Issue 
A&A
Volume 597, January 2017



Article Number  A117  
Number of page(s)  5  
Section  Astrophysical processes  
DOI  https://doi.org/10.1051/00046361/201629526  
Published online  13 January 2017 
Power requirements for cosmic ray propagation models involving diffusive reacceleration; estimates and implications for the damping of interstellar turbulence
^{1} Dublin Institute for Advanced Studies, School of Cosmic Physics, 31 Fitzwilliam Place, Dublin 2, Ireland
email: LD@cp.dias.ie
^{2} MPI für Extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany
Received: 13 August 2016
Accepted: 21 October 2016
We make quantitative estimates of the power supplied to the Galactic cosmic ray population by secondorder Fermi acceleration in the interstellar medium, or as it is usually termed in cosmic ray propagation studies, diffusive reacceleration. Using recent results on the local interstellar spectrum, following Voyager 1’s crossing of the heliopause, we show that for parameter values, in particular the Alfvén speed, typically used in propagation codes such as GALPROP to fit the B/C ratio, the power contributed by diffusive reacceleration is significant and can be of order 50% of the total Galactic cosmic ray power. The implications for the damping of interstellar turbulence are briefly considered.
Key words: cosmic rays / ISM: structure / turbulence / acceleration of particles
© ESO, 2017
1. Introduction
In most discussions of cosmic ray propagation it is assumed that the cosmic rays are produced in discrete sources, generally taken to be supernova remnants (SNRs), although there is increasing interest in and evidence for possible additional classes of sources, see e.g. the presentations in the recent conference organised by Tibolla & Drury (2014), and the recent exciting evidence for acceleration of protons to PeV energies in the Galactic centre region (H.E.S.S. Collaboration et al. 2016). They then diffuse through the interstellar medium and an extended cosmic ray halo before escaping from the Galaxy. This diffusion is not just in space, but also in momentum, if, as is inevitably the case, the magnetic fields that scatter the particles are not purely static but are in random motion with characteristic velocities of order the Alfvén speed. This leads to a certain amount of secondorder Fermi acceleration during propagation, an effect which for historical reasons is usually referred to as “reacceleration”. There has been a long and inconclusive debate as to the importance of reacceleration, but there is no doubt that the idea is attractive for a variety of reasons, and physically the effect must occur at some level. For clarity we note that the term “reacceleration” is also sometimes used to refer to the acceleration by supernova remnants (SNR) shocks of preexisting ambient cosmic rays; in this paper we do not consider this shock reacceleration process and are exclusively concerned with diffusive reacceleration.
One of the strongest arguments in favour of diffusive reacceleration is that it allows a rather natural fit to the low energy boron to carbon data. This was persuasively argued by Heinbach & Simon (1995) who showed that with reacceleration the B/C data could be well fit with a single powerlaw dependence of the escape pathlength as a function of rigidity, whereas in a leakybox model one had to suppose an unnatural decrease in the pathlength at low energies. The fact that the inferred powerlaw dependence of the pathlength also agreed with that predicted for Kolmogorov turbulence was seen as another positive feature of the model (although whether interstellar magnetic turbulence should be described by a Kolmogorov spectrum is another question).
This reacceleration by interstellar turbulence is a potentially significant contribution to the total Galactic cosmic ray source power (and of course also a potentially significant damping term for interstellar turbulence). This was qualitatively discussed in Thornbury & Drury (2014) and presented at the ICRC by Drury & Strong (2015) on the basis of analytic estimates. In this paper we seek to make quantitative estimates of the diffusive reacceleration power using both recent parametrisations of the local interstellar spectrum and the wellestablished cosmic ray propagation code GALPROP as first described in Strong & Moskalenko (1998). GALPROP has become the de facto reference model for cosmic ray propagation studies in our Galaxy and is thus an appropriate choice, but any other propagation model incorporating diffusive reacceleration should give very similar results, e.g. the DRAGON code of Evoli et al. (2016).
The power transferred to the cosmic rays comes of course at the expense of the general turbulence in the interstellar medium so we also evaluate a damping process for interstellar turbulence. An important aspect of this problem is that it depends (as we will see) sensitively on the lowenergy form of the cosmic ray spectrum in interstellar space. Until recently this was largely unknown, but we now have direct in situ observations from the Voyager spacecraft of the cosmic ray spectrum beyond the heliopause which we can use to constrain the local interstellar spectra at subrelativistic energies (Stone et al. 2013). There are also useful constraints from the diffuse gammaray emission of the Galaxy (Strong 2015) which are important as being independent of solar modulation and confirming the spectral break at GeV energies.
2. Reacceleration power
This section briefly reviews and expands on the main results of Thornbury & Drury (2014). The basic equation underpinning all diffusion models of cosmic ray transport, going back at least to the classic monograph of Ginzburg & Syrovatskii (1964) is (1)Here f(x,p,t) is the isotropic part of the phase space density of a given species as a function of position x, scalar momentum p and time t and Q(x,p,t) is a source term representing the initial production and acceleration of cosmic rays. The spatial and momentum space diffusion coefficients are D_{xx} and D_{pp} respectively and will in general be functions of position, momentum, and time. On heuristic grounds (Thornbury & Drury 2014) the two diffusion coefficients are related by (2)Detailed calculations (Skilling 1975a,b,c), see also Eqs. (9.38) and (9.39) in Berezinskii et al. (1990), show that (3)where the angle brackets denote an average over an isotropic pitch angle distribution μ being the pitch angle cosine, (4)and ν_{±} is the rate of pitchangle scattering off forward and backward propagating Alfvén waves. If the scattering rates are taken to be constant and equal we recover the naive heuristic result, but in general the scattering rates should be functions of the pitch angle and related to the wave spectrum through the gyroresonant condition. This introduces a weak dependence on the shape of the wave spectrum, but not on its amplitude. Specifically, if we assume a powerlaw wave spectrum with W(k) ∝ k^{− a} where ^{∫}W(k) dk is the total energy content of the waves and k is the wavenumber (a = 5/3 being a Kolmogorov spectrum for example). (5)where r_{g} = p/eB_{0} is the particle gyroradius, B_{0} the background magnetic field, and the resonant condition is (6)Considered as a function of pitch angle the scattering rates thus scale as (7)so that (assuming ν_{+} = ν_{−}) (8)Thus more generally (9)which agrees with the simple heuristic estimate for a = 1.
However if we hold μ fixed and look at the scattering rate as a function of particle momentum or gyroradius, then (10)and thus (11)which is the commonly used form, D ∝ vR^{δ} or velocity times a powerlaw in particle rigidity (momentum per charge, which is directly proportional to the gyroradius for fixed magnetic field). The powerlaw index of the rigidity dependence of the spatial diffusion coefficient, δ is thus related to that of the wave spectrum by (12)and as is easily verified (13)In fact the denominator can be written (14)which shows that it is symmetric about and has a local maximum at a = 1. Thus within this simple quasilinear theory of particle scattering we have (15)which is essentially the form used by GALPROP, see Eq. (1) in Strong & Moskalenko (1998) derived from Seo & Ptuskin (1994), if their factor 4/3w is set to unity (the inclusion of w appears formally incorrect, but as it is treated as a constant of order unity it makes no difference to the results). It is interesting to note that for equal intensities of forward and backward propagating waves the naive scattering estimate corresponds to the minimum possible level of reacceleration, but of course lower values can be obtained with anisotropic wave fields.
For convenience we will from now on write (16)For a Kolmogorov spectrum with δ = 1/3 we have ϑ = 81/385 ≈ 0.21 and the largest it can be is for δ = 1 where we have ϑ = 1/9 ≈ 0.11; the results of Strong & Moskalenko (1998) can be obtained by setting(17)The local reacceleration power density (energy per unit time and per unit volume) is shown in Thornbury & Drury (2014), assuming very reasonable regularity conditions on the particle distribution function, to be given by the integral over the particle spectrum, (18)which can be written, if D_{pp} is expressed in terms of D_{xx} using the above relation, as (19)If we parametrise the spatial diffusion in the usual fashion as (20)where m is the particle mass and c the speed of light this can be written in the useful and rather transparent form (21)which gives the local reacceleration power density in terms of a simple integral over the spectrum. The formula is interesting in that the term is a rate, mc^{2} is just the particle rest mass energy, and the integral is essentially just the total number density of cosmic ray particles biased by a powerlaw factor with exponent 1−δ. Thus the energy transfer is more or less as if all particles were acquiring their own rest mass energy on a time scale of . Integrating this over the entire Galaxy then gives the total power transferred to the cosmic ray population from Alfvénic turbulence.
2.1. Numerical estimates using Voyager data
Numerical evaluation of this integral requires knowledge of the lowenergy part of the interstellar cosmic ray spectrum, as noted in Thornbury & Drury (2014), and until recently this was quite poorly constrained. However the situation has dramatically changed with the recent passage of the Voyager spacecraft into the local interstellar medium which allows us for the first time to have access to in situ measurements of the lowenergy cosmic ray flux just outside the heliosphere (Potgieter 2014). A useful analytic fit to the local interstellar flux of protons, J_{LIS}, has been given by Vos & Potgieter (2015) in the form (22)where T is the kinetic energy in units of GeV and β = v/c is the dimensionless particle speed. Noting that dT = v dp and that p^{2}f(p)v dp = j(T) dT where p is particle momentum and f is the phase space density we can convert this flux to a local interstellar phase space density via (23)In Fig. 1 we show the corresponding spectrum plotted slightly unconventionally as a differential number spectrum in log momentum; we plot the number of protons per logarithmic interval in momentum, 4πp^{3}f(p) noting that the total number density of particles is just the area under this curve, (24)Presenting the data in this way brings out just how sharply peaked the local interstellar cosmic ray proton spectrum is around 1 GeV. On a more conventional log log plot one can see that there are powerlaw tails extending to both lower and higher energies, see Fig. 2, but by far the dominant population, at least by number, are the mildly relativistic ones. It is interesting to note that this spectrum corresponds to a total number density of 1.2 × 10^{3} cosmic ray protons per cubic meter locally, an energy density of 0.7 eV cm^{3} and a pressure of 0.33 eV cm^{3}.
Fig. 1 Local interstellar proton number spectrum from Vos & Potgieter (2015). 

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Fig. 2 Local interstellar proton number spectrum from Vos & Potgieter (2015) in a more conventional log log representation showing the powerlaw tails. 

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Fig. 3 Integral of (p/mc)^{1−δ} weighted by the local interstellar proton number spectrum from Vos & Potgieter (2015) as a function of δnote that the dimensions are m^{3}. The value for δ = 1 is just the cosmic ray number density. 

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Fig. 4 Local reacceleration power density from Eq. (21), the Vos and Potgieter local interstellar spectrum, V_{A} = 30 km s^{1} and D_{0} = 10^{28} cm^{2} s^{1}. 

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We can now evaluate the integral in Eq. (21) over the local interstellar spectrum as parametrized by Vos and Potgieter. The result is shown in Fig. 3 and shows a very weak dependence on δ. In Fig. 4 we show the corresponding power density from Eq. (21) using (25)and canonical values (26)We only plot the physically relevant range 0.3 <δ< 0.6 where we see that the power density is (27)if we now naively take the effective volume for the Galaxy to be 4 × 10^{61} m^{3} then the total power input from diffusive reacceleration can be estimated as 5 × 10^{33} W = 5 × 10^{40} erg s^{1}. This should be compared with the canonical estimate of the total cosmic ray Galactic luminosity of order 10^{34} W or 10^{41} erg s^{1} (see discussion in Drury 2014, where it is noted that there is probably half a decade of systematic uncertainty in this estimate either way). Thus we have the, at first sight rather remarkable, result that diffusive reacceleration may be contributing as much as 50% of the total cosmic ray luminosity of the Galaxy!
It is worth noting that if there is still some residual solar modulation beyond the heliopause, the local interstellar spectrum would have even more low energy particles and the diffusive reacceleration power would increase. Similarly, it is hard to believe that the local lowdensity bubble in which the solar system is located contains a significantly higher density of lowenergy cosmic rays than the general Galactic average at the Sun’s distance from the Galactic centre; if anything, adiabatic expansion of the hot bubble would imply a slightly lower value. The ionization rates inferred from interstellar chemistry in molecular clouds also seem to indicate that the solar system cosmic ray environment is quite representative of the local Galaxy, as does the diffuse gammaray emission of the Galaxy (although at higher energies), see e.g. Grenier et al. (2015).
2.2. Estimates using GALPROP
As a crosscheck on the above we now use the numerical CRpropagation package GALPROP^{1}, using parameters which reproduce B/C with reacceleration, and then with the same parameters but without the reacceleration term, so that the difference in energy content is due to the reacceleration process^{2}. The total CR proton energy content of the Galaxy is computed by integration over momentum and volume.
We base the calculation on the model z04LMS, which has reacceleration and a CR halo height of 4 kpc and V_{A} = 30 km s^{1}Strong et al. (2010). This model has typical parameter values which reproduce B/C in reacceleration models (see also Trotta et al. 2011; Jóhannesson et al. 2016).
The CR proton energy content of the Galaxy is (8.1, 6.4) × 10^{55} erg with and without reacceleration respectively. Hence 1.7 × 10^{55} erg results from reacceleration, or ≈20% of the total; stated another way, the original energy injected by sources is boosted by ≈25%.
The luminosity of the Galaxy can be estimated from the total energy content using a value for the residence time of CR in the Galaxy. The total proton luminosity for our reacceleration model^{3} is 8 × 10^{40} erg s^{1}Strong et al. (2010), so the effective CR residence time is ≈ 3 × 10^{7} yr. Hence the proton luminosity is 8.0, 6.3 × 10^{40} erg s^{1} with and without reacceleration respectively. This is consistent with the analytical estimates in Sect. 2.1. Note that the relative values quoted above are independent of the assumed residence time.
3. Conclusions and implications for interstellar turbulence
Our estimates of the reacceleration power are necessarily approximate, but suffice to demonstrate that, for parameters chosen to reproduce B/C and commonly used in propagation calculations, the energy input via reacceleration is of order a quarter to half the total energy input. SNRs are then not “the sources of CR” in such models, at least not in the conventional sense! In retrospect this is perhaps not as surprising as it first seems. If the bulk of the energy resides in mildly relativistic and subrelativistic particles, and if the spectrum in this region is to be significantly modified by reacceleration, then the energy input must be significant.
An interesting consequence is that the cosmic rays in such models must also damp interstellar turbulence and it is interesting to ask whether this is physically plausible and significant. Energetically it is not impossible. The main energy input into interstellar turbulence is generally taken to be the mechanical energy from expanding SNR shells and there is thus enough power input, but at quite large scales (Elmegreen & Scalo 2004; Scalo & Elmegreen 2004). The turbulence is normally assumed to be dissipated by nonlinear cascading to high wavenumber modes and the question is whether the cosmic rays can extract enough energy from the cascade at the scales which scatter mildly relativistic particles before thermal dissipation takes over. This is far from obvious, but if it is the case then the cosmic rays may define the inner scale of the interstellar turbulence. SNRs would then remain the ultimate engine driving cosmic ray acceleration, but through two channels; a direct one involving shock acceleration, and an indirect one mediated by interstellar turbulence.
Meanwhile it is essential to consider alternative explanations of the peak in the energydependence B/C, in particular convection gives a fairly natural mechanism (e.g. Korsmeier & Cuoco 2016) and there is evidence for a Galactic wind (e.g. Everett et al. 2012). The main message of this work is that behind the reacceleration term in the propagation codes there is a significant impact on the total energy budget of both the cosmic rays and the interstellar turbulence. It is not a free parameter than one can tune at will without physical consequences.
Current version available at https://sourceforge.net/projects/galprop
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All Figures
Fig. 1 Local interstellar proton number spectrum from Vos & Potgieter (2015). 

Open with DEXTER  
In the text 
Fig. 2 Local interstellar proton number spectrum from Vos & Potgieter (2015) in a more conventional log log representation showing the powerlaw tails. 

Open with DEXTER  
In the text 
Fig. 3 Integral of (p/mc)^{1−δ} weighted by the local interstellar proton number spectrum from Vos & Potgieter (2015) as a function of δnote that the dimensions are m^{3}. The value for δ = 1 is just the cosmic ray number density. 

Open with DEXTER  
In the text 
Fig. 4 Local reacceleration power density from Eq. (21), the Vos and Potgieter local interstellar spectrum, V_{A} = 30 km s^{1} and D_{0} = 10^{28} cm^{2} s^{1}. 

Open with DEXTER  
In the text 
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