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Cosmic-Ray Anisotropy and the Local Interstellar Turbulence

We study the role of local interstellar turbulence in shaping the large-scale anisotropy in the arrival directions of TeV-PeV cosmic-rays (CRs) on the sky. Assuming pitch-angle diffusion of CRs in a magnetic flux tube containing the Earth, we compute the CR anisotropy for Goldreich-Sridhar turbulence, and for isotropic fast modes. The narrow deficits in the 400 TeV and 2 PeV data sets of IceTop can be fitted for some parameters of the turbulence. The data also rule out a part of the parameter space. The shape of the CR anisotropy may be used as a local probe of the still poorly known properties of the interstellar turbulence and of CR transport.


Introduction
In this paper we report on investigations of how the shape of the large-scale (LS) anisotropy of TeV-PeV cosmic-rays, (i.e., excluding features whose angular sizes are smaller than a few tens of degrees) depends on the properties of the interstellar turbulence and cosmic ray (CR) transport within ∼ 10 pc from Earth [1]. Up until now, most studies of the large-scale CR anisotropy (CRA) have focussed on the direction and amplitude of the dipole, and in particular its relation to local sources of CRs (for a recent study see e.g. [2]). The direction of the CRA is observed to be compatible with that of the local interstellar magnetic field, as deduced from the IBEX ribbon and from polarization of starlight from stars within ten to a few tens of pc from Earth [3,4,5]. However, the LS CRA is not well described by a dipole [6]. A few earlier studies have modeled phenomenologically the LS CRA as the sum of a dipole and higher order multipoles (e.g. [7]), but the study we present here is, to our knowledge, the first quantitative description linking it to the power-spectrum and other parameters of the turbulence.

Expression for the large-scale CRA
The alignment of the CRA with local field lines within ∼ 10 pc is compatible with the widely held view that CRs diffuse preferentially along field lines. Furthermore, because the power in the fluctuations on which TeV-PeV CRs scatter (∼ 10 −4 − 1 pc 10 pc) is small with respect to that in the ordered field [3], we assume pitch-angle diffusion of CRs in a ∼ 10 pc-long, uniform flux tube containing the Earth, denoting by D µµ the corresponding pitchangle diffusion coefficient, (µ is the cosine of the CR pitch-angle, the angle between the CR momentum and the ordered magnetic field). Since we study here the shape of the CRA, and not its absolute amplitude, we normalize the latter to 1. Assuming homogeneous turbulence, and that the problem is 1D and stationary, the normalised CRA at Earth [1] is provided that the distance between the boundaries of the flux tube and the Earth is large enough for arXiv:1702.01001v1 [astro-ph.HE] 3 Feb 2017 the diffusion approximation to apply. A delimitation of the parameter space in which this condition is satisfied is given in [1]. Outside this range, the CRA is determined by unknown, external boundary conditions. From now on, we only consider cases where the CRA is proportional to g(µ). In the following, we use the (dimensionless) pitch-angle scattering frequency ν( where l denotes the outer scale of the turbulence and v ≈ c is the CR velocity. The physically unmotivated case of isotropic pitch-angle scattering corresponds ν(µ) = constant, and to a purely dipole anisotropy, g(µ) = µ. D µµ (cf. Eq. (20) in Ref. [1]) can be expressed in terms of a phenomenological resonance function, R n (k v − ω + nΩ), where k denotes the parallel component of the wavevector k, ω the angular frequency of waves, Ω the CR gyrofrequency, and v = vµ. We use broad (R B n ) and narrow (R N n ) resonance functions, taken respectively from [8] and [9]: where v ⊥ = v 1 − µ 2 . R B n takes into account the broadening of the resonance due to fluctuations of the magnetic field strength, expressed as the parameter δM A 1, whose local value is poorly constrained. R N n assumes, instead, that the broadening of the resonance, described by τ , is dominated by the Lagrangian correlation time of the turbulence.
First, we consider Goldreich-Sridhar (GS) turbulence [10], with a spectrum of Alfvén and pseudo-Alfvén waves following the prescription of [11]: , we also studied spectra with an abrupt cutoff in k and found qualitatively similar trends. The resonance function R N n provides so little scattering that the CRA is given by g(µ) only in a small fraction of parameter space, in which it anyway does not fit Ice-Top data. For GS turbulence, we then only use R B n . We calculate numerically D µµ , and plot ν(µ) (resp. the CRA, g(µ)) in the upper left (resp. centre) panel of Fig. 1, for 3 sets of values of { , δM A } that fit well IceTop data [6]: . For these parameters, ν exhibits a minimum in the range |µ| 0.55 − 0.8 which corresponds to the transition between two regions: At smaller |µ| (i.e. perpendicular to field lines), scattering is dominated by the n = 0 contribution of pseudo-Alfvén modes, whereas at larger |µ|, Alfvén modes dominate. At fixed , and when δM A increases, the minimum of ν occurs at larger |µ|, cf. the two red lines. Indeed, the width of the bump around µ = 0 increases for broader resonances. The minimum of ν corresponds to the sharp increase of g at large µ, see centre panel and Eq. (1). This leads to excesses/deficits in the CRA along field lines (µ = ±1) that are narrower than for a dipole (black dashed line). We plot the anisotropy in (R.A., decl.) for {10 −3 , 0.33} in the lower left panel. Tight cold/hot spots are present along the field, and a rather wide flat region lies in-between (magenta). This leads to a Southern sky map similar to what IceTop observes (lower centre panel): A narrow cold spot (dark blue) surrounded with a flat CR intensity. The two right panels show our predicted relative intensities at −75 • ≤ decl. ≤ −35 • versus IceTop data sets for a fixed set of turbulence parameters (δM A = 0.33): At low CR energy ( = 10 −3 ), we can fit well the 400 TeV data, and by increasing the energy by a factor 10 ( = 10 −2 ) -comparable to the factor 5 in the data, the 2 PeV data is also well fitted. We note that the existing data can also exclude a non-negligible range of possible parameter values, see [1] for a wider scan.
Second, we study isotropic fast mode turbulence with a power spectrum I F (k) ∝ k −3/2 , as suggested by [12]. In Fig. 2, we plot ν (left), g (centre), and the relative CR intensity at −75 • ≤ decl. ≤ −35 • versus IceTop 2 PeV data (right). We consider R B n with δM A = 0.01 (blue dashed-dotted lines), 0.1 (orange solid), 0.33 (red dashed), 1 (magenta dotted), as well as R N n for a local Alfvén velocity v A = 10 km/s (grey solid), and with τ = √ l/v A √ k. We take = 10 −3 for the plot of ν(µ). We find that g does not depend on here. As for pseudo-Alfvén modes above, the n = 0 term for fast modes is now responsible for the peak of ν around µ = 0.  This peak grows in width when δM A increases. With the narrow resonance function, it becomes very sharp and the minimum of ν is close to µ = 0, see grey line. This results in a qualitatively different shape of the CRA, cf. middle panel: Very wide cold/hot spots with a rather flat intensity inside. They take nearly half of the sky each ( 80 • halfwidth). IceTop data clearly rules out this a priori acceptable scenario, cf. right panel. For R B n , the 2 PeV data is well fitted with δM A = 0.1 and 0.33, where the deficit at R.A. ≈ 90 • reaches its minimum width. However, the 400 TeV data is not well fitted. Decreasing δM A makes the deficit too wide (blue lines), while increasing δM A to 1 (magenta lines) makes the anisotropy tend towards a dipole, which again increases the size of the deficit.

Discussion and perspectives
In all models above, the CRA exhibits a flattening in directions perpendicular to field lines, due to the peak of the scattering frequency around µ = 0. Interestingly, this signature is compatible with the observational data. Moderately broad resonance functions are able to produce deficits/excesses along the field direction (µ = ±1) that are narrower than those of a dipole. Too broad a resonance would, however, result in an approximately dipole anisotropy with constant ν, see the magenta lines in Fig. 2. On the other hand, narrow resonance functions are disfavoured by IceTop data. Nonetheless, we cannot formally exclude narrow resonance functions for models of turbulence in which ν is so small that the CR mean free path is 100 pc, such as in [9], since our study does not then apply. A very low CR scattering rate locally is not impossible, but shifts the problem of CR confinement and the explanation of its anisotropy to large distance. The increase with CR energy of the width of the deficit between the two IceTop data sets may hint at a |k|-dependent anisotropy in the turbulence powerspectrum, such as in GS turbulence. Other possibilities, such as an energy-dependence of the resonance function should also be explored. As for fast modes, they should suffer from damping [8], which we did not take into account, and which may have an effect on the CRA. A combined analysis of all available CRA data should yield tighter constraints than those presented in Sect. 3. Distortions of the CRA by heliospheric fields may complicate the picture at 10 TeV. The recent data from the Tibet Air Shower Array [13] hints at the presence of a narrow hot spot in the Northern hemisphere, in their 300 TeV data set (cf. their Fig. 4), as would be ex-  pected within our model and for a D µµ symmetric with respect to µ = 0.

Conclusions
Assuming pitch-angle diffusion of Galactic CRs in our local environment, we deduced the shape of the LS CRA, see Eq. (1). In general, it is not a pure dipole, but contains imprints of the still poorly known properties of (i) the local interstellar turbulent magnetic fields (e.g. power-spectrum), and (ii) CR transport (via R n ). We find that the existing observational data already puts constraints on these. A moderately broad resonance function seems to be favoured. IceTop 2 PeV data can be fitted either with GS turbulence or isotropic fast modes (see parameters in Figs. 1 and 2), but only the former can reproduce the change in the width of the deficit between the 400 TeV and 2 PeV data sets. We suggest that the shape of the LS CRA can be used as a new observable.