-
Pressure tensor in the presence of velocity shear: Stationary
solutions and self-consistent equilibriaS. S. Cerri, F. Pegoraro,
F. Califano, D. Del Sarto, and F. Jenko Citation: Physics of
Plasmas (1994-present) 21, 112109 (2014); doi: 10.1063/1.4901570
View online: http://dx.doi.org/10.1063/1.4901570 View Table of
Contents:
http://scitation.aip.org/content/aip/journal/pop/21/11?ver=pdfcov
Published by the AIP Publishing Articles you may be interested in
Generation of coherent magnetic fields in sheared inhomogeneous
turbulence: No need for rotation? Phys. Plasmas 18, 022307 (2011);
10.1063/1.3551700 Probability distribution function for
self-organization of shear flows Phys. Plasmas 16, 052304 (2009);
10.1063/1.3132631 Nonlocal properties of gyrokinetic turbulence and
the role of E × B flow shear Phys. Plasmas 14, 072306 (2007);
10.1063/1.2750647 Self-sustaining vortex perturbations in smooth
shear flows Phys. Plasmas 13, 062304 (2006); 10.1063/1.2209229
Shear-flow driven current filamentation: Two-dimensional
magnetohydrodynamic-simulations Phys. Plasmas 7, 5159 (2000);
10.1063/1.1322558
This article is copyrighted as indicated in the article. Reuse
of AIP content is subject to the terms at:
http://scitation.aip.org/termsconditions. Downloaded to IP:
130.183.100.95 On: Tue, 07 Apr 2015 12:47:42
http://scitation.aip.org/content/aip/journal/pop?ver=pdfcovhttp://oasc12039.247realmedia.com/RealMedia/ads/click_lx.ads/www.aip.org/pt/adcenter/pdfcover_test/L-37/1071598635/x01/AIP-PT/PoF_ArticleDL_040115/PT_SubscriptionAd_1640x440.jpg/6c527a6a713149424c326b414477302f?xhttp://scitation.aip.org/search?value1=S.+S.+Cerri&option1=authorhttp://scitation.aip.org/search?value1=F.+Pegoraro&option1=authorhttp://scitation.aip.org/search?value1=F.+Califano&option1=authorhttp://scitation.aip.org/search?value1=D.+Del+Sarto&option1=authorhttp://scitation.aip.org/search?value1=F.+Jenko&option1=authorhttp://scitation.aip.org/content/aip/journal/pop?ver=pdfcovhttp://dx.doi.org/10.1063/1.4901570http://scitation.aip.org/content/aip/journal/pop/21/11?ver=pdfcovhttp://scitation.aip.org/content/aip?ver=pdfcovhttp://scitation.aip.org/content/aip/journal/pop/18/2/10.1063/1.3551700?ver=pdfcovhttp://scitation.aip.org/content/aip/journal/pop/16/5/10.1063/1.3132631?ver=pdfcovhttp://scitation.aip.org/content/aip/journal/pop/14/7/10.1063/1.2750647?ver=pdfcovhttp://scitation.aip.org/content/aip/journal/pop/13/6/10.1063/1.2209229?ver=pdfcovhttp://scitation.aip.org/content/aip/journal/pop/7/12/10.1063/1.1322558?ver=pdfcov
-
Pressure tensor in the presence of velocity shear: Stationary
solutionsand self-consistent equilibria
S. S. Cerri,1,a) F. Pegoraro,2 F. Califano,2,3 D. Del Sarto,4
and F. Jenko1,3,51Max-Planck-Institut f€ur Plasmaphysik,
Boltzmannstr. 2, D-85748 Garching, Germany2Physics Department “E.
Fermi,” University of Pisa, Largo B. Pontecorvo 3, 56127 Pisa,
Italy3Max-Planck/Princeton Center for Plasma Physics,4Institut Jean
Lamour, UMR 7198 CNRS - Universit�e de Lorraine, BP 239 F-54506
Vandoeuvre les Nancy,France5Department of Physics and Astronomy,
University of California, Los Angeles, California 90095, USA
(Received 3 October 2014; accepted 30 October 2014; published
online 13 November 2014)
Observations and numerical simulations of laboratory and space
plasmas in almost collisionless
regimes reveal anisotropic and non-gyrotropic particle
distribution functions. We investigate how
such states can persist in the presence of a sheared flow. We
focus our attention on the pressure
tensor equation in a magnetized plasma and derive analytical
self-consistent plasma equilibria
which exhibit a novel asymmetry with respect to the magnetic
field direction. These results are
relevant for investigating, within fluid models that retain the
full pressure tensor dynamics, plasma
configurations where a background shear flow is present. VC 2014
AIP Publishing LLC.[http://dx.doi.org/10.1063/1.4901570]
I. INTRODUCTION
Sheared flows are frequently observed in space and
laboratory plasmas. They are an important source of free
energy and can drive various instabilities, such as the
Kelvin-Helmholtz instability1–10 (KHI) or the magnetorota-
tional instability11–17 (MRI). The KHI, on the one hand,
leads to the formation of fully developed large scale
vortices,
eventually ending in a turbulent state where energy is effi-
ciently transferred to small scales. In this context, a
relevant
example is given by the development of the KHI observed at
the flanks of the Earth’s magnetosphere18 driven by the
velocity shear between the solar wind (SW) and the magne-
tosphere (MS) plasma, and in general, observed at other
planetary magnetospheres. On the other hand, the MRI is
considered to be a main driver of turbulence (and turbulent
transport of angular momentum) in accretion disks around
astrophysical objects, such as stars and black holes. In
addi-
tion, small-scale sheared flows can emerge from turbulent
states and lead to kinetic anisotropy effects, as seen from
SW data and simulations.19–21
The standard magnetohydrodynamic (MHD) approach
to the study of shear flow configurations is justified when
the
scale length of the sheared flow is much larger than the
typi-
cal ion microscales, i.e., when di; qi � L. However, in thecase
of the interaction of the SW with the MS, satellite
observations show that the typical scale length of the
sheared
flow is roughly comparable to the ion gyroradius and/or the
skin depth, i.e., di � qi � L ðb � 1Þ. In general, a
commonassumption in the framework of MHD modeling is to
consider an isotropic pressure tensor even in the presence
of
a background magnetic field. However, a relatively simple
step to avoid such extreme simplification is to adopt the
Chew-Goldberger-Low (CGL) approximation,22 where the
pressure tensor is gyrotropic, i.e., the pressure can be
differ-
ent along the magnetic field and perpendicular to it. In
this
approach, three main features of the system appear to be
rel-
evant: (i) the pressure is isotropic in the plane
perpendicular
to the magnetic field, i.e., gyrotropy, (ii) the system is
sym-metric with respect to the relative orientation of the
magneticfield B and the fluid vorticity Xu � r� u, i.e., with
respectto the sign of Xu � B, and (iii) the equilibrium profiles
are notdependent on the velocity shear. These three points are
substantially modified when the pressure tensor equation is
retained in the fluid hierarchy or when kinetic models are
adopted. Also retaining first-order finite Larmor radius
(FLR) corrections of the ions within a two-fluid (TF) model,
the so called extended two-fluid (eTF) model,23 was
recentlyshown to substantially modify the previous picture.
In this work, we investigate the role of retaining the full
pressure tensor equation, still in the framework of a fluid
model. In order to simplify the picture for the sake of
clarity,
we will consider a configuration in which the inhomogeneity
direction, the flow direction, and the magnetic field are
orthogonal to each other. The main result of our approach is
to prove that, in the presence of a shear flow, an
additional
anisotropy in the perpendicular plane (agyrotropy) and
anasymmetry with respect to the sign of Xu � B arise even atthe
level of the equilibrium configurations, which depend
also on the shear strength. Indeed, a sheared flow can
induce
dynamical anisotropization of an initial isotropic pressure
configuration, together with an asymmetry with respect to
the sign of Xu � B, when, for instance, one retains
first-orderFLR corrections23 or the full pressure tensor
equation.24
Here, we focus our attention on the effect of the shear-
induced anisotropization at the level of a stationary state.
Such new features are intrinsic properties of the system,
and
their relevance is related, in general, to the plasma regime
under investigation. In particular, the deviation from an
MHD/CGL model becomes not negligible when the sheara)Electronic
mail: [email protected]
1070-664X/2014/21(11)/112109/9/$30.00 VC 2014 AIP Publishing
LLC21, 112109-1
PHYSICS OF PLASMAS 21, 112109 (2014)
This article is copyrighted as indicated in the article. Reuse
of AIP content is subject to the terms at:
http://scitation.aip.org/termsconditions. Downloaded to IP:
130.183.100.95 On: Tue, 07 Apr 2015 12:47:42
http://dx.doi.org/10.1063/1.4901570http://dx.doi.org/10.1063/1.4901570http://dx.doi.org/10.1063/1.4901570mailto:[email protected]://crossmark.crossref.org/dialog/?doi=10.1063/1.4901570&domain=pdf&date_stamp=2014-11-13
-
length scale is comparable with the ion microscales
(di; qi � L), as is the case for the SW-MS interaction.
Suchdeviations, important at the level of equilibrium
configura-
tions, can dramatically affect the study of one of the above
mentioned instabilities already in the linear phase and
possi-
bly leading to very different nonlinear stages, when kinetic
models are adopted.10 This highlights the importance of a
correct modeling of the sheared flow equilibrium configura-
tion, in which the possibly relevant ingredients, such as
the
pressure tensor, are retained. Moreover, as already antici-
pated, the approach presented here can give insights into
non-gyrotropic proton distribution functions that are
observed in SW data and Vlasov simulations.19–21
The remainder of this paper is organized as follows. In
Sec. II, we solve the stationary pressure tensor equation
without heat fluxes and in the presence of a sheared flow,
giving the solution in the form of traceless corrections to
the
CGL gyrotropic pressure tensor, discussing the emergence of
the perpendicular anisotropy and of the Xu � B-asymmetry.In Sec.
III, we consider the full non-gyrotropic ion pressure
tensor within the equilibrium problem. Implicit and exact
numerical solution for the equilibrium profiles are then
given, along with possibly useful explicit analytical
approxi-
mations, underlining again the role of the asymmetry and the
perpendicular anisotropy. Finally, alternative approximated
and exact analytical equilibria are given in the Appendix.
II. STATIONARY SOLUTION OF THE PRESSURETENSOR EQUATION
Within a fluid description of a plasma, the pressure ten-
sor equation is given by23
@Pa;ij@tþ @@xk
Pa;ijua;k þ Qa;ijkð Þ þPa;ik@ua;j@xk
þPa;jk@ua;i@xk¼ qa
mac�ilmPa;jl þ �jlmPa;ilð ÞBm; (1)
where qa and ma are the charge and the mass of the speciesa,
respectively, Pa;ij is the (ij-component of the) pressuretensor,
ua;k is the (k-component of the) fluid velocity, Qa;ijk isthe
(ijk-component of the) heat flux tensor, �ijk is the Levi-Civita
symbol, and Bm is the (m-component of the) magneticfield. Now, we
look for stationary solutions of Eq. (1) in the
limit of no heat fluxes, i.e., @Pa;ij=@t ¼ 0 and Qa;ijk ¼ 0 8
i,j, and k. Under these assumptions, Eq. (1) reduces to
@
@xkPa;ijua;kð Þ þPa;ik
@ua;j@xkþPa;jk
@ua;i@xk
¼ raXa �ilmPa;jl þ �jlmPa;ilð Þbm; (2)
where we have introduced the sign of the charge ra � signðqaÞand
the cyclotron frequency Xa � jqajjBj=mac of the speciesa,
respectively, and the magnetic field versor bm � Bm=jBj.
It is a well known result that, within a FLR expansion of
Eq. (2), the zero-order solution is given by the CGL
pressure
tensor,22,23
Pð0Þa ¼ pa;?sþ pa;jjbb; (3)
where s � I� bb is the projector onto the plane perpendicu-lar
to the magnetic field (b � B=jBj), pa;jj and pa;? are thepressure
parallel and perpendicular to B, respectively. Thetensor Pð0Þa
represents the kernel of the operator on the righthand side of the
pressure tensor equation, i.e., it is an
approximated solution of the equation when the left hand
side is negligible.
We now consider a velocity shear configuration such
that the inhomogeneity direction, the flow direction, and
the magnetic field direction form a right-handed basis,
e.g.,
u ¼ uyðxÞey and B ¼ BzðxÞez. Note that this
configuration,despite its apparent simplicity, is actually commonly
used in
various areas, e.g., for studying the KHI or the MRI.
Without
loss of generality, we can write the full pressure tensor as
Pa ¼ Pð0Þa þ ~Pa, in which ~Pa represents a traceless
correc-tion to the gyrotropic pressure tensor Pð0Þa . In fact,
remainingwithin a fluid framework, one has unambiguous
definitions
of pa;? � 12 Pa : s and pa;jj � Pa : bb, so the identity ~Pa :I
¼ 0 holds.25–30 The same conclusion can be directlyderived from the
Vlasov equation.31 From the definition of
pa;jj, one obtains also ~Pa : bb ¼ 0, so in our
configuration~Pa;zz ¼ 0 and the perpendicular components of the
pressuretensor read
Pa;xx ¼ pa;? þ ~Pa;xx; Pa;yy ¼ pa;? þ ~Pa;yy with~Pa;yy ¼ �
~Pa;xx: (4)
Inserting the above expressions into Eq. (2) gives the
follow-
ing non-gyrotropic diagonal pressure tensor:
Pa;zz ¼ pa;jj
Pa;xx ¼ 1�aa xð Þ
1þ aa xð Þ
� �pa;?
Pa;yy ¼ 1þaa xð Þ
1þ aa xð Þ
� �pa;?
8>>>>>><>>>>>>:
(5)
with
aa xð Þ �1
2
s3 raXa
dua;ydx
; (6)
where s3 � signðb3Þ is the relative orientation of the mag-netic
field and the z-axis (see Ref. 23). The positivity condi-tion on
the diagonal pressure terms in Eq. (5) gives
aa xð Þ � �1
2: (7)
It is interesting to note that here an asymmetry with
respect
to the sign of aaðxÞ appears. In fact, not all the values of
theshear strength are allowed when aa is negative, while in
prin-ciple there is no limitation when it is positive. The sign of
aadepends essentially on two physical factors: the species,
through ra, and the relative orientation of the magneticfield B
and the fluid vorticity Xu, through the sign ofs3ðdua;y=dxÞ. For
instance, if one considers ions (ri ¼ þ1)and a background magnetic
field oriented in the positive
direction of the z-axis (s3 ¼ þ1), from Eq. (7) we find
thatthere is no limitation in the velocity shear of ui if the
112109-2 Cerri et al. Phys. Plasmas 21, 112109 (2014)
This article is copyrighted as indicated in the article. Reuse
of AIP content is subject to the terms at:
http://scitation.aip.org/termsconditions. Downloaded to IP:
130.183.100.95 On: Tue, 07 Apr 2015 12:47:42
-
vorticity is aligned with the magnetic field (Xu � B >
0),while the velocity shear is limited to be maximum equal (in
absolute value) to the ion gyration frequency otherwise
(jXuj Xi). We note that this condition on the shearstrength
limitation asymmetry is indeed in accordance with
Ref. 24, where it is found that shear configurations of the
type considered here become dynamically unstable when
X0=Xi � 1þ ð@xui;yÞ=Xi < 0, which corresponds exactly tothe
condition aiðxÞ < �1=2 in our notation (in the case ofRef. 24,
however, the non-stationary pressure tensor equa-
tion was considered).
The solution in Eq. (5) introduces an additional anisot-
ropy in the plane perpendicular to the magnetic field
Aa;? �jPa;xx �Pa;yyj
pa;?¼ 2 aa xð Þ
1þ aa xð Þ
��������; (8)
which gives the maximum value of the anisotropy
(AðmaxÞ? ¼ 2) for a ¼ �1=2 and for a!1. A sketch ofPxx=p?;
Pyy=p? and A? versus a is given in Fig. 1. Theasymmetry is thus
found also in the perpendicular anisot-
ropy, which is here entirely due to the velocity shear.
For small jaj � 1, the corrections to the gyrotropicCGL pressure
tensor are small and, if we expand the
solution in Eq. (5) to the leading order in a, the first-order
FLR solution is found.23,25–30 However, in this
limit, the asymmetry with respect to the sign of a inEq. (7) is
lost.
III. EQUILIBRIA WITH THE COMPLETE PRESSURETENSOR
We now want to use the stationary solution of Pxx inEq. (5) for
solving the equilibrium condition23
d
dx
Xa
Pa;xx þB2
8p
" #¼ d
dxPi;xx þ pe;? þ
B2
8p
� �¼ 0; (9)
where here we are considering only the ions full pressure
tensor, while the electrons are gyrotropic, i.e.,
Pe ¼ pe;?sþ pe;jjbb. Note that in our configuration, sincethere
are no parallel gradients, the parallel balance is auto-
matically satisfied.32 We define the gyrotropic pressure and
the magnetic field profiles as
pi;?ðxÞ ¼ pi;?0FðxÞf ðxÞ;pe;?ðxÞ ¼ pe;?0GðxÞgðxÞ;B2ðxÞ ¼
B20HðxÞhðxÞ;
8>><>>: (10)
where pi;?0 and pe;?0 are positive constants, FðxÞ; GðxÞ andHðxÞ
correspond to the MHD equilibrium and f(x), g(x), andh(x) are the
corrections to the relative MHD profile. Theequilibrium condition,
Eq. (9), can then be conveniently
rewritten in dimensionless form as
~bi;?0 1�ai xð Þ
1þ ai xð Þ
� �F xð Þf xð Þ þ ~be;?0G xð Þg xð Þ
þ H xð Þh xð Þ1þ b?0
� 1 ¼ 0; (11)
where we have fixed the constant of integration to be
B20=8pþ pi;?0 þ pe;?0 and the quantities ~ba;?0 � ba;?0=ð1þb?0Þ;
b?0 ¼
Pa ba;?0 and ba;?0 � 8ppa;?0=B20 are intro-
duced. The equation can be further simplified. First, we
note
that the MHD equilibrium functions are related by the quasi-
neutrality requirement and the MHD equilibrium conditions,
i.e., quasi-neutrality gives23
GðxÞ ¼ ½FðxÞ1þ~c ; (12)
where ~c � ðce;?=ci;?Þ � 1 and a polytropic relation betweenthe
pressure and the density is assumed,33,34 while the MHD
force balance condition gives23
HðxÞ ¼ 1þ b?0 � ½bi;?0 þ be;?0ðFðxÞÞ~c FðxÞ: (13)
Then, we require again quasi-neutrality for our modified
equilibrium, i.e.,
GðxÞgðxÞ ¼ ½FðxÞf ðxÞ1þ~c or; equivalently;gðxÞ ¼ ½f ðxÞ1þ~c ;
(14)
where the equivalence is because of condition (12). We then
require that the perpendicular plasma beta bi;?ðxÞ
remainsunchanged with respect to the MHD equilibrium (see the
Appendix for alternative requests), which then leads to the
condition
hðxÞ ¼ f ðxÞ: (15)
FIG. 1. Left: plot of the solutions
Pxx=p? (blue solid line) and Pyy=p?(red dashed line). Right:
consequent
perpendicular anisotropy A? (solidline) versus the shear
parameter a.
112109-3 Cerri et al. Phys. Plasmas 21, 112109 (2014)
This article is copyrighted as indicated in the article. Reuse
of AIP content is subject to the terms at:
http://scitation.aip.org/termsconditions. Downloaded to IP:
130.183.100.95 On: Tue, 07 Apr 2015 12:47:42
-
If ~c ¼ 0 holds, this condition is equivalent to the
requirementthat the total perpendicular plasma beta b?ðxÞ
remainsunchanged. Thus, using the previous relations, the
equilib-
rium condition (11) reads
1� ~bi;?0ai xð Þ
1þ ai xð Þ
� �F xð Þ þ ~be;?0 F xð Þð Þ1þ~c f ~c xð Þ � 1
� �� �� f xð Þ � 1 ¼ 0; ð16Þ
which is intrinsically nonlinear in f, not only because of
theparameter ~c, but also because aiðxÞ itself contains the
mag-netic field profile which must be derived self-consistently
from the equilibrium, i.e.,
ai xð Þ
¼1ffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffi
H xð Þh xð Þp s3 mi c
2 e B0
dui;ydx� a0i xð Þffiffiffiffiffiffiffiffiffi
h xð Þp ; (17)
where for convenience we have
separatedffiffiffiffiffiffiffiffiffihðxÞ
pand a0iðxÞ,
since the latter term does not depend on the self-consistent
solution h(x). This intrinsic nonlinearity is the reason
thatjustifies our approach of extending an MHD/CGL equilib-
rium to the “corresponding” full pressure tensor
equilibrium:
in the MHD/CGL case, we do not have aiðxÞ, so the equilib-rium
condition is easily solvable and we find FðxÞ; GðxÞ andHðxÞ. Then,
we can compute a0iðxÞ and give the solution interms of it.
Moreover, the MHD equilibria are the most com-
monly adopted for various simulation initialization, even in
a
kinetic framework,10 and thus using them as a starting point
may be convenient.
In the following, when we give explicit examples, a
velocity profile described by a hyperbolic tangent will be
adopted
ui;y xð Þ ¼ u0 tanhx� x0
Lu
� �; (18)
which is often used for the study of KHI,4–6 and all the
quan-
tities will be given in units of ions quantities (mi, e, Xi;
di)and Alfvèn velocity (vA).
A. Discussion of the fully self-consistent equilibria
Let us consider the complete problem in which the aiðxÞfunction
is computed with the actual self-consistent magnetic
field profile, Eq. (17). For a0i the positivity condition of
thepressure, ai � �1=2, reads
a0i xð Þ � �ffiffiffiffiffiffiffiffiffih xð Þ
p2
8 x: (19)
Then, under the assumption of quasi-neutrality and the
request that the perpendicular plasma beta bi;?ðxÞ
remainsunchanged with respect to the MHD equilibrium, Eqs. (14)
and (15), the equilibrium condition (16) can be recast in
the
following form:
~be;?0FðxÞ1þ~c f ðxÞ3=2þ~c þ ½1� ~be;?0FðxÞ1þ
~c f ðxÞ3=2
þ ~be;?0FðxÞ1þ~ca0iðxÞf ðxÞ1þ~c þ ½1� ~bi;?0FðxÞ
� ~be;?0FðxÞ1þ~c a0iðxÞf ðxÞ � f ðxÞ1=2 � a0iðxÞ ¼ 0; (20)
which is absolutely non trivial, since the parameter ~c
canchange the order of the equation in a non obvious way. We
thus restrict the problem to the case ~c ¼ 0, i.e., to the case
ofan equal polytropic law for the electrons and the ions in the
plane perpendicular to B. This assumption is
physicallyreasonable and leaves total freedom for what concerns
the
parallel polytropic laws for electrons and ions. The
equilib-
rium condition for ~c ¼ 0 readsffiffiffiffiffiffiffiffiffiffif
ðxÞ3
qþ ½1� ~bi;?0FðxÞa0iðxÞf ðxÞ �
ffiffiffiffiffiffiffiffif ðxÞ
p� a0iðxÞ ¼ 0;
(21)
which can be interpreted as a cubic equation for wðxÞ
�ffiffiffiffiffiffiffiffif ðxÞ
p(f(x) cannot be negative since it is related to the pres-
sure—see Eq. (10)). In order to gain some insights from
Eq. (21), we can solve it for a0iðf Þ, i.e.,
a0i fð Þ ¼ffiffiffiffif 3
p�
ffiffiffifp
1� 1� ~bi;?0F xð Þh i
f; (22)
together with the condition in Eq. (19), which in our case,
hðxÞ ¼ f ðxÞ, becomes
a0i fð Þ � �ffiffiffifp
2: (23)
The implicit solution a0iðf Þ is shown in Fig. 2 for the case
ofF ¼ H ¼ 1 and jB0j ¼ 1, with different values of ~bi;?0
andvelocity shear strength, assuming a hyperbolic tangent
profile of the type in Eq. (18) with Lu¼ 3. Three cases
areshown: bi;?0 ¼ be;?0 ¼ 0:1 and u0 ¼ 2=3 (left panel),bi;?0 ¼
be;?0 ¼ 1 and u0 ¼ 2=3 (center), and bi;?0 ¼ be;?0 ¼2 and u0 ¼ 1:5
(right panel). The red continuous line repre-sents the positivity
condition border set by Eq. (23), i.e.,
a0i ¼ �ffiffiffifp
=2, and only solutions above that curve are physi-cal. The red
dashed lines represent instead the maximum
value of a0iðxÞ for the chosen velocity profile.From Fig. 2
several interesting features emerge: (i) the
parameter ~bi;?0F (here F ¼ 1) essentially determines how“fast”
the solution f deviates from unity when a0i deviatesfrom zero, (ii)
the strength of the velocity shear, i.e., the
parameter u0=B0Lu, determines how far from gyrotropy thesystem
is allowed to go, (iii) the presence of an asymmetry
with respect to the sign of a0i (due to the plot scale, this
ismore evident in the right panel, but it is true in general),
and
(iv) the existence of a second real solution for a0i 0 andnot
for a0i > 0, which is however unphysical (i.e., below
thepositivity border - see below). The above plots allow us to
represent solutions in implicit form. Considering a hyper-
bolic tangent velocity shear profile as in Eq. (18) and H ¼
1,the function a0iðxÞ reads
a0i xð Þ ¼s32
u0B0Lu
cosh�2 x=Luð Þ; (24)
where we took x0 ¼ 0 for simplicity. We consider the caseshown
in the central panel of Fig. 2 for a0iðf Þ. This plot ofa0i versus
f, zoomed in the region around a0i ¼ 0 and f¼ 1,is reproduced in
the right panel of Fig. 3. In the left panel of
112109-4 Cerri et al. Phys. Plasmas 21, 112109 (2014)
This article is copyrighted as indicated in the article. Reuse
of AIP content is subject to the terms at:
http://scitation.aip.org/termsconditions. Downloaded to IP:
130.183.100.95 On: Tue, 07 Apr 2015 12:47:42
-
Fig. 3, we show the plot of a0iðxÞ in Eq. (24), for both signsof
s3. The aim is to visualize how f(x) should look by draw-ing a0iðxÞ
and a0iðf Þ next to each other, with the values of a0ion the y-axis
of both plots (and with the same scale), so onecan go back and
forth from one plot to the other in three
steps: go along the x-axis of left panel of Fig. 3 (x
coordi-nate), (ii) look at the value that a0iðxÞ takes in the left
paneland then move to the same level of right panel (in both
pan-
els, the y-axis has the same scale and the values of a0i
arerepresented on it) and (iii) after reaching the curve a0iðf Þ
onthe right panel in the point that corresponds to the value of
a0i found at point (ii), go down to the x-axis of the rightpanel
in order to find the value of f that corresponds to thevalue of x
at point (i).
Imagine going along the whole x-axis, from �1 toþ1. For
sufficiently large jxj, we have a0i ¼ 0, so the solu-tion is
asymptotically f¼ 1 (e.g., for jxj� 4 in left panel ofFig. 3).
Then, still referring to Fig. 3, as we approach x¼ 0from negative
values a0i starts to deviate from zero (leftpanel) and thus also
f(x) starts to deviate from unity (rightpanel), becoming bigger or
smaller if a0i becomes positive ornegative, respectively. In
passing through x¼ 0 (left panel),we pass through the global
maximum (minimum) of the pos-
itively (negatively) valued a0i, corresponding to the maxi-mum
deviation of f(x) from unity in the right panel (i.e., inthe point
where the curve a0iðf Þ intercepts the horizontal reddashed line,
above f¼ 1 or below it accordingly with thesign of a0i). Then,
leaving x¼ 0 behind and proceeding toincreasing positive x-values
in the left panel of Fig. 3, a0istarts to decrease (increase) and
so does f(x) in the right
panel, until it comes back to unity for sufficiently high
x-val-ues (note that for x> 0 we are going on the curve a0iðf Þ
allthe way back compared to how it had been covered for x< 0,the
point x¼ 0 being the turning point).
Explicit numerical solutions f(x) of Eq. (21) for a0iðxÞgiven in
Eq. (24) are plotted in Fig. 4 for the three cases in
Fig. 2. The corresponding profiles PxxðxÞ (s3 ¼ þ1: bottomblue
solid line and s3 ¼ �1: top blue dashed line) andPyyðxÞ (s3 ¼ þ1:
top red solid line and s3 ¼ �1: bottom reddashed line) are also
given (from Eqs. (33) and (34)—see
below). The asymmetry with respect to the sign of Xu � B ismore
evident on the right panel due to the choice of the pa-
rameters, but it is present in all cases.
In order to trace back the origin of the double solution
for a0i 0 and to show that one of the two solutions isunphysical
because of the positivity condition in Eq. (23),
we consider the equilibrium condition, Eq. (21), and look
for
solutions which deviate from gyrotropy weakly. For this pur-
pose, we treat ~bi;?0 as a small parameter (here, we considerthe
case F ¼ 1, but the bound 0 F 1 always holds). For~bi;?0 ¼ 0, Eq.
(21) is exactly solvable
ðf ðxÞ � 1Þðffiffiffiffiffiffiffiffif ðxÞ
pþ a0iðxÞÞ ¼ 0; (25)
and admits two real roots
f0ðxÞ ¼ 1 8 x~f 0ðxÞ ¼ a20iðxÞ 8 x 2 fxja0iðxÞ 0g;
((26)
where f0 ¼ 1 means gyrotropy, while ~f 0 represents the~bi;?0 !
0 limit of the second solution in Fig. 2 for a0i 0.
FIG. 2. Plot of the implicit solution a0iðf Þ in Eq. (22) for
different plasma parameters: bi;?0 ¼ be;?0 ¼ 0:1 and u0 ¼ 2=3
(left), bi;?0 ¼ be;?0 ¼ 1 and u0 ¼ 2=3(center), bi;?0 ¼ be;?0 ¼ 2
and u0 ¼ 1:5 (right). The other parameters are F ¼ H ¼ 1; jB0j ¼ 1,
Lu¼ 3 for all cases. Red continuous line represents the borderabove
which the pressure is positive, Eq. (23). Red dashed lines
represent the bounds of a0i values (for both s3 ¼ þ1 and s3 ¼ �1),
while the dotted anddashed-dotted lines are the reference for f¼ 1
and a0i ¼ 0, respectively.
FIG. 3. Left: plot of a0iðxÞ in Eq. (24)for both sign of s3 (see
inset). Right:zoom around f¼ 1 and a0i ¼ 0 of thecenter plot in
Fig. 2.
112109-5 Cerri et al. Phys. Plasmas 21, 112109 (2014)
This article is copyrighted as indicated in the article. Reuse
of AIP content is subject to the terms at:
http://scitation.aip.org/termsconditions. Downloaded to IP:
130.183.100.95 On: Tue, 07 Apr 2015 12:47:42
-
However, ~f 0 is below the positivity condition ai � �1=2 (forf
! ~f 0 we obtain ai ! �1). Keeping the first order in~bi;?0F � 1
for the physical solution near unity leads to
f xð Þ ’ 1þ ~bi;?0F xð Þa0i xð Þ
1þ a0i xð Þ; (27)
which corresponds to the first-order Taylor expansion for
small C0a0i=ð1þ a0iÞ of the solution in Eq. (30) (see
below).This means that, at least in the limit of small-~bi;?0, the
twosolutions are close to each other. Note that the
small-~bi;?0limit does not necessarily mean small-bi;?0, but it can
bereached also in the large perpendicular temperature ratio,
s? ¼ Te;?0=Ti;?0 � 1. Finally, physical solutions of Eq.
(21)only exist within restricted domains of (~bi;?0; a0i). In
partic-ular, this turns out to be the case only when a0i is
negative,i.e., for Xu � B < 0. An example of this asymmetric
behavioris given in Fig. 5, where we show that solutions for a0i
< 0may disappear because of the positivity constraint
depending
on the value of ~bi;?0. For a0i > 0, i.e., for Xu � B > 0,
a
solution is instead always present, regardless of the value
of~bi;?0.
B. Approximate analytical solution of the
equilibriumcondition
In the limit of small corrections to the MHD equilib-
rium, we can give analytical solutions for f(x) with ~c 6¼ 0.
Inthis limit, the ion cyclotron frequency Xi in the ai functioncan
be computed with the MHD profile of the magnetic field,
jBðxÞj ’ B0ffiffiffiffiffiffiffiffiffiffiHðxÞ
p, i.e.,
ai xð Þ ’ a0i xð Þ ¼s3
2B0ffiffiffiffiffiffiffiffiffiffiffiH xð Þ
p dui;ydx
; (28)
which is an approximation that one should check a poste-
riori (see the Appendix for a simple case in which this
case is exact), and leads to the following equilibrium
condition:
FIG. 4. Top row: plot of the explicit numerical solution f(x) of
Eq. (21). Bottom row: corresponding Pxx and Pyy profiles (see in
the text). The three casesabove correspond to the three cases in
Fig. 2: bi;?0 ¼ be;?0 ¼ 0:1 and u0 ¼ 2=3 (left), bi;?0 ¼ be;?0 ¼ 1
and u0 ¼ 2=3 (center), bi;?0 ¼ be;?0 ¼ 2 and u0 ¼ 1:5(right).
FIG. 5. Plot of the implicit solution
a0iðf Þ for the case bi;?0 ¼ be;?0 ¼ 5(left) and for the case
bi;?0 ¼ 10;be;?0 ¼ 1 (right), corresponding to~b i;?0 ¼ 5=11 and
5/6, respectively.The other parameters are F ¼ H ¼ 1;u0 ¼ 2:45;
jB0j ¼ 1, Lu¼ 3 for bothcases.
112109-6 Cerri et al. Phys. Plasmas 21, 112109 (2014)
This article is copyrighted as indicated in the article. Reuse
of AIP content is subject to the terms at:
http://scitation.aip.org/termsconditions. Downloaded to IP:
130.183.100.95 On: Tue, 07 Apr 2015 12:47:42
-
1� ~bi;?0F xð Þa0i xð Þ
1þ a0i xð Þ
�
þ~be;?0 F xð Þð Þ1þ~c f ~c xð Þ � 1� �i
f xð Þ ¼ 1: (29)
Treating ~c as a small parameter, we solve the above
equilib-rium problem iteratively. The solution of Eq. (29) for ~c ¼
0is straightforward, i.e.,
f0 xð Þ ¼ 1� C0 xð Þa0i xð Þ
1þ a0i xð Þ
� ��1; (30)
where C0ðxÞ ¼ ~bi;?0FðxÞ. Noting that Eq. (29) is equivalentto
the equilibrium condition Eq. (23) in Ref. 23, with the
substitution
~u0 xð Þ ! a0i xð Þ1þ a0i xð Þ
;
we can derive the iterative solution (cf. Eqs.(24)–(26) in
Ref. 23), i.e.,
f xð Þ ¼ 1� C xð Þ a0i xð Þ1þ a0i xð Þ
� ��1; (31)
with
CðxÞ ¼ ½1þ ~c~be;?0ðFðxÞÞ1þ~c �1C0ðxÞ: (32)
In the above, we have assumed that j~c~be;?0ðFðxÞÞ1þ~c j <
18x
for the convergence of the resulting series, which can be
shown to be always the case (see Ref. 23). Moreover, the
solution passes through a Taylor expansion in which we
consistently assume that the correction to the MHD profile
is
small, i.e., jCa0i=ð1þ a0iÞj � 1. In this regard, the
relationja0i=ð1þ a0iÞj 1 8 a0i � �1=2 holds, ~bi;?0 < 1 by
defini-tion and we can always choose pi;?0 such that FðxÞ <
18x.Thus, the condition jCa0i=ð1þ a0iÞj � 1 is valid for most ofthe
parameter range commonly adopted. Finally, the solution
in Eq. (31) reduces to the first-order FLR solution given in
Ref. 23 if we retain only the first order in a0i inside the
squarebrackets.
1. Explicit equilibrium profiles
We give also the explicit equilibrium profiles of the
physical quantity of interest, for the sake of clarity
Pi;xx ¼ pi;?0 1�ai xð Þ
1þ ai xð Þ
� �F xð Þf xð Þ; (33)
Pi;yy ¼ pi;?0 1þai xð Þ
1þ ai xð Þ
� �F xð Þf xð Þ; (34)
Pi;zz � pi;jj ¼ pi;jj0ðFðxÞf ðxÞÞci;jj=ci;? ; (35)
nðxÞ ¼ n0ðFðxÞf ðxÞÞ1=ci;? ; (36)
Pe;xx ¼ Pe;yy � pe;? ¼ pe;?0ðFðxÞf ðxÞÞ1þ~c ; (37)
Pe;zz � pe;jj ¼ pe;jj0ðFðxÞf ðxÞÞce;jj=ci;? ; (38)
BzðxÞ ¼
B0ffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiffiHðxÞf
ðxÞ
p: (39)
If the parallel and perpendicular temperatures are of
interest,32
instead of the corresponding pressures, from Eqs. (33)–(36)
we have
Ti;? �1
n
Pi;yy þPi;yy2
¼ Ti;?0 F xð Þf xð Þð Þci;?�1ci;? ; (40)
Ti;jj �pi;jjn¼ Ti;jj0 F xð Þf xð Þð Þ
ci;jj�1ci;? ; (41)
Te;? �pe;?
n¼ Ti;?0 F xð Þf xð Þð Þ
ce;?�1ci;? ; (42)
Te;jj �pe;jjn¼ Ti;jj0 F xð Þf xð Þð Þ
ce;jj�1ci;? : (43)
We define the MHD profiles with the superscript (0), e.g.,
Tð0Þi;? � Ti;?0FðxÞ
ðci;?�1Þ=ci;? , and the overlined quantities asthe ratio between
the actual and the MHD profiles, e.g.,�T i;? � Ti;?=Tð0Þi;?. Note
that taking the perpendicular andparallel polytropic indices to be
c? ¼ 2 and cjj ¼ 1 for bothspecies, one obtains
�T jj ¼ 1; (44)
�T? ¼ �n ¼ �B; (45)
which mean �pjj �B2=�n3 ¼ const: and �p?=�n �B ¼ const:.
Thus,
if the initial MHD profiles are such that pð0Þjj ðBð0ÞÞ
2=ðnð0ÞÞ3 ¼const: and p
ð0Þ? =n
ð0ÞBð0Þ ¼ const: (as, e.g., for the caseF ¼ H ¼ 1), then also
pjjB2=n3 ¼ const: and p?=nB¼ const:, as expected from the double
adiabatic laws.22
Finally, in order to visualize the asymmetry due to the
sign of Xu � B, we plot the equilibrium profiles for a
givencase. In Fig. 6, we show the velocity shear ui;yðxÞ andthe
function CðxÞa0iðxÞ=½1þ a0iðxÞ (left panel) and the cor-responding
equilibrium profiles for Pi;xx and Pi;yy (rightpanel).
The parameters used for the profiles in Fig. 6 are
u0 ¼ 2=3, Lu¼ 3, B0 ¼ 61 (s3 ¼ 61), bi;?0 ¼ be;?0 ¼ 1;and ~c ¼
0. For the sake of clarity, we have chosen the sim-plest MHD case
of F ¼ G ¼ H ¼ 1. By an inspection of theplot, some considerations
emerge. First, while the condition
jCðxÞa0iðxÞ=½1þ a0iðxÞj � 1 holds, as assumed in thederivation
on the profiles, the effects on the anisotropy
are actually big (�20%� 30%). The same considerationremains true
even for more extreme cases. Second, the asym-
metry between the two cases s3 ¼ 61 is impressive, evenfor this
moderate case: the two set of profiles are remarkably
different, while the value of ai, which gives us an idea ofhow
far from gyrotropy (a0i ¼ 0) the system is, only reachesa0i ’ 0:11
(a0i ’ �0:11) for the configuration with s3 ¼ þ1(s3 ¼ �1). The
fundamental difference between the two con-figurations, s3 ¼ 61,
may then lead to very different dynam-ical evolution of the system
and thus of the instability under
study already in the linear phase.1,2,10 In Fig. 7, we show
the
same quantities as in Fig. 6 for a different set of
parameters:
F ¼ G ¼ H ¼ 1; u0 ¼ 3=2, Lu¼ 3, B0 ¼ 61 (s3 ¼ 61),
112109-7 Cerri et al. Phys. Plasmas 21, 112109 (2014)
This article is copyrighted as indicated in the article. Reuse
of AIP content is subject to the terms at:
http://scitation.aip.org/termsconditions. Downloaded to IP:
130.183.100.95 On: Tue, 07 Apr 2015 12:47:42
-
bi;?0 ¼ be;?0 ¼ 2; and ~c ¼ 0, which correspond toa0i ’
60:25.
IV. CONCLUSIONS AND DISCUSSION
We have presented a study of the role of the pressure
tensor in the presence of a sheared velocity field within a
fluid plasma framework. The heat fluxes are neglected.
Solutions of the stationary pressure tensor equation are
given
for a simple, but commonly adopted configuration, and the
properties of such equilibrium solutions are discussed. In
particular, we have shown that, in addition to the well
known
parallel-perpendicular anisotropy (pjj 6¼ p?), the system isalso
anisotropic in the plane perpendicular to the magnetic
field, i.e., Pxx 6¼ Pyy 6¼ Pzz. The magnitude of the
perpen-dicular anisotropy turns out to depend on the strength of
the
velocity shear and on its scale length of variation.
Moreover,
the system is strongly asymmetric with respect to the
relative
orientation of the background magnetic field and of the
fluid
vorticity, i.e., with respect to the sign of Xu � B. These
prop-erties of the system are present even at the level of the
equi-
librium state representing the starting point for the study
of
shear-flow instabilities.
A method for deriving equilibrium profiles is presented
and both numerical and approximated analytical solutions
are provided for some representative cases. The profiles
derived in the present paper are shown to be different with
respect to the usual MHD or even CGL equilibria. In particu-
lar, they depend on the velocity shear and are asymmetric
with respect to the sign of Xu � B. These features, arising
al-ready at the level of the equilibrium configuration, turn
out
to be relevant when fluid models that retain the pressure
tensor equation and/or kinetic models are adopted, as for
the
study of the KHI and the MRI.
Finally, despite the relative simplicity of the system con-
figuration adopted, it seems plausible that our results can
be
used for the interpretation of satellite data where non-
gyrotropic distribution functions are observed. This could
be
the case, for instance, of solar wind data, since, as
pointed
out by recent studies, one expects that the turbulence
sponta-
neously generates local velocity shear flows.
ACKNOWLEDGMENTS
The research leading to these results received funding
from the European Research Council under the European
Unions Sevenths Framework Programme (FP7/2007-2013)/
ERC Grant Agreement No. 277870. The research leading to
these results has received funding from the European
Commission’s Seventh Framework Programme (FP7/2007-
2013) under the Grant Agreement SWIFF (Project No.
263340, www.swiff.eu).
APPENDIX: ALTERNATIVE ANALYTICAL EQUILIBRIA
A relevant feature of Eq. (11) is that it is general and
versatile. Depending on the physical requirements, whichthen
translate into mathematical relations between f, g, andh, one can
compute very different equilibrium profiles. In thefollowing, we
give some examples.
1. Preserving the total perpendicular plasma beta
Requiring that the total perpendicular plasma beta b?ðxÞremains
unchanged in passing from MHD to full pressure
tensor equilibria, the relation in Eq. (15) is substituted
by
FIG. 6. Left: velocity profile ui;yðxÞ(blue solid line) and the
function
CðxÞaiðxÞ=½1þ aiðxÞ (red dashed line).Right: plot of the
approximated equi-
librium profiles Pi;xxðxÞ (s3 ¼ þ1: bot-tom blue solid line, s3
¼ �1: top bluedashed line) and Pi;yyðxÞ (s3 ¼ þ1: topred solid
line, s3 ¼ �1: bottom reddashed line). Here, the parameters
are:
F ¼ G ¼ H ¼ 1; u0 ¼ 2=3, Lu¼ 3,B0 ¼ 61 (s3 ¼ 61), bi;?0 ¼ be;?0
¼ 1and ~c ¼ 0.
FIG. 7. Left: velocity profile ui;yðxÞ(blue solid line) and the
function
CðxÞaiðxÞ=½1þ aiðxÞ (red dashed line).Right: plot of the
approximated equi-
librium profiles Pi;xxðxÞ (s3 ¼ þ1: bot-tom blue solid line, s3
¼ �1: top bluedashed line) and Pi;yyðxÞ (s3 ¼ þ1: topred solid
line, s3 ¼ �1: bottom reddashed line). Here, the parameters
are:
F ¼ G ¼ H ¼ 1; u0 ¼ 3=2, Lu¼ 3,B0 ¼ 61 (s3 ¼ 61), bi;?0 ¼ be;?0
¼ 2and ~c ¼ 0.
112109-8 Cerri et al. Phys. Plasmas 21, 112109 (2014)
This article is copyrighted as indicated in the article. Reuse
of AIP content is subject to the terms at:
http://scitation.aip.org/termsconditions. Downloaded to IP:
130.183.100.95 On: Tue, 07 Apr 2015 12:47:42
www.swiff.eu
-
hðxÞ ¼ n~cðF ; f ; xÞf ðxÞ; (A1)
where the function
n~c F ; f ; xð Þ �bi;?0 þ be;?0 F xð Þf xð Þð Þ~c
bi;?0 þ be;?0 F xð Þð Þ~c; (A2)
has been defined, such that it reduces to n0ðF ; f ; xÞ ¼ 1
for~c ¼ 0. For ~c ¼ 0 we indeed recover Eq. (15) and thus
theequilibrium condition in Eq. (16) and its solution. For ~c 6¼
0,the equilibrium condition reads
n~c F ; f ; xð Þ þ ~bi;?01� n~c F ; f ; xð Þ 1þ a0i xð Þð Þ
1þ a0i xð Þ
" #F xð Þ
(
þ ~be;?0 F xð Þð Þ1þ~c f ~c xð Þ � n~c F ; f ; xð Þ
�)
f xð Þ ¼ 1; (A3)
which, Taylor expanding f ~c and n~c as in Sec. III B and
aftersome algebra, admits the solution
f xð Þ ¼ 1� C xð Þ ai xð Þ1þ ai xð Þ
� ��1; (A4a)
CðxÞ ¼ ½1þ ~c~be;?0 ~F~cðxÞ�1C0ðxÞ; (A4b)
~F~c xð Þ � F xð Þð Þ~c
~bi;?0 þ ~be;?0 F xð Þð Þ~c: (A4c)
2. Preserving the magnetic field configuration
We may want to fix the magnetic field configuration:
this is equivalent to requiring that the magnetic field
profile
remains unchanged with respect to the MHD profile, i.e.,
h xð Þ¼ 1; H xð Þ1þb?0
¼ 1� ~bi;?0þ ~be;?0 F xð Þð Þ~ch i
F xð Þ; (A5)
and thus we need to solve the following equilibrium
condition:
~bi;?0 1�ai xð Þ
1þ ai xð Þ
� �þ ~be;?0F~c xð Þf ~c xð Þ
� �f xð Þ
¼ ~bi;?0 þ ~be;?0F~c xð Þ; (A6)
which, considering the case ~c ¼ 0 for simplicity, has
thesolution
f0 xð Þ ¼1þ s?
1þ s? � a0i xð ÞffiffiffiffiffiffiffiffiH xð Þp þa0i xð Þ;
(A7)
where we have defined the perpendicular temperature ratio
s? � Te;?0=Ti;?0 for brevity and now the function aiðxÞ
iscomputed with the actual local magnetic field, without
approximations (i.e., aiðxÞ � a0iðxÞ).
1H. Nagano, Planet. Space Sci. 27, 881 (1979).2J. D. Huba,
Geophys. Res. Lett. 23, 2907, doi:10.1029/96GL02767 (1996).3A.
Miura, Phys. Plasmas 4, 2871 (1997).4M. Faganello, F. Califano, and
F. Pegoraro, Phys. Rev. Lett. 100, 015001(2008).
5F. Califano, M. Faganello, F. Pegoraro, and F. Valentini,
Nonlinear
Processes Geophys. 16, 1 (2009).6M. Faganello, F. Califano, and
F. Pegoraro, New J. Phys. 11, 063008(2009).
7T. K. M. Nakamura, H. Hasegawa, and I. Shinohara, Phys. Plasmas
17,042119 (2010).
8T. K. M. Nakamura, H. Hasegawa, I. Shinohara, and M.
Fujimoto,
J. Geophys. Res. 116, A03227, doi:10.1029/2010JA016046
(2011).9F. Palermo, M. Faganello, F. Califano, F. Pegoraro, and O.
Le Contel,
J. Geophys. Res. 116, A04223, doi:10.1029/2010JA016400
(2011).10P. Henri, S. S. Cerri, F. Califano, F. Pegoraro, C. Rossi,
M. Faganello, O.
Sebek, P. Travnicek, P. Hellinger, J. T. Frederiksen, A.
Nordlund, S.
Markidis, R. Keppens, and G. Lapenta, Phys. Plasmas 20, 102118
(2013).11E. P. Velikhov, J. Exp. Theor. Phys. (USSR) 36, 1398
(1959); available at
http://www.aip.de/groups/MHD/news/velikhov.pdf.12S.
Chandrasekhar, Proc. Natl. Acad. Sci. U.S.A. 46, 253 (1960).13P.
Sharma, G. Hammett, E. Quataert, and J. M. Stone, Astrophys. J.
637,
952 (2006).14N. M. Ferraro, Astrophys. J. 662, 512 (2007).15H.
Ren, J. Cao, Z. Wu, and P. K. Chu, Plasma Phys. Control. Fusion
53,
065021 (2011).16M. A. Riquelme, E. Quataert, P. Sharma, and A.
Spitkovsky, Astrophys. J.
755, 50 (2012).17K. Shirakawa and M. Hoshino, Phys. Plasmas 21,
052903 (2014).18H. Hasegawa, M. Fujimoto, T.-D. Phan, H. R�eme, A.
Balogh, M. W.
Dunlop, C. Hashimoto, and R. TanDokoro, Nature 430, 755
(2004).19S. Servidio, F. Valentini, F. Califano, and P. Veltri,
Phys. Rev. Lett. 108,
045001 (2012).20S. Servidio, K. T. Osman, F. Valentini, D.
Perrone, F. Califano, S.
Chapman, W. H. Matthaeus, and P. Veltri, Astrophys. J. Lett.
781, L27(2014).
21F. Valentini, S. Servidio, D. Perrone, F. Califano, W. H.
Matthaeus, and P.
Veltri, Phys. Plasmas 21, 082307 (2014).22G. F. Chew, M. L.
Goldberger, and F. E. Low, Proc. R. Soc. A 236, 112
(1956).23S. S. Cerri, P. Henri, F. Califano, D. Del Sarto, M.
Faganello, and F.
Pegoraro, Phys. Plasmas 20, 112112 (2013).24D. Del Sarto, F.
Pegoraro, and F. Califano, “Pressure anisotropy and small
spatial scales induced by a velocity shear” (unpublished).25M.
N. Rosenbluth and A. Simon, Phys. Fluids 8, 1300 (1965).26A.
Macmahon, Phys. Fluids 8, 1840 (1965).27J. J. Ramos, Phys. Plasmas
12, 052102 (2005).28P. Goswami, T. Passot, and P. L. Sulem, Phys.
Plasmas 12, 102109
(2005).29T. Passot and P. L. Sulem, Phys. Plasmas 14, 082502
(2007).30P. L. Sulem and T. Passot, “Landau fluid closures with
nonlinear large-
scale finite Larmor radius corrections for collisionless
plasmas,” J. Plasma
Phys. (published online 2014).31A. A. Schekochihin, S. C.
Cowley, F. Rincon, and M. S. Rosin, Mon. Not.
R. Astron. Soc. 405, 291 (2010).32T. Passot, V. Ruban, and P. L.
Sulem, Phys. Plasmas 13, 102310 (2006).33Note that, without heat
flux, one could argue that a natural closure should
be provided by the double adiabatic laws22 (see also Ref. 34 for
a more
convenient formulation). However, in the present case where heat
flux is
neglected and no parallel gradients are present, the double
adiabatic clo-
sures are actually equivalent to two different perpendicular and
parallel
polytropic relations with c? ¼ 2 and cjj ¼ 1. In fact, a
polytropic law ofthe type dðPn�CÞ=dt ¼ 0 can be rewritten, using
continuity equationdn=dt ¼ �nr � u, as dP=dt ¼ �CPr � u. The
previous relation is equiva-lent to Eq. (17) in Ref. 34 with C¼ 2
for p? and C¼ 1 for pjj, if heat fluxand parallel gradients are
neglected: dp?=dt ¼ �2p?r � u anddpjj=dt ¼ �pjjr � u.
34T. Chust and G. Belmont, Phys. Plasmas 13, 012506 (2006).
112109-9 Cerri et al. Phys. Plasmas 21, 112109 (2014)
This article is copyrighted as indicated in the article. Reuse
of AIP content is subject to the terms at:
http://scitation.aip.org/termsconditions. Downloaded to IP:
130.183.100.95 On: Tue, 07 Apr 2015 12:47:42
http://dx.doi.org/10.1016/0032-0633(79)90013-8http://dx.doi.org/10.1029/96GL02767http://dx.doi.org/10.1063/1.872419http://dx.doi.org/10.1103/PhysRevLett.100.015001http://dx.doi.org/10.5194/npg-16-1-2009http://dx.doi.org/10.5194/npg-16-1-2009http://dx.doi.org/10.1088/1367-2630/11/6/063008http://dx.doi.org/10.1063/1.3385445http://dx.doi.org/10.1029/2010JA016046http://dx.doi.org/10.1029/2010JA016400http://dx.doi.org/10.1063/1.4826214http://www.aip.de/groups/MHD/news/velikhov.pdfhttp://dx.doi.org/10.1073/pnas.46.2.253http://dx.doi.org/10.1086/498405http://dx.doi.org/10.1086/517877http://dx.doi.org/10.1088/0741-3335/53/6/065021http://dx.doi.org/10.1088/0004-637X/755/1/50http://dx.doi.org/10.1063/1.4875739http://dx.doi.org/10.1038/nature02799http://dx.doi.org/10.1103/PhysRevLett.108.045001http://dx.doi.org/10.1088/2041-8205/781/2/L27http://dx.doi.org/10.1063/1.4893301http://dx.doi.org/10.1098/rspa.1956.0116http://dx.doi.org/10.1063/1.4828981http://dx.doi.org/10.1063/1.1761402http://dx.doi.org/10.1063/1.1761116http://dx.doi.org/10.1063/1.1884128http://dx.doi.org/10.1063/1.2096582http://dx.doi.org/10.1063/1.2751601http://dx.doi.org/10.1017/S0022377814000671http://dx.doi.org/10.1017/S0022377814000671http://dx.doi.org/10.1111/j.1365-2966.2010.16493.xhttp://dx.doi.org/10.1111/j.1365-2966.2010.16493.xhttp://dx.doi.org/10.1063/1.2356485http://dx.doi.org/10.1063/1.2138568