extensive studies on the standard perturbation,
including the global existence, time-asymptotic behavior, and even the
pointwise structure, see [7, 16, 27, 28] and
the references therein. It would be very interesting to see that can we
still obtain the precise space-time structure of the solution for initial
data with a polynomial tail?
Moreover, since the perturbation setting describes the collisions between a
small amount of released particles and the ambient particles that have
reached thermal equilibrium, the physical intuition suggests that the
distribution of the released particles will also approach thermal
equilibrium over a long period, namely, it will become close to a Gaussian
in terms of the microscopic velocity. It is a challenge problem that is it
possible to give a quantitative description of the transition process?
The main goal of this paper is to answer the above two questions.
Specifically, we will construct a pointwise estimate of solution to (3) with respect to all variables, space, time, and velocity.
The estimate not only exhibits the wave motion in space-time, but also
reveals how the solution transitions from a polynomial tail to a Gaussian
tail.
1.2. Review of previous works
Concerning the polynomial tail perturbation for collisional kinetic
equation, there has been substantial progress recently. For the torus case,
it was initiated by Gualdani-Mischler-Mouhot [17] for the
Boltzmann equation with hard sphere. It was then generalized by
[8] for Landau equation, by [1, 18] for the Boltzmann equation without angular cutoff, and by [5] for the Boltzmann equation with soft potentials. For the whole
space case, we refer to [9, 6] for the non-cutoff
Boltzmann equation and [13] for the cutoff Boltzmann equation. These works mainly focused
on global existence and large time decay of the solution, whereas our study
aim at providing a more quantitative description of the structure of the
solution.
Next, we review some space-time pointwise results closely related to the
current study. It was initiated by Liu [22] for 1D viscous
conservation laws, then developed to multi-dimensional compressible
Navier-Stokes equation [10, 12, 23, 24].
There are two key ingredients. The first is the construction of Green’s
function for the linearized system, where rich wave phenomena, such as
dissipative Huygens wave, diffusion wave, Riesz wave are identified. The
other one is the careful estimate of nonlinear wave couplings between the
above basic wave patterns. As is known, the long time behavior of the
Boltzmann equation is governed by macroscopic fluid. There are some parallel
results for Boltzmann equation with standard Gaussian tail. The result for 1D hard sphere Boltzmann
equation was constructed by Liu-Yu [25]. As
the nonlinear interaction is strong in 1D, the authors need to extract the
so called “kinetic Burger equations” to
close the nonlinear problem. Later, [26, 27] obtained the
explicit structure of Green’s function for the linearized Boltzmann equation
with hard sphere in 3D. Recently, [20] constructed the explicit
structure of the relativistic Boltzmann equation for “hard
ball”, an exponentially sharp ansatz similar to structure
in [10] was justified. In these works, the nonlinear
interactions have been estimated to the extent necessary to close the
nonlinear ansatz.
The transition from polynomial tail to Gaussian tail is related to the decay
estimates for large velocities in the Boltzmann equation. For space
homogeneous case, there are extensive studies on moments or
pointwise decay, both for polynomial and exponential weight, see [2, 3, 11, 15] and references therein. For space
inhomogeneous case, the results are relatively fewer. Generation of
polynomial moments in or pointwise sense was established under
suitable moment bound conditions for hard potential with or without cutoff,
see [4, 17, 19]. Different from the conditional
results, our result provides a dynamic process for Gaussian tail generation
in the perturbation regime.
1.3. Notations
Before stating our main results, we introduce some notations used in this
paper. We denote , . For the microscopic variable , we denote
and the weighted norms can be defined by
The inner product in will be denoted by , i.e.,
For the Boltzmann equation with hard sphere, the natural norm in is , which is defined as
For the space variable , we have similar notations, namely,
Finally, with and being two normed spaces, we
define
and for simplicity, we denote
For any two functions and , we define the space-time
convolution as
For any two real numbers and , we define .
For simplicity of notations, hereafter, we abbreviate to , where is a constant depending only on fixed numbers.
1.4. Main theorem and significant points of our results
In order to achieve our goal, we introduce the decomposition . Here corresponds to the part with only polynomial
tail, while has Gaussian tail. Heuristically, the
closer a distribution function to a Gaussian, the closer the behavior
resembles macroscopic hydrodynamics. Therefore, one may expect behaves
like particle, and behaves like fluid.
The following coupled system designed for and is to realize
one’s intuition:
(4)
with initial data
where
is the so called linearized Boltzmann collision operator,
is the nonlinear Boltzmann collision operator, and with
for a constant large enough, being the indicator
function.
It is noted that similar decomposition was also employed in [6] for Boltzmann equation without angular cutoff. Based on this
decomposition, we have the main theorem as follows:
Theorem 1.
Let be sufficiently large. Assume that is compactly supported in
the variable for all
Then for any fixed , there exists small enough such that the
solution of exists for and it can be
decomposed as , where and
satisfy with the following estimates:
For , we have
and
for some positive constant .
For , we have
for some positive constants . Here is the sound speed associated with global Maxwellian .
Several remarks on the main theorem are in order:
•
The main result is the combinations of Theorems 9, 10, and 15. In Theorem 9, we
obtain the global wave structure, which is accurate in the time-like region
but only shows polynomial decay for in the space-like region. In
Theorem 10, the estimate in space-like region is further
improved to be exponentially sharp. Theorem 15 describes
the dynamic process of transition from polynomial tail to Gaussian tail for .
•
The result shows that the polynomial tail part decays
exponentially in both space and time, while Gaussian tail part exhibits rich wave phenomena and dominates the solution at
large time. This is consistent with our intuition: the polynomial and
Gaussian tail parts are associated with particle-like and fluid-like
behaviors, respectively.
•
In the estimate of , we see that the terms consist of and orders. The order terms
represent linear waves, such as Huygens, diffusion, and Riesz waves, as
given by the Green’s function. The order terms arise from
nonlinear interactions between these basic waves. They consist of polynomial
versions of Huygens and diffusion waves, primarily concentrate inside the
acoustic wave cone. Compared to the linear waves, the nonlinear waves not
only have a order magnitude, but also decay faster by than their linear counterparts. However, previous works [10, 12, 20, 23, 24] only showed that they
have the same decay rates. Thus, our results provide a more accurate
description for the nonlinear effect, based on sharper estimates of
nonlinear wave couplings.
•
The polynomial tail of the solution is fully captured by part.
The pointwise estimate of in velocity variable thus shows how the
polynomial tail transitions to a Gaussian tail. Specifically, only
exhibits a polynomial tail initially, as time evolves it immediately
acquires an exponential tail. As time continues to evolve, the particles
with velocity will become Gaussian
tail, while the non-Gaussian part is of the order and any
moments generated by the non-Gaussian part are bounded by .
Therefore, as time tends to infinity, the distribution function will
eventually transit to a Gaussian tail; but however, the transition cannot be
completed in any finite time.
•
The assumption that the initial data has compact support in space is
unessential. It is not hard to generalize to the case where the initial data
decays polynomially in space, but in this case, the space-like behavior
should be modified accordingly. We do not pursue this, as our focus is on
the quantitative description of wave motion and the transition to a Gaussian
tail.
1.5. Ideas and strategies
We now outline the ideas and strategies for the proof of the main theorem.
1.5.1. Global wave structure
Let us begin with Theorem 9, the global wave structure of the solution. Consider the coupled system (4). Let and be the solution operators to the damped transport equation and (standard) linearized Boltzmann equation respectively, namely, solves
and solves
Then by Duhamel principle, solutions and to (4) satisfy the following coupled integral system
(5)
The essential step for constructing global wave structure is to find out the accurate ansatz for the solution.
We neglect the nonlinear effects for the time being. In the equation for , if is chosen sufficiently large, the integral operator can be regarded as a perturbation of the damped transport operator. This results in an exponential decay of in both space and time. We then substitute the estimate of into the integral equation for , requiring consideration of . The explicit structure of Green’s function is constructed in [26, 27] (we stated it in Lemma 8), showing rich wave structures, including a dissipative Huygens wave (acoustic wave described by a moving heat kernel), a diffusion wave (thermal wave described by a stationary heat kernel), a Riesz wave (related to vorticity of macroscopic fluid, described by a polynomial analogue of diffusion wave confined in the wave cone), and a space-time exponential decay term. The estimate of is given by the convolution of the Green’s function and the source term , inheriting a structure similar to that of the Green’s function (see Lemmas 19-21). This indicates that can be viewed as particle-like wave, while can be viewed as fluid-like wave.
Next, we incorporate nonlinear effects. In designing the coupled system, we intentionally placed all nonlinear terms involving in the first equation of (4), as it describes the particle-like behavior. The term is included in the second equation, as it is associated with the fluid-like behavior. The key term is , which accounts for the nonlinear wave interactions. A fundamental property is that the nonlinear operator is purely microscopic, and when acted upon by the Green’s operator, it gains an extra -order time decay. Substituting the linear estimates leads to the convolution estimates:
The main effort is to provide sharp estimates of these convolutions. Without delving into the details, we provide a heuristic explanation of the interaction process here. We illustrate this with the convolution of two Huygens waves.
where for simplicity.
The following figure is to explain the interaction process:
Figure 1. Interaction between two Huygens waves
Here, the source is plotted as a forward cone with thickness , and the propagator is plotted as a backward cone with thickness . The space is represented in 2D in the figure.
The interaction essentially occurs in the following space-time region:
Inside this region, the exponential term in Huygens wave is not effective, and the decay is mainly due to time decay factor. The key point is the sharp estimate of the volume for this space-time region. In Section 6.2, we first provide some heuristic calculations. In fact, our rigorous estimates are greatly motivated by the heuristics. We identify the strong interaction region (which appears in the regions and of Section 6) and perform very careful estimates there. The results match those obtained by the heuristic argument.
Through these sharp convolution estimates, we propose an appropriate ansatz, which is exponential decay for and polynomially sharp for as the main focus here is the region inside wave cone, where only polynomial decay can be expected. Justifying the ansatz involves even more complicated convolution estimates, but the underlying idea remains similar. Additionally, the damped transport operator is used to compensate the loss of velocity decay from the nonlinear operator in the justification for (see Lemmas 4 and 5).
Our result distinguishes between the linear and nonlinear parts of the solution, significantly improving upon previous results in [10, 12, 20, 23, 24], where the nonlinear couplings and the linear part have the same decay rate.
1.5.2. Exponential decay outside the acoustic wave cone
In Theorem 9, we obtain space-time exponential decay for , but for , we only achieve a polynomial decay estimate. This is because we designed a polynomial-type ansatz to facilitate the control of the nonlinear part of . This ansatz is accurate for the structure inside the acoustic wave cone. However, since the initial data has compact support in space and corresponds to a fluid structure that propagates at a finite speed, we expect the solution to decay exponentially outside the wave cone.
To observe the behavior of outside the cone, we multiply a suitable weight function on and prove an bound of the weighted solution through regularization and energy estimates. This approach for obtaining the space asymptotic behavior of the Boltzmann equation was developed in our previous work [21], and here it is adapted to handle .
It is worth mentioning that in our previous work, we proved exponential decay outside a wave cone for a sufficiently large . Here, through careful calculation of the micro projection, we show that indeed decays space-time exponentially outside the wave cone for any positive (see Theorem 10), where is the sound speed. This result is more consistent with physical reality.
1.5.3. The transition from polynomial tail to Gaussian tail
In the decomposition , the latter already exhibits Gaussian tail. Therefore, studying the transition process is equivalent to examining the generation of the Gaussian tail for . The mechanism for generating velocity decay comes from in the damped transport operator :
At first glance, it seems that can gain arbitrary velocity decay as time evolves. However, the upper bound for velocity decay is limited by the coupling between and , specifically by the term
in the second equation of (5). The velocity weight will ultimately be slowed down by as it decay at most as a Gaussian. We design a suitable weighted function
to capture this feature. By carefully analyzing the commutator between this weight function and the operators, we complete the description of dynamic transition process (see Theorem 15).
It is interesting to note that the mechanism for gaining velocity weight and the limitation of the maximal generation both stem from collisions with the global Maxwellian. This is entirely consistent with our physical intuition.
1.6. Organization of the paper
The rest of this paper is organized as follows: In Section 2, we
first prepare some basic properties of the integral operator ,
and present some estimates for the damped transport equation and the
linearized Boltzmann equation. In Section 3, we
construct the global wave structures of the solution, fully utilizing sharp
nonlinear wave interactions. In Section 4, we apply the
weighted energy estimate to prove that the solution indeed decays
exponentially in space-time outside the wave cone.
In Section 5, we provide a quantitative description of how
solution approaches a Gaussian tail in terms of the microscopic velocity.
Finally, we present the proof of all kinds of wave interactions in Section 6.
2. Preliminaries
To begin with, we study some essential properties of the collision frequency
, the operator and the collision
operator . It is well known that there exist two positive constants and such that
for all . In [5, Lemma 2.1 and Lemma 6.2],
the following estimates of the collision kernel have been proved.
For any , there exists a constant
depending only on such that
and
Moreover, for any ,
In order to study the first equation of (4), we introduce
the damped transport operator , that is, is the solution of the equation:
Lemma 4.
Let and . Assume that and satisfy
and
for some constants with . If
satisfies the integral equation
then
where
Proof.
Let , we have
The proof is completed.
Lemma 5.
Let and . Assume
that satisfies
If satisfies the integral equation
then
for some constant .
Proof.
The proof is similar to Lemma 4. It suffices to verify
that
Let . If , then
and thus
If , then
and so
Therefore,
∎
Lemma 6.
Let and . Assume that satisfies
If satisfies the integral equation
then
for some constant .
Proof.
The proof is similar to Lemma 4 and it suffices to
verify that
We consider two cases and .
Case 1: . We split into two parts
If , then
and thus
If , then
Therefore,
Case 2: . If , then
and thus
It implies that
If , , then
and so
If , , then
and thus
Consequently,
Combining all the discussion, there exists a constant
such that
as desired.
∎
For the second equation of decomposition (4), we list some
basic properties of the linearized Boltzmann collision operator and
nonlinear operator as below.
It is well known that the null space of
is a five-dimensional vector space, where
Let be the orthogonal projection with respect to the inner product onto , and . That is, for any ,
The solution of the wave propagation is connected to the operator for
In Theorem 9, the estimate for is exponentially sharp,
while the estimate of is only polynomially sharp. The reason is
that, to facilitate the closure of nonlinearity, we focused on the structure
inside sound wave cone, so we chose a polynomial ansatz. However, since our
initial data is compactly supported in space and represents the
fluid part with an essentially finite propagation speed. Therefore, we
expect a faster decay in the space-like region.
In this section, we will improve the behavior of outside the sound
wave cone. Indeed, we can prove that has exponential decay both in
space and time there. The result is stated as follows.
Theorem 10.
Under the same assumption of Theorem 9,
for any , if is sufficiently small, there
exists a large positive constant depending on , such that for ,
where the constant is independent of time and as .
To attain this end, we consider the weighted nonlinear equation
corresponding to . That is, let , , where the weight function is given by
and sufficiently large . Note that by
Theorem 9, decays in space and time exponentially, so
that can be controlled if is large enough, that is, there
exists such that
In view of , satisfies the
equation
After choosing large such that is small, we have
Under this situation, we are ready to estimate . Let be a
finite number. Denote
According to the wave-remainder decomposition, and
Since
we get
By finite steps of bootstrap argument, we obtain the desired estimate for . Similarly, by Lemma 11, Proposition 13, and the bootstrap
argument, we obtain estimate for
as well. We summarize the estimates for as below.
Proposition 14.
Let be large enough and let .
Then for and large , the corresponding satisfies
for some positive constants and dependent on but independent of and .
Now, we are ready to prove Theorem 10. For any fixed , we take , and consider the weight
function
with being chosen large. In view of Proposition 14,
choosing sufficiently small gives
5. The transition from polynomial tail to Gaussian tail
In this section, we study the behavior of in the microscopic
variable as increases. We provide a quantitative description of how the
velocity variable transitions from a polynomial tail to a Gaussian tail. The
result is as follows:
Theorem 15.
Let , be sufficiently large and , . Assume that satisfies the
same condition as in Theorem 9. If is
sufficiently small, then there exists a constant
only depending on such that
for all , , , where . Consequently, for any
fixed , then
and
Firstly, we need some estimate for the weight function . For simplicity, we define
(20)
with , . Now, we give an
inequality regarding the function .
Lemma 16.
Let be a
function defined by
for and . Then
for all , .
Proof.
If either or , it is trivial. By symmetry, we may assume that and so . In the following we discuss the
inequality in four cases.
Case 1: . Then
Case 2: . Then
Case 3: . Then
Case 4: . Then
As , it is a consequence of Case 1-Case 3. Gathering all the cases,
the proof is complete.
According to this lemma, we can prove the following weighted estimate
regarding and .
Lemma 17.
Let , and let be defined by . Then there exists a
constant depending only on such that
(21)
Moreover, if , we have
(22)
Proof.
Let and .
Then , , , . By change of
variables,
We split into two parts
Then
Making a change of variable by gives
If , then
If , then for and thus
Therefore,
Observe that . Hence,
the last inequality being valid due to Lemma 16. It
follows
According to the estimate in the proof of [5, Lemma 2.11], there
exists a constant depending only on such that
where is a universal constant. This completes the proof of (21).
For the estimate of (22), applying the same argument as (21), one gets
Then one can modify the argument in [5, Lemma 2.11] (in fact, it is
easier) to conclude our result.
∎
Corollary 18.
Let , and let
be defined by . Then there exists a constant depending only on such that
Moreover, for any , and , we have
Proof.
We only prove the estimate of since the estimate of is
similar. By definition of ,
We may assume that . Choosing sufficiently small such that
we obtain
Since ,
for any finite . Consequently,
for some constant depending only on ,
i.e.,
for all , , .
∎
6. Some convolution estimates
In this section, we will compute the interactions
between different wave patterns, which are essential for determining the
precise space-time structure of the solution. Although these estimates
appear complicated, there is a clear physical picture behind them (see
Section 6.2 for some illustrations). The proofs
in fact aim to translate this heuristic picture into refined convolution
estimates.
To facilitate the estimates, we decompose space-time domain into the
following regions:
6.1. Linear interaction
Lemma 19(Diffusion wave convolved with exponential decay).
for some constants and .
Lemma 20(Huygens wave convolved with exponential decay).
for some constants and .
Lemma 21(Riesz wave convolved with exponential decay).
for some constants .
The proof of Lemma 19 is easy and hence we
omit it.
Proof of Lemma 20
(Huygens wave convolved with exponential decay).
We rewrite
We discuss the integral in each domain for which belongs to.
Case 1: . Direct computation gives
Note that if , , then
for , so that
for . Consequently,
for all , where .
Case 2: .
Case 3: . We split the integral
into four parts
Note that if , then
if , then
It immediately follows that
As for ,
since . Now we
discuss two cases: (i) , and (ii) . For case (i),
which follows that
For case (ii), it is easy to see
and thus
so that
Hence,
Combining all above estimates, we have
for some constants and .
Case 4: . We split the integral into
two parts
For ,
since .
For , we decompose into two parts
If , , then
If , , then
Hence,
and
Since and for ,
and thus
which implies that
Therefore,
Combining this with and , we get the desired estimate
Case 5: . We split the integral
into three parts
It immediately follows that
and
For , we decompose into two parts
If , , then
If , , then
Hence,
Since , we have
and thus
Consequently,
Combining this with , we get the desired estimate.
∎
Proof of Lemma 21 (Riesz
wave convolved with exponential decay). .
We compute the integral for two cases: and .
Case 1: . Let . If and , then
Hence,
It immediately follows that
As for ,
since .
Now, we consider the cases: and . For , we have
so that
For , it follows that
and thus
Consequently,
Case 2: . Direct
computation gives
To sum up,
for some constants , .
∎
6.2. Nonlinear wave interaction
Lemma 22(Diffusion wave convolved with Diffusion wave).
Lemma 23(Space-time exponential decay convolved with Huygens wave).
Lemma 24(Riesz wave convolved with Huygens wave).
Lemma 25(Huygens wave convolved with Huygens wave).
Lemma 26(Huygens wave convolved with diffusion wave).
Lemma 27(Diffusion wave convolutied with Huygens wave).
We omit the proof of Lemma 22 and Lemma 23. Before we
proceed to the detailed proof of Lemmas 24-27, let us present some heuristic calculations to help
understand the mechanism of nonlinear wave interactions. We use two examples
for illustration: the convolution of two Huygens waves (Lemma 25) and convolution of diffusion wave with a Huygens wave
(Lemma 27).
We can interpret as a receiver located at that can only receive signals
along the wave cone concentrated on with thickness . Similarly, can be viewed as a sender
located at that sends signals along the wave cone concentrated on with thickness .
Figure 2. Interaction between two Huygens waves
During the interaction process, the interaction becomes strong in the
following space-time region (See Figure 2)
(27)
Inside this region, the space decay terms in the convolution are of order , and the decay is mainly from time factor. The key point is the sharp
estimate of the volume for the strong interaction region.
If , as increases from to , the receiving and
sending wave cones are almost disjoint, so the interaction is very weak.
Now we focus the case where .
The interaction process starts at and ends at (See Figure 2). To satisfy the
condition in (27), one has
Let , be the angle between and , and set . The above constraints are equivalent to
Other convolutions can be estimated heuristically in a similar manner. It
turns out that the convolutions in Lemmas 25 and 26 are the dominated ones among all the nonlinear wave
couplings.
We now begin the rigorous proofs, transforming the previous heuristic
calculations into refined (and complex) convolution estimates!
Case 1: . We split the integral into
two parts to obtain
Case 2: . We split the integral into
two parts:
First one can see
As for , we further decompose into two parts:
If ,
then we have
and thus
If
and , then
for . Hence,
whenever , and
whenever . Therefore, we get
Combining all the estimates, we have
Case 3: . We split the integral into
two parts
For , we further decompose the space domain into two parts:
If ,
then
and thus
If
and , we have
so that
since for . Therefore, we obtain
Next for , we decompose into two parts
If , we have
so
and
Therefore,
Case 4: . Observe that
We split the integral into three parts:
For , we decompose into two parts and . If and , then
Thus,
As for and , it immediately follows that
and
since .
Therefore, we have
∎
Acknowledgments:
This work is partially supported by the National Key R&D Program of China
under grant 2022YFA1007300. Y.-C. Lin is supported by the National Science
and Technology Council under the grant NSTC 112-2115-M-006-006-MY2. H.-T.
Wang is supported by NSFC under Grant No. 12371220 and 12031013, the
Strategic Priority Research Program of Chinese Academy of Sciences under
Grant No. XDA25010403. K.-C. Wu is supported by the National Science and
Technology Council under the grant NSTC 112-2628-M-006-006 -MY4 and National
Center for Theoretical Sciences.
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