# Hawking-Unruh Hadronization and  Strangeness Production in High Energy Collisions

Authors: Paolo Castorina; Helmut Satz
Journal: Advances in High Energy Physics
 (2014)

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## Abstract

The thermal multihadron production observed in different high energy collisions poses many basic problems: why do even elementary,e+e- and hadron-hadron, collisions show thermal behaviour? Why is there in such interactions a suppression of strange particle production? Why does the strangeness suppression almost disappear in relativistic heavy ion collisions? Why in these collisions is the thermalization time less than ≃0.5 fm/c? We show that the recently proposed mechanism of thermal hadron production through Hawking-Unruh radiation can naturally answer the previous questions. Indeed, the interpretation of quark (q)-antiquark (q̅) pairs production, by the sequential string breaking, as tunneling through the event horizon of colour confinement leads to thermal behavior with a universal temperature, T≃170 Mev, related to the quark acceleration, a, by T=a/2π. The resulting temperature depends on the quark mass and then on the content of the produced hadrons, causing a deviation from full equilibrium and hence a suppression of strange particle production in elementary collisions. In nucleus-nucleus collisions, where the quark density is much bigger, one has to introduce an average temperature (acceleration) which dilutes the quark mass effect and the strangeness suppression almost disappears.


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## Body

## 1. Introduction

Hadron production in high energy collisions shows remarkably universal thermal features. Ine+e- annihilation [1–3], in pp, in pp- [4], and more general hh interactions [3], as well as in the collisions of heavy nuclei [5–11], over an energy range from around 10 GeV up to the TeV range; the relative abundances of the produced hadrons appear to be those of an ideal hadronic resonance gas at a quite universal temperature TH≈ 160–170 MeV [12].There is, however, one important nonequilibrium effect observed: the production of strange hadrons in elementary collisions is suppressed relative to an overall equilibrium. This is usually taken into account phenomenologically by introducing an overall strangeness suppression factorγs<1 [13], which reduces the predicted abundances by γs,γs2, and γs3 for hadrons containing one, two, or three strange quarks (or antiquarks), respectively. In high energy heavy ion collisions, strangeness suppression becomes less and disappears at high energies [14, 15].The origin of the observed thermal behaviour has been an enigma for many years and there is a still ongoing debate about the interpretation of these results [16–24]. Indeed, in high energy heavy ion collisions multiple parton scattering could lead to kinetic thermalization, but e+e- or elementary hadron interactions do not readily allow such a description.The universality of the observed temperatures, on the other hand, suggests a common origin for all high energy collisions, and it was recently proposed [25] that thermal hadron production is the QCD counterpart of Hawking-Unruh (H-U) radiation [26, 27], emitted at the event horizon due to colour confinement. In the case of approximately massless quarks, the resulting hadronization temperature is determined by the string tension σ, with T≃σ/2π≃170 Mev [25]. Moreover in [28], it has been shown that strangeness suppression in elementary collisions naturally occurs in this framework without requiring a specific suppression factor. The crucial role here is played by the nonnegligible strange quark mass, which modifies the emission temperature for such quarks: in the Hawking-Unruh approach the temperature associated with strange particle production is different from that one of nonstrange particles. Although this conclusion has been obtained by a full analysis in the statistical hadronization model in [28], here we propose an elementary scheme of understanding strangeness suppression which, moreover, opens the possibility of explaining why this suppression disappears in heavy ion collisions where the large parton density in causally connected space-time region of hadronization produces a unique temperature for strange and nonstrange particles.In particular, in the second section, after recalling the statistical hadronization model, one discusses the subsequent description in terms of H-U radiation in QCD, including the dependence of the radiation temperature on the mass of the produced quark and the strangeness suppression in elementary collisions. In Section3 the dynamical mechanism for strangeness enhancement (i.e., no suppression) in relativistic heavy ion scatterings is introduced giving a coarse grain evaluation of the Wroblewski factor [29], a parameter which counts the relative number of strange and nonstrange quarks and antiquarks. Section 4 is devoted to comments and conclusions.


## 2. Hawking-Unruh Hadronization

In this section we will recall the essentials of the statistical hadronization model and of the Hawking-Unruh analysis of the string breaking mechanism. For a detailed descriptions see [3, 25, 28].


### 2.1. Statistical Hadronization Model

The statistical hadronization model assumes that hadronization in high energy collisions is a universal process proceeding through the formation of multiple colourless massive clusters (or fireballs) of finite spacial extension. These clusters are taken to decay into hadrons according to a purely statistical law: every multihadron state of the cluster phase space defined by its mass, volume, and charges is equally probable. The mass distribution and the distribution of charges (electric, baryonic, and strange) among the clusters and their (fluctuating) number are determined in the prior dynamical stage of the process. Once these distributions are known, each cluster can be hadronized on the basis of statistical equilibrium, leading to the calculation of averages in themicrocanonical ensemble, enforcing the exact conservation of energy and charges of each cluster.Hence, in principle, one would need the mentioned dynamical information in order to make definite quantitative predictions to be compared with data. Nevertheless, for Lorentz-invariant quantities such as multiplicities, one can introduce a simplifying assumption and thereby obtain a simple analytical expression in terms of a temperature. The key point is to assume that the distribution of masses and charges among clusters is again purely statistical [3], so that, as far as the calculation of multiplicities is concerned, the set of clusters becomes equivalent, on average, to a large cluster (equivalent global cluster) whose volume is the sum of proper cluster volumes and whose charge is the sum of cluster charges (and thus the conserved charge of the initial colliding system). In such a global averaging process, the equivalent cluster generally turns out to be large enough in mass and volume so that the canonical ensemble becomes a good approximation. In other words, a temperature can be introduced which replaces thea priori more fundamental description in terms of an energy density.To obtain a simple expression for our further discussion, we neglect for the moment an aspect which is important in any actual analysis. Although in elementary collisions the conservation of the various discrete abelian charges (electric charge, baryon number, strangeness, heavy flavour) has to be taken into accountexactly [30], we here consider for the moment a grand-canonical picture. We also assume Boltzmann distributions for all hadrons. The multiplicity of a given scalar hadronic species j then becomes
(1)〈nj〉primary=VTmj22π2γsnjK2(mjT)
with mj denoting its mass and nj the number of strange quarks/antiquarks it contains. Here primary indicates that it gives the number at the hadronisation point, prior to all subsequent resonance decay. The Hankel function K2(x), with K(x)~exp⁡{-x} for large x, gives the Boltzmann factor, while V denotes the overall equivalent cluster volume. In other words, in an analysis of 4π data of elementary collisions, V is the sum of the all cluster volumes at all different rapidities. It thus scales with the overall multiplicity and hence increases with collision energy. A fit of production data based on the statistical hadronisation model thus involves three parameters: the hadronisation temperature T, the strangeness suppression factor γs, and the equivalent global cluster volume V.As previously discussed, at high energy the temperature turns out to be independent of the initial configuration and this result calls for a universal mechanism underlying the hadronization. In the next paragraph we recall the interpretation of the string breaking as QCD H-U radiation.


### 2.2. String Breaking and Event Horizon

Let us outline the thermal hadron production process through H-U radiation for the specific case ofe+e- annihilation (see Figure 1). The separating primary qq- pair excites a further pair q1q-1 from the vacuum, and this pair is in turn pulled apart by the primary constituents. In the process, the q-1 shields the q from its original partner q-, with a new qq-1 string formed. When it is stretched to reach the pair production threshold, a further pair is formed, and so on [31, 32]. Such a pair production mechanism is a special case of H-U radiation [33–37], emitted as hadron q-1q2 when the quark q1 tunnels through its event horizon to become q-2. The corresponding hadron radiation temperature is given by the Unruh form TH=a/2π, where a is the acceleration suffered by the quark q-1 due to the force of the string attaching it to the primary quark Q. This is equivalent to that suffered by quark q2 due to the effective force of the primary antiquark Q-. Hence we have
(2)aq=σwq=σmq2+kq2,
where wq=mq2+kq2 is the effective mass of the produced quark, with mq for the bare quark mass and kq the quark momentum inside the hadronic system q1q-1 or q2q-2. Since the string breaks [25] when it reaches a separation distance
(3)xq≃2σmq2+(πσ2),
the uncertainty relation gives us kq≃1/xq(4)wq=mq2+[σ2(4mq2+2πσ)]
for the effective mass of the quark. The resulting quark-mass dependent Unruh temperature is thus given by
(5)T(qq)≃σ2πwq.
Note that here it is assumed that the quark masses for q1 and q2 are equal. For mq≃0, (5) reduces to
(6)T(00)≃σ2π,
as obtained in [25].Figure 1
String breaking throughqq- pair production.If the produced hadronq-1q2 consists of quarks of different masses, the resulting temperature has to be calculated as an average of the different accelerations involved. For one massless quark (mq≃0) and one of strange quark mass ms, the average acceleration becomes
(7)a-0s=w0a0+wsasw0+ws=2σw0+ws.
From this the Unruh temperature of a strange meson is given by
(8)T(0s)≃σπ(w0+ws),
with w0≃1/2πσ and ws given by (4) with mq=ms. Similarly, we obtain
(9)T(ss)≃σ2πws,
for the temperature of a meson consisting of a strange quark-antiquark pair (ϕ). With σ≃0.2 GeV2, (6) gives  T0≃0.178 GeV. A strange quark mass of 0.1 GeV reduces this to T(0s)≃0.167 GeV and T(ss)≃157MeV, that is, by about 6% and 12%, respectively.The scheme is readily generalized to baryons. The production pattern is illustrated in Figure2 and leads to an average of the accelerations of the quarks involved. We thus have
(10)T(000)=T(0)≃σ2πw0
for nucleons,
(11)T(00s)≃3σ2π(2w0+ws)
for Λ and Σ production,
(12)T(0ss)≃3σ2π(w0+2ws)
for Ξ production, and
(13)T(sss)=T(ss)≃σ2πws
for that of Ω’s. We thus obtain a resonance gas picture with five different hadronization temperatures, as specified by the strangeness content of the hadron in question: T(00)=T(000),T(0s),T(ss)=T(sss),T(00s) and T(0ss).Figure 2
Nucleon formation by string breaking throughqq- pair production.


### 2.3. Strangeness Suppression in Elementary Collisions

In order to evaluate the primary hadron multiplicities, the previous different species-dependent temperatures, fully determined by the string tensionσ and the strange quark mass ms, have been inserted into a complete statistical model calculation [28].Apart from possible variations of the quantities ofσ and ms, the description is thus parameter-free. As illustration, we show in Table 1 the temperatures obtained for σ=0.2 GeV2 and three different strange quark masses. It is seen that in all cases, the temperature for a hadron carrying nonzero strangeness is lower than that of nonstrange hadrons and this leads to an overall strangeness suppression in elementary collisions, in good agreement with data [28], without the introduction of the ad-hoc parameter γs.Table 1
Hadronization temperatures for hadrons of different strangeness content, forms = 0.075, 0.100, 0.125 GeV and σ = 0.2 GeV2.
T
m
s
=
0.075
m
s
=
0.100
m
s
=
0.125
T
(
00
)
0.178
0.178
0.178
T
(
0
s
)
0.172
0.167
0.162
T
(
s
s
)
0.166
0.157
0.148
T
(
000
)
0.178
0.178
0.178
T
(
00
s
)
0.174
0.171
0.167
T
(
0
s
s
)
0.170
0.164
0.157
T
(
s
s
s
)
0.166
0.157
0.148Although a complete statistical hadronization model calculation has been necessary for a detailed comparison with experimental results [28], a rather simple, coarse grain argument can illustrate why a reduction of the H-U temperature for strange particle production reproduces the γs effect.To simplify matters, let us assume that there are only two species: scalar and electrically neutral mesons, “pions” with massmπ, and “kaons” with mass mk and strangeness s=1.According to the statistical model with theγs suppression factor, the ratio Nk/Nπ is obtained by (1) and is given by
(14)NkNπ|γsstat=mk2mπ2γsK2(mk/T)K2(mπ/T)
because there is thermal equilibrium at temperature T.On the other hand, in the H-U based statistical model there is noγs, Tk=T(0s)≠Tπ=T(00)=T and therefore
(15)NkNπ|H-Ustat=mk2mπ2TkTπK2(mk/Tk)K2(mπ/Tπ).
Which corresponds to a γs parameter given by
(16)γs=TkTπK2(mk/Tk)K2(mk/Tπ).
For σ=0.2 GeV2, ms=0.1 GeV, Tπ=178 Mev, and Tk=167 Mev (see Table 1), the crude evaluation by (16) gives γs≃0.73.In conclusion, our picture implies that the produced hadrons are emitted slightly “out of equilibrium,” in the sense that the emission temperatures are not identical. As long as there is no final state interference between the produced quarks or hadrons, we expect to observe this difference and hence a modification of the production of strange hadrons, in comparison to the corresponding full equilibrium values.Once such interference becomes likely, due to the increases of parton density, as in high energy heavy ion collisions, equilibrium can be essentially restored producing a small strangeness suppression as we will discuss in the next section.


## 2.1. Statistical Hadronization Model

The statistical hadronization model assumes that hadronization in high energy collisions is a universal process proceeding through the formation of multiple colourless massive clusters (or fireballs) of finite spacial extension. These clusters are taken to decay into hadrons according to a purely statistical law: every multihadron state of the cluster phase space defined by its mass, volume, and charges is equally probable. The mass distribution and the distribution of charges (electric, baryonic, and strange) among the clusters and their (fluctuating) number are determined in the prior dynamical stage of the process. Once these distributions are known, each cluster can be hadronized on the basis of statistical equilibrium, leading to the calculation of averages in themicrocanonical ensemble, enforcing the exact conservation of energy and charges of each cluster.Hence, in principle, one would need the mentioned dynamical information in order to make definite quantitative predictions to be compared with data. Nevertheless, for Lorentz-invariant quantities such as multiplicities, one can introduce a simplifying assumption and thereby obtain a simple analytical expression in terms of a temperature. The key point is to assume that the distribution of masses and charges among clusters is again purely statistical [3], so that, as far as the calculation of multiplicities is concerned, the set of clusters becomes equivalent, on average, to a large cluster (equivalent global cluster) whose volume is the sum of proper cluster volumes and whose charge is the sum of cluster charges (and thus the conserved charge of the initial colliding system). In such a global averaging process, the equivalent cluster generally turns out to be large enough in mass and volume so that the canonical ensemble becomes a good approximation. In other words, a temperature can be introduced which replaces thea priori more fundamental description in terms of an energy density.To obtain a simple expression for our further discussion, we neglect for the moment an aspect which is important in any actual analysis. Although in elementary collisions the conservation of the various discrete abelian charges (electric charge, baryon number, strangeness, heavy flavour) has to be taken into accountexactly [30], we here consider for the moment a grand-canonical picture. We also assume Boltzmann distributions for all hadrons. The multiplicity of a given scalar hadronic species j then becomes
(1)〈nj〉primary=VTmj22π2γsnjK2(mjT)
with mj denoting its mass and nj the number of strange quarks/antiquarks it contains. Here primary indicates that it gives the number at the hadronisation point, prior to all subsequent resonance decay. The Hankel function K2(x), with K(x)~exp⁡{-x} for large x, gives the Boltzmann factor, while V denotes the overall equivalent cluster volume. In other words, in an analysis of 4π data of elementary collisions, V is the sum of the all cluster volumes at all different rapidities. It thus scales with the overall multiplicity and hence increases with collision energy. A fit of production data based on the statistical hadronisation model thus involves three parameters: the hadronisation temperature T, the strangeness suppression factor γs, and the equivalent global cluster volume V.As previously discussed, at high energy the temperature turns out to be independent of the initial configuration and this result calls for a universal mechanism underlying the hadronization. In the next paragraph we recall the interpretation of the string breaking as QCD H-U radiation.


## 2.2. String Breaking and Event Horizon

Let us outline the thermal hadron production process through H-U radiation for the specific case ofe+e- annihilation (see Figure 1). The separating primary qq- pair excites a further pair q1q-1 from the vacuum, and this pair is in turn pulled apart by the primary constituents. In the process, the q-1 shields the q from its original partner q-, with a new qq-1 string formed. When it is stretched to reach the pair production threshold, a further pair is formed, and so on [31, 32]. Such a pair production mechanism is a special case of H-U radiation [33–37], emitted as hadron q-1q2 when the quark q1 tunnels through its event horizon to become q-2. The corresponding hadron radiation temperature is given by the Unruh form TH=a/2π, where a is the acceleration suffered by the quark q-1 due to the force of the string attaching it to the primary quark Q. This is equivalent to that suffered by quark q2 due to the effective force of the primary antiquark Q-. Hence we have
(2)aq=σwq=σmq2+kq2,
where wq=mq2+kq2 is the effective mass of the produced quark, with mq for the bare quark mass and kq the quark momentum inside the hadronic system q1q-1 or q2q-2. Since the string breaks [25] when it reaches a separation distance
(3)xq≃2σmq2+(πσ2),
the uncertainty relation gives us kq≃1/xq(4)wq=mq2+[σ2(4mq2+2πσ)]
for the effective mass of the quark. The resulting quark-mass dependent Unruh temperature is thus given by
(5)T(qq)≃σ2πwq.
Note that here it is assumed that the quark masses for q1 and q2 are equal. For mq≃0, (5) reduces to
(6)T(00)≃σ2π,
as obtained in [25].Figure 1
String breaking throughqq- pair production.If the produced hadronq-1q2 consists of quarks of different masses, the resulting temperature has to be calculated as an average of the different accelerations involved. For one massless quark (mq≃0) and one of strange quark mass ms, the average acceleration becomes
(7)a-0s=w0a0+wsasw0+ws=2σw0+ws.
From this the Unruh temperature of a strange meson is given by
(8)T(0s)≃σπ(w0+ws),
with w0≃1/2πσ and ws given by (4) with mq=ms. Similarly, we obtain
(9)T(ss)≃σ2πws,
for the temperature of a meson consisting of a strange quark-antiquark pair (ϕ). With σ≃0.2 GeV2, (6) gives  T0≃0.178 GeV. A strange quark mass of 0.1 GeV reduces this to T(0s)≃0.167 GeV and T(ss)≃157MeV, that is, by about 6% and 12%, respectively.The scheme is readily generalized to baryons. The production pattern is illustrated in Figure2 and leads to an average of the accelerations of the quarks involved. We thus have
(10)T(000)=T(0)≃σ2πw0
for nucleons,
(11)T(00s)≃3σ2π(2w0+ws)
for Λ and Σ production,
(12)T(0ss)≃3σ2π(w0+2ws)
for Ξ production, and
(13)T(sss)=T(ss)≃σ2πws
for that of Ω’s. We thus obtain a resonance gas picture with five different hadronization temperatures, as specified by the strangeness content of the hadron in question: T(00)=T(000),T(0s),T(ss)=T(sss),T(00s) and T(0ss).Figure 2
Nucleon formation by string breaking throughqq- pair production.


## 2.3. Strangeness Suppression in Elementary Collisions

In order to evaluate the primary hadron multiplicities, the previous different species-dependent temperatures, fully determined by the string tensionσ and the strange quark mass ms, have been inserted into a complete statistical model calculation [28].Apart from possible variations of the quantities ofσ and ms, the description is thus parameter-free. As illustration, we show in Table 1 the temperatures obtained for σ=0.2 GeV2 and three different strange quark masses. It is seen that in all cases, the temperature for a hadron carrying nonzero strangeness is lower than that of nonstrange hadrons and this leads to an overall strangeness suppression in elementary collisions, in good agreement with data [28], without the introduction of the ad-hoc parameter γs.Table 1
Hadronization temperatures for hadrons of different strangeness content, forms = 0.075, 0.100, 0.125 GeV and σ = 0.2 GeV2.
T
m
s
=
0.075
m
s
=
0.100
m
s
=
0.125
T
(
00
)
0.178
0.178
0.178
T
(
0
s
)
0.172
0.167
0.162
T
(
s
s
)
0.166
0.157
0.148
T
(
000
)
0.178
0.178
0.178
T
(
00
s
)
0.174
0.171
0.167
T
(
0
s
s
)
0.170
0.164
0.157
T
(
s
s
s
)
0.166
0.157
0.148Although a complete statistical hadronization model calculation has been necessary for a detailed comparison with experimental results [28], a rather simple, coarse grain argument can illustrate why a reduction of the H-U temperature for strange particle production reproduces the γs effect.To simplify matters, let us assume that there are only two species: scalar and electrically neutral mesons, “pions” with massmπ, and “kaons” with mass mk and strangeness s=1.According to the statistical model with theγs suppression factor, the ratio Nk/Nπ is obtained by (1) and is given by
(14)NkNπ|γsstat=mk2mπ2γsK2(mk/T)K2(mπ/T)
because there is thermal equilibrium at temperature T.On the other hand, in the H-U based statistical model there is noγs, Tk=T(0s)≠Tπ=T(00)=T and therefore
(15)NkNπ|H-Ustat=mk2mπ2TkTπK2(mk/Tk)K2(mπ/Tπ).
Which corresponds to a γs parameter given by
(16)γs=TkTπK2(mk/Tk)K2(mk/Tπ).
For σ=0.2 GeV2, ms=0.1 GeV, Tπ=178 Mev, and Tk=167 Mev (see Table 1), the crude evaluation by (16) gives γs≃0.73.In conclusion, our picture implies that the produced hadrons are emitted slightly “out of equilibrium,” in the sense that the emission temperatures are not identical. As long as there is no final state interference between the produced quarks or hadrons, we expect to observe this difference and hence a modification of the production of strange hadrons, in comparison to the corresponding full equilibrium values.Once such interference becomes likely, due to the increases of parton density, as in high energy heavy ion collisions, equilibrium can be essentially restored producing a small strangeness suppression as we will discuss in the next section.


## 3. Hawking-Unruh Strangeness Enhancement in Heavy Ion Collisions

As previosuly discussed, in elementary collisions the production of hadrons containingn strange quarks or antiquarks is reduced in comparison to nucleus-nucleus scattering and this reduction can be accounted for by the introduction of the phenomenological universal strangeness suppression factor γsn.However, the hadron production in high energy collisions occurs in a number of causally disconnected regions of finite space-time size [38]. As a result, globally conserved quantum numbers (charge, strangeness, and baryon number) must be conserved locally in spatially restricted correlation clusters. This provides a dynamical basis for understanding the suppression of strangeness production in elementary interactions (pp, e+e-) due to a small strangeness correlation volume [11, 30, 39, 40].The H-U counterpart of this mechanism is that in elementary collisions there is a small number of partons in a causally connected region and the hadron production comes from the sequential breaking of independentqq- strings with the consequent species-dependent temperatures which reproduce the strangeness suppression.In contrast, the space-time superposition of many collisions in heavy ion interactions largely removes these causality constraints [38], resulting in an ideal hadronic resonance gas in full equilibrium.In the H-U approach, the effect of a large number of causally connected quarks and antiquarks can be implemented by defining the average temperature of the system and determining the hadron multiplicities by the statistical model with this “equilibrium” temperature.Indeed, the average temperature depends on the numbers of light quarks,Nl, and of strange quarks, Ns, which, in turn, are counted by the number of strange and nonstrange hadrons in the final state at that temperature.A detailed analysis requires again a full calculation in the statistical model that will be done in a forthcoming paper; however the mechanism can be roughly illustrated in the world of “pions” and “kaons” introduced in Section2.Let us consider a high density system of quarks and antiquarks in a causally connected region. Generalizing our formulas in Section2, the average acceleration is given by
(17)a-=Nlw0a0+NswsasNlw0+Nsws.
By assuming Nl≫Ns, by ((6)–(8)), after a simple algebra, the average temperature, T-=a-/2π, turns out to be
(18)T-=T(00)[1-NsNlw0+wsw0(1-T(0s)T(00))]+O[(NsNl)2].
Now in our world of “pions” and “kaons” one has Nl=2Nπ+Nk and Ns=Nk and therefore
(19)T-=T(00)[1-Nk2Nπw0+wsw0(1-T(0s)T(00))]+O[(NkNπ)2].
On the other hand, in the H-U based statistical calculation the ratio Nk/Nπ depends on the equilibrium (average) temperature T-; that is,
(20)NkNπ=mk2mπ2K2(mk/T-)K2(mπ/T-),
and, therefore, one has to determine the temperature T- in such a way that (19) and (20) are self-consistent. This condition implies the equation
(21)2[1-T-/T(00)]w0[1-T(0s)/T(00)](ws+w0)=mk2mπ2K2(mk/T-)K2(mπ/T-),
that can be solved numerically.Forσ=0.2 GeV2, ms=0.1, and the temperatures in Table 1, the average temperature turns out T-=174 Mev and one can evaluate the Wroblewski factor defined by
(22)λ=2NsNl,
where Ns is the number of strange and antistrange quarks in the hadrons in the final state and Nl is the number of light quarks and antiquarks in the final state minus their number in the initial configuration.The experimental value of the Wroblewski factor in high energy collisions is rather independent on the energy and is aboutλ≃0.26 in elementary collisions and λ≃0.5 for nucleus-nucleus scattering.In our simplified world, fore+e- annhilation, λ=Nk/Nπ and is given by (15) with the species-dependent temperatures in Table 1. One gets λ≃0.26.To evaluate the Wroblewski factor in nucleus-nucleus collisions one has to consider the average “equilibrium” temperatureT- and the number of light quarks in the initial configuration. The latter point requires a realistic calculation in the statitical model which includes all resonances and stable particles.However to show that one is on the right track, let us neglect the problem of the initial configurationa and let us evaluate the effect of substituting in (15) the species-dependent temperatures with the equilibrium temperature T-. With this simple modification the Wroblewski factor increases, λ=0.33.In other terms, the change from a nonequilibrium condition, with species-dependent temperatures, to an equilibrated system with the average temperatureT- is able to reproduce part of the observed growing of the number of strange quarks with respect to elementary interactions.


## 4. Conclusions and Comments

The Hawking-Unruh hadronization mechanism gives a dynamical basis to the universality of the temperature obtained in the statistical model, to the strangeness suppression in elementary collisions and to its enhancement in nucleus-nucleus scatterings.We are aware that the simplified formulation in Section3 has to be checked by a full analysis in the hadron resonance gas framework or by montecarlo simulations and that, in addition, the interpretation of production of charmed hadrons in e+e- annihilations, which is very successfully described by the hadron resonance gas model with an exact charm conservation, should be addressed through Hawking-Unruh radiation mechanism to check if there is a consistent picture.However the proposed approach is also able to understand the extremely fast equilibration of hadronic matter. Indeed, Hawking-Unruh radiation provides a stochastic rather than kinetic approach to equilibrium, with a randomization essentially due to the quantum physics of the color horizon. The barrier to information transfer due to the event horizon requires that the resulting radiation states excited from the vacuum be distributed according to maximum entropy, with a temperature determined by the strength of the confining field.The ensemble of all produced hadrons, averaged over all events, then leads to the same equilibrium distribution as obtained in hadronic matter by kinetic equilibration. In the case of a very high energy collision with a high average multiplicity already one event can provide such equilibrium; because of the interruption of information transfer at each of the successive quantum color horizons, there is no phase relation between two successive production steps in a given event. The destruction of memory, which in kinetic equilibration is achieved through sufficiently many successive collisions, is here automatically provided by the tunnelling process. So the thermal hadronic final state in high energy collisions is obtained through a stochastic process.Finally, high energy particle physics, and in particular hadron production, is, in our opinion, the promising sector to find the analogue of the Hawking-Unruh radiation for two main reasons: color confinement and the huge acceleration that cannot be reached in any other dynamical systems.



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*Source: 376982-2014-05-11.xml*