A 3D MHD simulation of SN 1006: a polarized emission study for the turbulent case

1.9 MB·

by  P. F. Velázquez

MNRAS000,1–8(2002) Preprint23January2017 CompiledusingMNRASLATEXstylefilev3.0
A 3D MHD simulation of SN 1006: a polarized emission
study for the turbulent case
P. F. Vela´zquez1(cid:63), E. M. Schneiter2,3, E. M. Reynoso4, A. Esquivel1, F. De Colle1,
J. C. Toledo-Roy5, D.O. Go´mez 4,6, M.V. Sieyra2, A. Moranchel-Basurto7
1Instituto de Ciencias Nucleares, Universidad Nacional Auto´noma de M´exico, Ciudad de M´exico, M´exico
2Instituto de Astronom´ıa Te´orica y Experimental, Universidad Nacional de Co´rdoba, C´ordoba, Argentina
3Departamento de Materiales y Tecnologia, UNC, Co´rdoba, Argentina
7 4CONICET-Universidad de Buenos Aires. Instituto de Astronom´ıa y F´ısica del Espacio, Suc. 28, CP: 1428, Buenos Aires, Argentina
1 5Centro de Ciencias de la Complejidad, Universidad Nacional Aut´onoma de M´exico, Ciudad de M´exico, M´exico.
0 6 Departamento de F´ısica, Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, Buenos Aires, Argentina
2 7Escuela Superior de F´ısica y Matema´tica, Instituto Polit´ecnico Nacional, Ciudad de M´exico, M´exico.

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J Accepted.Received

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ABSTRACT

] Three dimensional magnetohydrodynamical simulations were carried out in order to
E
perform a new polarization study of the radio emission of the supernova remnant SN
H
1006. These simulations consider that the remnant expands into a turbulent interstel-
. lar medium (including both magnetic field and density perturbations). Based on the
h
p referenced-polarangletechnique,astatisticalstudywasdoneonobservationalandnu-
- merical magnetic field position-angle distributions. Our results show that a turbulent
o medium with an adiabatic index of 1.3 can reproduce the polarization properties of
r
t theSN1006remnant.Thisstatisticalstudyrevealsitselfasausefultoolforobtaining
s the orientation of the ambient magnetic field, previous to be swept up by the main
a
supernova remnant shock.
[

1 Key words: MHD–radiation mechanisms: general – methods : numerical – super-
v novae: individual: SN1006 –ISM: supernova remnants
9
8
5
5
0 1 INTRODUCTION in turn affects the radio emission and is imprinted in the
. measured Stokes parameters.
1 SN 1006 is a young supernova remnant (SNR) that has
Jun&Jones(1999)performed2DMHDsimulationsof
0 gainedinterestduetothelargeobservationaldataavailable
the evolution of a young Type Ia SNR interacting with an
7 inawidewavelengthrange,thereforeservingasanideallab-
interstellarcloud.Theyfoundthattheinteractionproduced
1 oratorywhentryingtounderstandtheobservedmorphology
: RT instabilities causing amplification of the magnetic field,
v in each frequency. This remnant is classified as part of the
andsubsequentlychangingthesynchrotronbrightness.This
i bilateral SNR group, whose main characteristic is the pres-
X work emphasized the importance of including a turbulent
ence of two bright and opposite arcs in radio-frequencies.
medium when trying to match observations. In this direc-
r The morphology and emission of this type of SNRs is
a tion,Balsaraetal.(2001)performedmorerealistic3Dsim-
largelydeterminedbytheenvironmentinwhichtheyevolve,
ulationsofaSNRevolvinginaturbulentbackground.They
sometimeshavinganirregularorclumpybackgroundand/or
found that the variability of the emission during the early
with the presence of density and magnetic fields gradients.
phase of SNR evolution gives information about the turbu-
The interstellar medium is known to be turbulent, as
lent environment. At the same time, that the interaction
inferred from observational data (Lee & Jokipii 1976) and
with such a turbulent environment generates an enhanced
local information on the interplanetary medium (Jokipii
turbulent post-shock region which has observational conse-
et al. 1969). Such turbulent medium, with a Kolmogorov-
quences,asitaffectstheaccelerationofrelativisticparticles.
likepowerspectrumthatspansoveralargerangeofspatial
Guo et al. (2012) employed 2D MHD simulations to
scales (Guo et al. 2012), gives rise to Rayleigh-Taylor (RT)
study the magnetic field amplification mechanisms during
instabilities during the fast expansion of the SNR, which
the propagation of the SNR blast wave. They found that,
for high resolution simulations, magnetic field growth at
small scales occurs efficiently in two distinct regions: one
(cid:63) Email:[email protected] related to the shock amplification, and the other, to the
(cid:13)c 2002TheAuthors
2 Vel´azquez et al.
RT-instabilities at the contact discontinuity between the
shocked ejecta and the shocked interstellar medium.
Fang&Zhang(2012)carriedoutastudysimilartothat (a)
of Guo et al. (2012) but considering different adiabatic in-
dexes to account for both the diffusive shock acceleration
and the escape of the accelerated particles from the shock.
Theyfoundthatasmallereffectiveadiabaticindexproduces
a larger magnetic field enhancement. They extended their
studyconsideringascenariowheretheexpandingejectain-
teracts with a large, dense clump and found, in addition
to an increase in the complexity of the magnetic field, the
development of a non-thermal emitting filament. In a sub-
sequentstudy,Fangetal.(2014)performed3DMHDsimu-
lationsconsideringaturbulentmediumwithaKolmogorov-
like power spectrum with parameters resembling the SNR (b)
RX J0852.0-4622. Their X-ray and γ-ray synthetic maps
showedtheexpectedrippledmorphologywithabrokencir-
cular shape along the shell, nicely reproducing the observa-
tions.
In general, the diffusive shock acceleration is driven by
magneticfieldsstrongenoughtogeneratenon-thermalemis-
sion. Therefore, any structure or dynamic interaction that
resultsintheamplificationofthemagneticfieldhasimpor-
tant consequences on the observed brightness.
According to the non-thermal radio-emission morphol-
ogy, SN 1006 has been classified as a bilateral or barrel-
shaped SNR (Kesteven & Caswell 1987), showing two main
bright arcs towards the NE and SW. The non-thermal X-
ray emission is also predominant in the NE and SW rims (c)
(Cassam-Chena¨ı et al. 2008).
SN 1006 is located at a high Galactic latitude and is
therefore thought to be evolving in a fairly homogenous in-
terstellar medium. In Schneiter et al. (2010) and Schneiter
et al. (2015) we made use of this assumption and presented
studiesofthesystemin2Dand3D,respectively.Inthelat-
terworkwefurtherintroducedsyntheticmapsoftheStokes
Q and U parameters wich allowed a better and more direct
comparison with the observations (Reynoso et al. 2013).
Recently, West et al. (2016b, a) (see also, West et al.
2016a,b)studiedradioemissionforasampleofGalacticax-
isymmetric SNRs, including SN 1006. They concluded that
thequasi-perpendicularaccelerationmechanismcansucess-
Figure 1. Comparison of the linearly polarized intensity at 1.4
fully fit the observed morphology of the remnants in their
GHzbetweentheobservations(panel(a))andsyntheticmapsofa
sample, although SN 1006 seems to be the exception, since
SNRexpandingintoaturbulentmediumwithadiabaticindexγ=
the quasi-parallel mechanism agrees better with observa-
5/3(modelR1b,panel(b))andγ=1.3(modelR2b,panel(c))
tions.
InthepresentworkweusethesameSNRinitialization
as in the two previous works of Schneiter et al. (2010) and presentedinsection§4.Thediscussionandfinalconclusions
Schneiteretal.(2015)butrelaxingtheassumptionofaho- are given in section §5.
mogeneousISMbyconsideringthattheSNRevolvesintoa
turbulent medium as it was shown in Yu et al. (2015) (see
also Fang et al. 2014).
2 NUMERICAL MODEL
The goal of this work is to propose an alternative
methodtodeterminethepositionangleoftheambientmag- The numerical model employed is basically the same as in
netic field, based on the polar-referenced angle method em- Schneiteretal.(2010,2015),withtheadditionalassumption
ployedbyReynosoetal.(2013)andSchneiteretal.(2015). ofaturbulentbackground,whereboththedensityandmag-
The numerical model is presented in section §2. For netic fluctuations have a 3D Kolmogorov-like power spec-
completeness we recall the basic model employed by trum, as will be explained further down.
Schneiter et al. (2015) in §2.1 and in section §2.2 we ex- To simulate the evolution of SN 1006 we employed the
plain how the turbulence is introduced. Section §3 explains Mezcal code (De Colle & Raga 2006; De Colle et al. 2008,
howsyntheticradiomapswereobtainedandtheresultsare 2012).ThiscodesolvesthefullsetofidealMHDequationsin
MNRAS000,1–8(2002)
A 3D MHD study of the SN1006: the turbulent case 3
a Cartesian geometry with an adaptive mesh, and includes
a cooling function to account for radiative losses (De Colle (a)
& Raga 2006).
The computational domain is a cube of 24 pc per side,
whichwewilldenoteas(x,y,z),andisdiscretizedonafive
level binary grid with a maximum resolution of 4.7×10−2
pc. All the outer boundaries were set to outflow condition.
2.1 SNR initial conditions
In what follows, we describe the physical parameters and
setupusedtosimulatetheSNR,whicharethesameasthose
presented in Schneiter et al. (2015).
A supernova explosion is initialized by the deposition
of E =2.05×1051 erg in a radius of R =0.65 pc located
0 0 (b)
at the centre of the computational domain. The energy is
distributedsuchthat95%ofitiskineticandtheremaining
5% is thermal.
Theejectedmasswasdistributedintwoparts:aninner
homogeneous sphere of radius r containing 4/7ths of the
c
total mass (M = 1.4M ) with a density ρ , and an outer
∗ (cid:12) c
shell containing the remaining 3/7ths of the mass following
a power law (ρ ∝ r−7) as in Jun & Norman (1996a). The
velocityhasaincreasinglinearprofilewithr,whichreaches
a value of v at r = R . The parameters ρ , r , and v
0 0 c c 0
are functions of E , M , and R , and were computed using
0 ∗ 0
equations (1)-(3) of Jun & Norman (1996a).
(c)
2.2 The turbulent background
Jun&Jones(1999)suggestedthattheturbulentstructures
of the brightest radio emission correlate well with the mag-
neticfieldingeneral.Forthisreasonweperformednewsim-
ulationswithamorerealisticmagnetizedturbulentinterstel-
lar medium. In what follows, we will make use of equations
(10) to (15) of Yu et al. (2015), which we reproduce below.
To introduce the turbulent background we assumed a 3D
Kolgomorov-like power spectrum fluctuation for both the
density and the magnetic field, similar to that of Jokipii
(1987)(seealsoYuetal.2015;Fangetal.2014).Thepower
spectrum follows:
Figure2.SameasFigure1butformapsoftheStokesparameter
Q.
1
P ∝ . (1)
1+(kL )11/3
c with
To generate the turbulence we assume a coherence
ulelnagtitohnsofarLecc=om3ppucteadnwdiathwNavmen=um90b3erwkav=e m2Lπod.eOs,uarnsdimL- A2(kn)=σB2 1+(k∆VLn)11/3 (cid:88)Nm(cid:20)1+(k∆VLn)11/3(cid:21)−1, (4)
variesbetweenLmin =∆xandLmax =Lsim,being∆xand n c n=1 n c
L the cell and the computational domain sizes, respec-
sim whereσ2 isthewavevarianceofthemagneticfield,andthe
tively. B
normalization factor, ∆V , is given by:
The initial magnetic field is given by: n
∆V =4πk2∆k . (5)
n n n
B(x,y,z)=B +δB, (2)
0
Both systems (x(cid:48),y(cid:48),z(cid:48)) and (x,y,z) are related by:
whereB =B (x)yˆandthemagneticfieldperturbationis:
0 0 x(cid:48) cosθ cosφ cosθ sinφ −sinθ x
n n n n n
δB=(cid:60)(cid:20)(cid:88)NmA(kn)(cid:0)cosαnxˆ(cid:48)+isinαnyˆ(cid:48)(cid:1)exp(iknzn(cid:48))(cid:21), yz(cid:48)(cid:48)=sin−θsnincoφsnφn sincθonssφinnφn cos0θn yz
n=1
(3) where θ and φ represent the direction of propagation of
n n
MNRAS000,1–8(2002)
4 Vel´azquez et al.
run γ δB δρ
(a)
R1a 5/3 no no
R1b 5/3 yes yes
R2a 1.3 no no
R2b 1.3 yes yes
R2c 1.3 yes no
R2d 1.3 no yes
Table 1. Runs carried out in this paper with their correspond-
ing hypothesis: adiabatic index, turbulent magnetic field and/or
turbulentdensitydistribution.
of a turbulent background with a Kolgomorov-like power
spectrum for both density and magnetic field. These runs
(b) are labeled as Rip, where i is 1 for the case of simulations
with an adiabatic index γ = 5/3, and 2 for γ = 1.3. The
label“p”indicatesthepresenceorabsenceofturbulencein
the background magnetic field and density: p = a indicates
no turbulence in either variable; p = b includes turbulence
inboth;p=conlyconsidersaturbulentB;andp=donly
considers a turbulent ρ.
Synthetic radio emission maps were obtained from the
numericalresults.Inordertocomparethemwiththeobser-
vations,thecomputationaldomain(denotedasxyzsystem),
theywererotatedwithrespecttothe“image”system(x y z
i i i
system). At the beginning both systems coincide. The x y
i i
plane of the “image” system is the plane of the sky, being
yˆ the direction towards the “North”, −xˆ the direction to-
i i
Figure 3. Synthetic polar-referenced angle maps obtained from
wards the “East”, and the line of sight (hereafter LoS) the
numericalsimulationsoftheSNR1006expandingintoaturbulent
zˆdirection. Then, synthetic maps were obtained after per-
mediumandwithadiabaticindexγ=5/3(modelR1b,panel(a))
formingthreerotationsonthecomputationaldomain.First,
and γ = 1.3 (model R2b, panel(b)) The axes are in pc and the
linearcolorscaleisgivenindegrees. arotationaroundyˆi wasapplied(the“North”)withanan-
gle ϕ . Second, a rotation in ϕ was carried out around
yi xi
thexˆ -direction.Finally,thecomputationaldomainwasro-
i
thewavemodenwiththewavenumberkn andpolarization tated by ϕzi around the zˆi-direction (the line of sight). To
αn. get the best agreement with the observations, after several
For the density fluctuation we employed the same log- tests these angles were set as −15◦, −30◦, and 60◦ for ϕ ,
xi
normal distribution as in Giacalone & Jokipii (2007): ϕ , and ϕ , respectively . In this way, the projection of
yi zi
the unperturbed magnetic field B was tilted by 60◦ with
0
respect to the yˆ direction.
n(x,y,z)=n exp(f +δf), (6) i
0 0
where f is a constant and δf is the density perturbation
0
withawavevarianceσ2.Bothδf andδBhavethesame3D 3.1 Synchrotron emissivity
d
Kolmogorov-like power spectral index.
Foreachpoint(x ,y ,z )oftheSNRwecanobtainthesyn-
The turbulent environment temperature and number i i i
chrotron specific intensity as (see C´ecere et al. 2016, and
density were set to T =104K and n =5×10−2cm−3, re-
0 0 references therein):
spectively.Thewavevariancesformagneticfieldanddensity
were set as σ2 =0.25B2 and σ2 =0.4n2.
B 0 d 0
As mentioned above, one of the purposes of this work j(x ,y ,z ,ν)∝Kρ v4α Bα+1ν−α, (7)
i i i ⊥
is to be able to study the effect of a perturbation on some
observedparameters.Tocomparewiththeobservations,the where ν is the observed frequency, B⊥ is the component of
synthetic maps were performed for an integration time cor- themagneticfieldperpendiculartotheLoS,αisthespectral
responding to 1000 yr (the age of SN 1006). index -which was set to 0.6 for this object- and ρ and v are
the density and velocity of the gas, respectively. The coeffi-
cientK includestheobliquitydependence,beingeitherpro-
portional to sin2Θ for the quasi-perpendicular case or to
3 SYNTHETIC EMISSION MAPS Bs
cos2Θ forthequasi-parallelcase.TheangleΘ isthean-
Bs Bs
InTable1welisttherunsthatwerecarriedout.Withthese gle between the shock normal and the post-shock magnetic
runs we want to analyze the effects of both the reduction field(Fulbright&Reynolds1990).ForthecaseofSN1006,
of the value of the adiabatic index γ and/or the inclusion Bocchinoetal.(2011)andReynosoetal.(2013)showedthat
MNRAS000,1–8(2002)
A 3D MHD study of the SN1006: the turbulent case 5
The position angle of the local magnetic field φ (x ,y ,z )
B i i i
is known from the simulations, and the position angle of
the local electric field φ(x ,y ,z ) can be obtained from
i i i
φ (x ,y ,z ) by applying a π rotation and correcting for
B i i i 2
Faraday rotation, as:
π
φ(x ,y ,z )=φ (x ,y ,z )− +∆χ . (12)
i i i B i i i 2 F
The Faraday correction term ∆χ is given by:
F
∆χ =RM λ2, (13)
F
where RM is the rotation measure (in units of rad m−2)
and λ is the wavelength of the observations (given in m).
In the present study, only the external RM arising in the
foreground ISM is considered. Bandiera & Petruk (2016)
explored the effects of internal RM on the polarized syn-
chrotronemissionofSNRs.ForthecaseofSN1006,wehave
Figure 4.Comparisonofthenormalizeddistributions(withre- carriedoutaroughestimationoftheinternalRM,obtaining
spect to their maxima) of the magnetic field position-angle as a value close to 10% of the reported one by Reynoso et al.
obtained from the observations and from the runs R1a and R2a (2013)whoobtainedaRMof12rad m−2 forthisremnant.
(different γ and both corresponding to a SNR propagating into
The linearly polarized intensity is computed as:
auniformmedium,i.e.withδB=δρ=0;seetable1),applying
thepolar-referencedangleselection.
(cid:112)
I (x ,y ,ν)= Q(x ,y ,ν)2+U(x ,y ,ν)2 (14)
P i i i i i i
the observed morphology of this remnant can be explained and the maps of the polarization angle distribution were
byconsideringthequasi-parallelcase.Schneiteretal.(2015) computed as follows:
carriedoutapolarisationstudyofthisremnant,basedon3D
MHD simulations, finding that only the quasi-parallel case 1
χ(x ,y )= tan−1(U(x ,y ,ν)/Q(x ,y ,ν)) (15)
can succesfully reproduced the observed morpholoy of the i i 2 i i i i
Stokes parameter Q (see Figure 3 of Schneiter et al. 2015).
Similarly,thedistributionofthemagneticfieldorienta-
For these reasons only the quasi-parallel case was consid-
tion can be calculated as:
eredinthiswork.Thesyntheticsynchrotronemissionmaps
are obtained by integrating j(x ,y ,z ,ν) along the LoS or
i i i 1
zi-axis, i.e.: χB(xi,yi)= 2tan−1(UB(xi,yi,ν)/QB(xi,yi,ν)) (16)
(cid:90) where UB(xi,yi,ν) and QB(xi,yi,ν)) are calculated with
I(xi,yi,ν)= j(xi,yi,zi,ν)dzi, (8) the equations (9) and (10) and replacing φ(xi,yi,ν) with
LoS φ (x ,y ,ν).
B i i
being x and y the coordinates in the plane of the sky.
i i
4 RESULTS
3.2 Stokes parameters and position angle
distribution maps 4.1 Synthetic polarization maps
With the purpose of comparing the numerical results with Figure 1 shows a comparison between the observed map of
the observations, synthetic maps of the Stokes parameters the linearly polarized intensity of SN 1006 (upper panel),
QandU werecalculatedasfollows(Clarkeetal.1989;Jun and the synthetic polarization maps obtained for runs with
& Norman 1996b; Schneiter et al. 2015): γ =5/3(runR1b,middlepanel)andγ =1.3(runR2b,bot-
tom panel) by using Equation (14). The observed map was
(cid:90) constructedbycombiningdataobtainedwiththeATCAand
Q(xi,yi,ν)= f0j(xi,yi,zi,ν)cos[2φ(xi,yi,zi)]dzi, theVLAat1.4GHz,asexplainedinReynosoetal.(2013).
LoS The polarized emission image, as well as the distribution of
(9)
the Q and U parameters, were convolved to a 15(cid:48)(cid:48) beam.
The two models used to construct the synthetic maps con-
(cid:90)
U(x ,y ,ν)= f j(x ,y ,z ,ν)sin[2φ(x ,y ,z )]dz , sider that the SNR is expanding into a turbulent medium
i i 0 i i i i i i i
LoS withperturbationsinbothdensityandmagneticfield.These
(10)
synthetic maps are shown in arbitrary units. Two opposite
where φ(x ,y ,z ) is the position angle of the local electric
i i i bright,noisyarcsareobservedinbothsyntheticmaps,hav-
field in the plane of the sky and f is the degree of linear
0 ing a striking resemblance to the observations. Reducing
polarization, which is a function of the spectral index α:
the value of γ produces a 5% smaller expansion radius of
α+1 theremnantasmeasuredonthelinearlypolarizedintensity
f = . (11)
0 α+5/3 maps.
MNRAS000,1–8(2002)
6 Vel´azquez et al.
Gaussian mean(◦) σ(◦)
g1 58.0 9.0
g2 23.0 13.0
Table 2. Two Gaussian fit of the observational position-angle
distribution
field perpendicular to the LoS, which is obtained through
Equation (16).
By using Equation (17), polar-referenced angle maps
areobtainedforrunsR1bandR2b,whichareshowninFig-
ure3.Thebluecolorindicatestheregionwherethemagnetic
fieldisalmostparalleltotheradialdirection,whileredcolor
highlights the regions where it is mostly perpendicular.
Giventhatthepolar-referencedangletechniqueisause-
Figure 5. Two Gaussian fit of the observed position-angle dis-
tribution. ful tool for estimating the direction of the pre-shock ISM
magneticfield(seeReynosoetal.2013;Schneiteretal.2015)
we carried out a statistical study based on the analysis of
theposition-angledistributioninthoseregionswhereχ ap-
r
proaches zero.
The analysis was performed for both the numerical re-
sults and the observations in regions with synchrotron in-
tensities larger than 10% of the maximum, and where the
condition χ (cid:54) 14◦ (the observational angle error) is satis-
r
fied. These criteria were chosen to assure a good signal to
noise ratio of the sample. The results are shown in Figure
4. To obtain the observational distribution, electric vectors
were computed by combining the Q and U images with the
miriadtaskIMPOL,andwerelaterrotatedby π toconvert
2
themintomagneticvectors.Theobservationalcurvehastwo
maxima:alargeoneat∼57◦ andasmalloneat∼25◦.Fig-
ure5showsafittingoftheobservationaldistributionbytwo
Gaussian labeled as g1 and g2, whose parameters are given
in Table 2. The mean value of Gaussian g1 is 58◦, which is
close to the inclination of the Galactic plane (60◦) and in
agreementwiththemaximaofthecurvescomputedforthe
Figure 6.SameasFigure4butcomparingthedistributionob-
tained for observations (excluding the contribution of Gaussian runs R1a and R2a (see Figure 4).
g2)andrunsR1bandR2b(withdifferentγ andforaturbulent It is reasonable to expect that the resulting ambient
medium,i.e.includingbothδρandδB). magnetic field is parallel to the Galactic plane at the lati-
tudeofSN1006(Bocchinoetal.2011;Reynosoetal.2013;
Schneiter et al. 2015). The secondary peak of the observed
Following the analysis developed by Schneiter et al. position-angledistributionwouldindicateanextramagnetic
(2015), we compare the observational and synthetic maps fieldcomponent,whichisnotconsideredinoursimulations.
of the Stokes parameter Q, obtained for the quasi-parallel Inordertoeliminatethissecondaryunmodelledcomponent,
case using Equation 9. These maps are shown in Figure 2. wesubtractedtheGaussianfitlabeledg2fromtheobserved
Agoodoverallagreementbetweenobservationsandnumer- distribution. The resulting curve will be referred to as the
ical results is obtained, since the opposite bright arcs are modified observational distribution.
wellreproduced.Also,notethatthesearcsareslightlymore Figure 6 compares the modified observational distribu-
elongatedthantheonesobtainedforthenon-turbulentISM tionwiththoseresultingfromtherunsR1bandR2b.Clearly
(Schneiter et al. 2015). thesenumericalcurvesdisplaynowwiderdistributionscom-
paredwithrunsR1aandR2a,whichisaconsequenceofin-
cludingperturbationsinBandρ.Themaximaofnumerical
4.2 Polar-referenced angle and a statistical study distributions remain close to 60◦.
In Figure 7 we explore the effect of selectively includ-
The polar-referenced angle distribution χ is given by:
r ing the perturbations in B and/or ρ for γ = 1.3. The curve
χ =cos−1(rˆ·ˆb ), (17) corresponding to the run R2d (δρ (cid:54)= 0 and δB= 0) does
r ⊥
not show any significant widening, in contrast with those
(cid:112)
where rˆ = (−x,y)/ x2+y2 is the radial direction and corresponding to the runs R2b and R2c, both with δB(cid:54)=0.
ˆb = (−sin(χ ),cos(χ )) is the direction of the magnetic Inordertocarryoutamorequantitativestudy,astatistical
⊥ B B
MNRAS000,1–8(2002)
A 3D MHD study of the SN1006: the turbulent case 7
formedonboththeobservationsandnumericalresults.This
mean(◦) σ(◦) skewness kurtosis studyrevealsthattheobservationaldistributioniswideand
has two maxima or components: a large one at 58◦that co-
R1a 60. 3.5 −0.32 0.2
incideswiththeexpecteddirectionoftheambientmagnetic
R1b 59. 7.5 0.52 5.2
field,andasmallcomponentat23◦.Thecurvescorrespond-
R2a 62. 6.6 −5.80 91.0
R2b 58. 11.0 −3.0 9.7 ing to runs R1a an R2a have a single peak and narrower
R2c 56. 13.0 −2.2 4.7 distributions.Thesecondarypeakoftheobservationscould
R2d 58. 9.9 −3.70 14.0 beduetolocalblow-outsproducedduringtheexpansionof
obs-g2 57. 22.0 −0.68 6.5 partsofthemainSNRshockfrontintolow-densitycavities,
such as those explored by Yu et al. (2015). Since our sim-
Table 3.Statisticsoftheposition-angledistributions ulations do not have this secondary component we filtered
it our from the observations and focused our comparison
withthedominantcomponent,asexplainedintheprevious
section.
The subsequent analysis was carried out by compar-
ingtheposition-angledistributionsobtainedfromnumerical
simulationswiththeobservationaldistributioncurve.Asta-
tistical study performed on these distributions reveals that
models which include a turbulent pre-shock magnetic field,
successfully explain the observed polar-angle distribution.
Furthermore, all of them share a maximum at a position
angleof60◦,whichisparalleltotheGalacticPlaneandco-
incideswiththeexpecteddirectionoftheGalacticmagnetic
field around SN1006 (Bocchino et al. 2011; Reynoso et al.
2013).
Insummary,thestatisticalanalysisbasedonthepolar-
referenced angle technique carried out in this work made
it possible to recover the orientation of the ambient mag-
netic field. Based on previous observational and theoreti-
cal studies of SN1006 (Bocchino et al. 2011; Reynoso et al.
2013; Schneiter et al. 2015), we have only considered the
Figure 7. Comparison of the position-angle distributions ob- quasi-parallel acceleration mechanism to estimate the syn-
tainedforrunsR2p,i.e.thoseconsideringγ=1.3.InmodelR2a chrotronemission.However,itisimportanttomentionthat
themediumisinitializedasuniformatthebeginningofthesim- the same technique presented here can be applied with the
ulation,whileinmodelR2btheSNRpropagatesintoaturbulent
quasi-perpendicularcase.Finally,agoodagreementbetween
medium(i.e.,δB,δρ(cid:54)=0.InmodelsR2candR2dthemediumis
observations and numerical results is obtained if the simu-
“partially” turbulent, with δB (cid:54)= 0,δρ = 0 and δρ (cid:54)= 0,δB = 0
lations include magnetic field perturbations.
respectively.
analysis was performed, comparing the distributions of the ACKNOWLEDGMENTS
position-angle obtained from observations (subtracting the
contributionofGaussiang2)andsimulations.Theresultsof The authors thank the referee for reading this manuscript
thisstatisticalanalysisaresummarizedinTable3.Compar- and for her/his useful comments. PFV, AE, and FDC
ingthevaluesobtainedforthestandarddeviation,skewness acknowledge finantial support from DGAPA-PAPIIT
andkurtosis,wenotethatthemodelsachievingabetterfit (UNAM) grants IG100516, IN109715, IA103315, and
with the observations are those that consider a perturbed IN117917. EMS, EMR, and DOG are members of the Car-
magnetic field, and a lower γ (runs R2b and R2c). rera del Investigador Cient´ıfico of CONICET, Argentina.
MVS and AM-B are fellows of CONICET (Argentina) and
CONACyT (M´exico), respectively. EMS thanks Paulina
Vela´zquezforherhospitalityduringhisvisittoMexicoCity.
5 DISCUSSION AND CONCLUSIONS WethankEnriquePalacios-Boneta(co´mputo-ICN)forman-
tainingtheLinuxserverswhereoursimulationswerecarried
AradiopolarizationstudyofSN1006wasperformedbased
out.
on 3D MHD simulations, considering the expansion of the
remnant into a turbulent interstellar medium (including
both magnetic field and density perturbations).
The inclusion of perturbations in magnetic field and REFERENCES
densitydonotchangethemainconclusionofSchneiteretal.
BalsaraD.,BenjaminR.A.,CoxD.P.,2001,ApJ.,563,800
(2015), namely that the quasi-parallel case is the accelera-
BandieraR.,PetrukO.,2016,MNRAS,459,178
tion mechanism that better explains the observedmorphol-
BocchinoF.,OrlandoS.,MiceliM.,PetrukO.,2011,A&A,531,
ogy in the distribution of the Stokes parameter Q. A129
Basedonthepolar-referencedanglemethod,astudyof Cassam-Chena¨ı G., Hughes J. P., Reynoso E. M., Badenes C.,
thepositionangledistributionofthemagneticfieldwasper- MoffettD.,2008,ApJ,680,1180
MNRAS000,1–8(2002)
8 Vel´azquez et al.
C´ecereM.,Vel´azquezP.F.,AraudoA.T.,DeColleF.,Esquivel
A., Carrasco-Gonz´alez C., Rodr´ıguez L. F., 2016, ApJ, 816,
64
ClarkeD.A.,BurnsJ.O.,NormanM.L.,1989,ApJ,342,700
DeColleF.,RagaA.C.,2006,A&A,449,1061
DeColleF.,RagaA.C.,EsquivelA.,2008,ApJ.,689,302
DeColleF.,GranotJ.,L´opez-C´amaraD.,Ramirez-RuizE.,2012,
ApJ.,746,122
FangJ.,ZhangL.,2012,MNRAS,424,2811
FangJ.,YuH.,ZhangL.,2014,MNRAS,445,2484
FulbrightM.S.,ReynoldsS.P.,1990,ApJ,357,591
GiacaloneJ.,JokipiiJ.R.,2007,ApJL,663,L41
GuoF.,LiS.,LiH.,GiacaloneJ.,JokipiiJ.R.,LiD.,2012,ApJ.,
747,98
JokipiiJ.R.,1987,ApJ,pp842–846
JokipiiJ.R.,LercheI.,SchommerR.A.,1969,ApJL,157,L119
JunB.-I.,JonesT.W.,1999,ApJ,511,774
JunB.-I.,NormanM.L.,1996a,ApJ,465,800
JunB.-I.,NormanM.L.,1996b,ApJ,472,245
KestevenM.J.,CaswellJ.L.,1987,A&A,183,118
LeeL.C.,JokipiiJ.R.,1976,ApJ,206,735
ReynosoE.M.,HughesJ.P.,MoffettD.A.,2013,AJ,145,104
Schneiter E. M., Vel´azquez P. F., Reynoso E. M., de Colle F.,
2010,MNRAS,408,430
SchneiterE.M.,Vel´azquezP.F.,ReynosoE.M.,EsquivelA.,De
ColleF.,2015,MNRAS,449,88
West J. L., Safi-Harb S., Ferrand G., 2016a, preprint,
(arXiv:1609.02887)
West J. L., Safi-Harb S., Jaffe T., Kothes R., Landecker T. L.,
FosterT.,2016b,A&˜A,587,A148
YuH.,FangJ.,ZhangP.F.,ZhangL.,2015,A&A,579,A35
ThispaperhasbeentypesetfromaTEX/LATEXfilepreparedby
theauthor.
MNRAS000,1–8(2002)