An Improved Core-Corona Model for Λ and Λ Polarization in Relativistic Heavy-Ion Collisions

Abstract

Due to its sensitivity to the dynamics of strongly interacting matter subject to extreme conditions, hyperon global polarization has become an important observable to study the system created in relativistic heavy-ion collisions. Recently, the STAR and HADES collaborations have measured the global polarization of both $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$ produced in semi-central collisions in a wide range of collision energies. The polarization excitation functions show an increasing trend as the collision energy decreases, with the increase being more pronounced for the $\overline{\mathrm{\Lambda }}$. In this work, we make a summary of a core-corona model that we have developed to quantify the global polarization contributions from $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$ created in different regions of the fireball. The core-corona model assumes that $\mathrm{\Lambda }$s and $\overline{\mathrm{\Lambda }}$s are produced in both regions, the high-density core and the lower density corona, with different relative abundances which modulate the polarization excitation function. We have shown that the model works well for the description of experimental results. The global polarization excitation functions computed with the model show a peak at different collision energies in the region $\sqrt{s_{NN}}\le 10$ GeV. Finally, we discuss and report on the model global polarization predictions for BES-II, NICA and CBM at FAIR and HADES energies.

1. Introduction

The global polarization of hyperons has recently gained great interest given its sensitivity to study aspects of the strongly interacting matter created in heavy-ion collisions such as vorticity, viscosity and flow. It can also provide information about the onset of criticality in the phase diagram [1,2,3,4,5,6,7,8,9,10,11,12,13]. In a non-central collision, the system acquires a large angular momentum along the direction of the transverse plane. This angular momentum can be quantified in terms of the thermal vorticity, which could be partially transferred to the spin degrees of freedom of particles created in the collision. The self-analysing properties of $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$ particles through their charged decay are useful to measure this global polarization. Recently, the STAR-BES and HADES collaborations measured the $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$ global polarizations for different collision energies [14,15,16,17]. These measurements show several interesting features: the polarizations increase as the energy of the collision decreases, and the increase is more pronounced for the $\overline{\mathrm{\Lambda }}$. The polarizations show what seem to be maximum values close to the $\mathrm{\Lambda }$ production threshold energy in pp collisions which then decrease for lower energies. The system created at BES-I energies is dominated by a QGP phase, so the global polarization at these energies is understood as a mechanism where this highly vortical fluid modifies the spin properties of hadrons produced at later stages. In systems created at lower energies, the QGP phase coexists with a baryon rich environment, so the polarization mechanism could be driven mainly by baryon dominated processes. Understanding the subtleties of the different mechanisms, by which global polarization is transferred to hyperons at BES-II, HADES, CBM at FAIR and NICA energies, can provide another important tool to pinpoint the critical phenomena expected to emerge at these energies. In order to contribute to this effort, we have developed a core-corona model [18,19,20,21,22]. In this contribution, we summarize the main components of this model, and we compare its predictions for $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$ global polarization with experimental data at BES-II and HADES energies. We show that the model works well in the description of experimental results. We predict the presence of a maximum for each of the global polarizations at different collision energies in the region $\sqrt{s_{NN}}\le 10$ GeV. Finally, we comment on current progress for the core-corona model improvement and the feasibility of global polarization measurements at NICA, HADES and CBM at FAIR energies.

2. A Core-Corona Model for $\mathrm{\Lambda }/\overline{\mathrm{\Lambda }}$ Polarization

In the core-corona model, the system is assumed to be formed with distinct density regions, as sketched in Figure 1. The overlap of the two colliding ions consists of a core in the central part and a corona in the periphery. We model the core as a region with a high enough density of participants to create a thermalized QGP fireball, while in the corona the interactions are more like those in pp collisions. Consequently, the particles that come from each region have different characteristics due to their different hadronisation mechanisms, by QGP or recombination processes, and interaction with the surrounding environment. We expect that observables, such as the polarization, will show a dependence not only in the collision energy and/or centrality, but also in the relative abundances of particles coming from the core and the corona, and its polarization mechanism associated with each region.

In the core-corona scenario, the $\mathrm{\Lambda }$ average global polarization, ${\mathcal{P}}^{\mathrm{\Lambda }}$, is defined as

$${\mathcal{P}}^{\mathrm{\Lambda }}=\frac{(N_{\mathrm{\Lambda }QGP}^{\uparrow }+N_{\mathrm{\Lambda }REC}^{\uparrow })-(N_{\mathrm{\Lambda }QGP}^{\downarrow }+N_{\mathrm{\Lambda }REC}^{\downarrow })}{(N_{\mathrm{\Lambda }QGP}^{\uparrow }+N_{\mathrm{\Lambda }REC}^{\uparrow })+(N_{\mathrm{\Lambda }QGP}^{\downarrow }+N_{\mathrm{\Lambda }REC}^{\downarrow })},$$

(1)

and, similarly for the $\overline{\mathrm{\Lambda }}$ average global polarization, ${\mathcal{P}}^{\overline{\mathrm{\Lambda }}}$, is given by

$${\mathcal{P}}^{\overline{\mathrm{\Lambda }}}=\frac{(N_{\overline{\mathrm{\Lambda }}QGP}^{\uparrow }+N_{\overline{\mathrm{\Lambda }}REC}^{\uparrow })-(N_{\overline{\mathrm{\Lambda }}QGP}^{\downarrow }+N_{\overline{\mathrm{\Lambda }}REC}^{\downarrow })}{(N_{\overline{\mathrm{\Lambda }}QGP}^{\uparrow }+N_{\overline{\mathrm{\Lambda }}REC}^{\uparrow })+(N_{\overline{\mathrm{\Lambda }}QGP}^{\downarrow }+N_{\overline{\mathrm{\Lambda }}REC}^{\downarrow })},$$

(2)

the ratio of the difference between the number of particles with their spin pointing along (up arrow) and opposite (down arrow) to a given direction, to their sum. In both Equations (1) and (2), we have used the total number of $\mathrm{\Lambda }$s ($\overline{\mathrm{\Lambda }}$s), and $N_{\mathrm{\Lambda }}=N_{\mathrm{\Lambda }QGP}+N_{\mathrm{\Lambda }REC}$ ($N_{\overline{\mathrm{\Lambda }}}=N_{\overline{\mathrm{\Lambda }}QGP}+N_{\overline{\mathrm{\Lambda }}REC}$) is given as the sum of the number of $\mathrm{\Lambda }$s ($\overline{\mathrm{\Lambda }}$s) coming from the core $N_{\mathrm{\Lambda }QGP}$ ($N_{\overline{\mathrm{\Lambda }}QGP}$) and the number of $\mathrm{\Lambda }$s ($\overline{\mathrm{\Lambda }}$s) coming from the corona, $N_{\mathrm{\Lambda }REC}$ ($N_{\overline{\mathrm{\Lambda }}REC}$). Throughout this manuscript, the subscripts QGP and REC refer to the type of hadronisation mechanism involved in each region, by a coalescence-type of processes in the QGP, in the core and recombination of a di-quark(antiquark) with an s-quark(antiquark) as in pp collisions in the corona, respectively.

Next, we define the intrinsic polarization of $\mathrm{\Lambda }$s and $\overline{\mathrm{\Lambda }}$s coming from the core as

$$z=\frac{N_{\mathrm{\Lambda }QGP}^{\uparrow }-N_{\mathrm{\Lambda }QGP}^{\downarrow }}{N_{\mathrm{\Lambda }QGP}}\mathrm{and}\overline{z}=\frac{N_{\overline{\mathrm{\Lambda }}QGP}^{\uparrow }-N_{\overline{\mathrm{\Lambda }}QGP}^{\downarrow }}{N_{\overline{\mathrm{\Lambda }}QGP}},$$

(3)

which helps to highlight the importance of the relative number of each kind of hyperon with spin aligned in opposite directions in each region, with respect to the total number of hyperons in that same region. Analogously, we identify the contribution to the global polarization from the corona as

$${\mathcal{P}}_{REC}^{\mathrm{\Lambda }}=\frac{N_{\mathrm{\Lambda }REC}^{\uparrow }-N_{\mathrm{\Lambda }REC}^{\downarrow }}{N_{\mathrm{\Lambda }REC}}\mathrm{and}{\mathcal{P}}_{REC}^{\overline{\mathrm{\Lambda }}}=\frac{N_{\overline{\mathrm{\Lambda }}REC}^{\uparrow }-N_{\overline{\mathrm{\Lambda }}REC}^{\downarrow }}{N_{\overline{\mathrm{\Lambda }}REC}}.$$

(4)

We can now rewrite the average global polarization ${\mathcal{P}}^{\mathrm{\Lambda }}$ and ${\mathcal{P}}^{\overline{\mathrm{\Lambda }}}$ from Equations (1) and (2) as

$${\mathcal{P}}^{\mathrm{\Lambda }}=\frac{{\mathcal{P}}_{REC}^{\mathrm{\Lambda }}+z\frac{N_{\mathrm{\Lambda }QGP}}{N_{\mathrm{\Lambda }REC}}}{1+\frac{N_{\mathrm{\Lambda }QGP}}{N_{\mathrm{\Lambda }REC}}},{\mathcal{P}}^{\overline{\mathrm{\Lambda }}}=\frac{{\mathcal{P}}_{REC}^{\overline{\mathrm{\Lambda }}}+\overline{z}\left(\frac{w^{\prime }}{w}\right)\frac{N_{\mathrm{\Lambda }QGP}}{N_{\mathrm{\Lambda }REC}}}{1+\left(\frac{w^{\prime }}{w}\right)\frac{N_{\mathrm{\Lambda }QGP}}{N_{\mathrm{\Lambda }REC}}},$$

(5)

where the ratios $w^{\prime }=N_{\overline{\mathrm{\Lambda }}QGP}/N_{\mathrm{\Lambda }QGP}$ and $w=N_{\overline{\mathrm{\Lambda }}REC}/N_{\mathrm{\Lambda }REC}$ control the antiparticle to particle relative abundances within the same region. Equation (5) shows that the $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$ polarizations are governed by z, $\overline{z}$, ${\mathcal{P}}_{REC}^{\mathrm{\Lambda }}$, ${\mathcal{P}}_{REC}^{\overline{\mathrm{\Lambda }}}$, w, $w^{\prime }$, and the ratio $N_{\mathrm{\Lambda }QGP}/N_{\mathrm{\Lambda }REC}$. The dependence of these variables, with respect to collision energy and centrality, can be determined either from calculations or from experimental data. In the Appendix A, Appendix Band Appendix C, we provide a brief summary of the procedures to fix w, $w^{\prime }$, and the ratio $N_{\mathrm{\Lambda }QGP}/N_{\mathrm{\Lambda }REC}$, respectively.

3. $\mathrm{\Lambda }$ ($\overline{\mathrm{\Lambda }}$) Intrinsic Polarization z ($\overline{z}$)

In order to calculate the intrinsic global $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$ polarizations from the core, we assume that the s- and $\overline{s}$-quark polarizations, z and $\overline{z}$, respectively, translate into the $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$ polarizations during the hadronisation process. This allows us to express the intrinsic polarization z (or $\overline{z}$) in terms of the relaxation time $\tau$(or $\overline{\tau }$), that is, the time required by the corresponding quark to align its spin with the thermal vorticity $\omega$, as a function of the QGP lifetime, $\Delta {\tau }_{QGP}$ [23],

$$\begin{array}{ccc}\hfill z& =& 1-e^{-\Delta {\tau }_{QGP}/\tau },\hfill \\ \hfill \overline{z}& =& 1-e^{-\Delta {\tau }_{QGP}/\overline{\tau }}.\hfill \end{array}$$

(6)

$\tau$ (or $\overline{\tau }$) is computed as the inverse of the total interaction rate $\tau \equiv 1/\Gamma$. The interaction rate is obtained from the imaginary part of the self-energy $\Sigma$ of a quark with four-momentum $P=(p_0,\overrightarrow{p})$ as

$$\Gamma \left(p_0\right)=\tilde{f}\left(p_0\right)\mathrm{Tr}[{\gamma }^0\mathrm{Im}\Sigma ]$$

(7)

where $\tilde{f}\left(p_0\right)$ is the Fermi–Dirac distribution. The interaction between the spin and the thermal vorticity $\omega$ is modeled within the medium by means of a vertex coupling quarks and thermal gluons, as depicted in Figure 2.

Equation (7) can be rewritten as [23]

$$\begin{array}{ccc}\hfill \Gamma \left(p_0\right)& =& \frac{{\alpha }_s}{4\pi }{\left(\frac{\omega }{T}\right)}^2\frac{C_F}{\sqrt{p_0^2-m_q^2}}{\int }_0^{\infty }dkk{\int }_{\mathcal{R}}d{k}_0[1+f\left(k_0\right)]\hfill \\ & & \times \tilde{f}(p_0+k_0-{\mu }_q)\sum _{i=L,T}{C}_i(p0,k_0,k){\rho }_i(k_0,k),\hfill \end{array}$$

(8)

where the integral is performed over the kinematically available region, weighted with the statistical distributions, Bose-Einstein f for gluons and Fermi–Dirac $\tilde{f}$ for quarks. The temperature T is the ${\mu }_B$-dependent freeze-out temperature. These quantities are explicitly given in Appendix B. The thermal vorticity $\omega$ is computed from the initial angular vorticity of events simulated with UrQMD [24,25]. $C_i$ with $i=T,L$ are the result of the trace calculation after contraction of the transverse and longitudinal projection operators that come together with the gluon spectral functions ${\rho }_i$, the quark propagator and the vertices, after summing over the Matsubara frequencies.

The total interaction rate is obtained by integrating over the available phase space

$$\Gamma =V\int \frac{d^{3}p}{{\left(2\pi \right)}^3}\Gamma \left(p_0\right),$$

(9)

where V is the volume of the core region.

The volume of the core is computed as $V=\pi R^2\Delta {\tau }_{QGP}$, which depends on the collision energy as well as on the QGP life-time

$$\Delta {\tau }_{QGP}=Aln\sqrt{s_{NN}}$$

(10)

with $A=0.6803\pm 0.05509,1.116\pm 0.09444$. This parametrization is obtained from the fit to the experimental distribution calculated with $\Delta {\tau }_{QGP}={\tau }_f-{\tau }_0={\tau }_0[{\left(\frac{T_0}{T_f}\right)}^3-1]$ where we assumed a Bjorken expansion in which the elapsed time between the initial formation ${\tau }_0$ and the hadronisation ${\tau }_f$ times is related with the corresponding temperatures $T_0$ and $T_f$.

The initial temperature is extracted from experimental data from transverse momentum distributions of $\varphi$ mesons, whereas the final temperature corresponds to the temperature along the chemical freeze-out curve, given in Appendix B. We choose ${\tau }_0=0.35,0.60$ fm to fit the different centrality data.

The intrinsic polarization obtained for collisions at $b=7.26$ fm is shown in Figure 3.

4. Polarization in the Corona ${\mathcal{P}}_{REC}^{\mathrm{\Lambda }}$ (${\mathcal{P}}_{REC}^{\overline{\mathrm{\Lambda }}}$)

As a first approach, we set ${\mathcal{P}}_{REC}^{\mathrm{\Lambda }}={\mathcal{P}}_{REC}^{\overline{\mathrm{\Lambda }}}=0$, given that, in cold nuclear matter, reactions are less efficient at aligning the spin in the direction of the angular momentum than in the QGP. We can describe the main characteristics of the excitation functions in terms of the ratios $N_{\mathrm{\Lambda }QGP}/N_{\mathrm{\Lambda }REC}$ ($N_{\overline{\mathrm{\Lambda }}QGP}/N_{\overline{\mathrm{\Lambda }}REC}$) and $1/(1+N_{\mathrm{\Lambda }QGP}/N_{\mathrm{\Lambda }REC})$ ($1/(1+N_{\overline{\mathrm{\Lambda }}QGP}/N_{\overline{\mathrm{\Lambda }}REC})$). In central collisions, particle production is dominated by the core region, but as the collision becomes more peripheral, this behaviour reverses. For mid-central collisions, we find that the ratio $N_{\mathrm{\Lambda }QGP}/N_{\mathrm{\Lambda }REC}$ is smaller than one. It decreases monotonically with the collision energy. On the other hand, the ratio $1/(1+N_{\mathrm{\Lambda }QGP}/N_{\mathrm{\Lambda }REC})$ monotonically increases with the collision energy. We notice that the excitation functions peak near where these ratios cross, as shown in Figure 4; the green line, corresponding to ${\mathcal{P}}^{\mathrm{\Lambda }}$, peaks at $\sqrt{s_{NN}}\approx 3$ GeV, where the ratios $N_{\mathrm{\Lambda }QGP}/N_{\mathrm{\Lambda }REC}$ (purple line) and $1/(1+N_{\mathrm{\Lambda }QGP}/N_{\mathrm{\Lambda }REC})$ (blue line) cross. In a similar manner ${\mathcal{P}}^{\overline{\mathrm{\Lambda }}}$, in orange, peaks at $\sqrt{s_{NN}}\approx 6-8$ GeV, where the ratios $N_{\overline{\mathrm{\Lambda }}QGP}/N_{\overline{\mathrm{\Lambda }}REC}$ and $1/(1+N_{\overline{\mathrm{\Lambda }}QGP}/N_{\overline{\mathrm{\Lambda }}REC})$ (not shown in the figure) cross. In the case of $\overline{\mathrm{\Lambda }}$, this function peaks at a higher collision energy, resulting in a larger polarization than that for the $\mathrm{\Lambda }$s for $\sqrt{s_{NN}}\gtrsim 4$ GeV. This is consistent with experimental data reported by STAR [14]. We could have expected that the $\overline{\mathrm{\Lambda }}$ polarization is smaller than the $\mathrm{\Lambda }$ polarization since $\overline{z}<z$, as shown in Figure 3. However, this is not the case, as we show in Ref. [18]; the interplay between the factor $w^{\prime }/w>1$ (or $w/w^{\prime }<1$) and the ratio $N_{\mathrm{\Lambda }QGP}/N_{\mathrm{\Lambda }REC}<1$ amplifies the polarization, producing that ${\mathcal{P}}^{\mathrm{\Lambda }}<{\mathcal{P}}^{\overline{\mathrm{\Lambda }}}$. As is shown in the left panel of Figure 5, the ratio ${\mathcal{P}}^{\overline{\mathrm{\Lambda }}}/{\mathcal{P}}^{\mathrm{\Lambda }}$ increases as $w/w^{\prime }$ decreases. In the uttermost case in which $z=\overline{z}$ and $N_{\mathrm{\Lambda }REC}=N_{\mathrm{\Lambda }QGP}$, ${\mathcal{P}}^{\overline{\mathrm{\Lambda }}}$ is always larger than ${\mathcal{P}}^{\mathrm{\Lambda }}$ for $w/w^{\prime }<1$. However, for values close to those in mid-central an peripheral collisions, for which $N_{\mathrm{\Lambda }QGP}$ becomes smaller than $N_{\mathrm{\Lambda }REC}$ and $\overline{z}$ is smaller than z (Figure 3), the ratio ${\mathcal{P}}^{\overline{\mathrm{\Lambda }}}/{\mathcal{P}}^{\mathrm{\Lambda }}$ is still larger than 1 for small enough values of the ratio $w/w^{\prime }\lesssim 0.1$, which are reached for $\sqrt{s_{NN}}<10$ GeV. This is shown in the right panel of Figure 5. The explicit expressions for w and $w^{\prime }$ are shown in Appendices Appendix A and Appendix B, respectively.

5. Results

We can now use Equation (5) and the results in the appendices to calculate the global $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$ polarizations as functions of the collision energy. This is shown in Figure 6.

To compare with the STAR-BES data [14,15,16], we compute the number of $\mathrm{\Lambda }$s and $\overline{\mathrm{\Lambda }}$s, using the expressions in Appendix C, considering the impact parameter interval $b\in (6.66,10.52)$ fm, which corresponds to the centrality range 20–50%, the scaling constant between the number of $N_{\mathrm{\Lambda }QGP}$ created and the $N_{\mathrm{p}QGP}$ number of participants in the collision, $c=0.0025$, and the radius and skin depth of a gold ion, $R_{Au}=6.554$ fm and $a=0.523$ fm, respectively.

The shaded areas in Figure 6 correspond to the regions delimited by fits to the QGP lifetime and volume from Equation (10), used to evaluate the intrinsic polarizations z and $\overline{z}$ considering the thermal vorticity (in Equation (8)) at the corresponding average impact parameter $\langle b\rangle =8.73$ fm.

Notice that the model calculation gives a good description of experimental data. The difference between the model and HADES data are due to the different centrality intervals. Recall that the magnitude of the polarization decreases for more central collisions, as a consequence of a smaller system vorticity. The maximum of the $\mathrm{\Lambda }$ polarization is close to its production threshold energy in the $pp\to \mathrm{\Lambda }+K^{-}+p$ channel, while the $\overline{\mathrm{\Lambda }}$ maximum spreads over an interval that in the model depends on the $w^{\prime }/w$ ratio.

6. Discussion

We have shown that the core-corona model is successful in describing the general features of the average global polarization measurements for both $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$. However, the model has limitations for the description of $\mathrm{\Lambda }$ polarization of smaller colliding systems such as Ag + Ag at $\sqrt{s_{NN}}=2.55$ GeV in the 10–40% centrality class, or for large systems such as Au + Au at small collision energies such as $\sqrt{s_{NN}}=3$ GeV for centralities larger than 40%. For these conditions, $\mathrm{\Lambda }$s and $\overline{\mathrm{\Lambda }}$s in the core are barely produced (see Appendix C), resulting in polarizations that tend to zero. Now, to improve our study, we remove the assumption that the polarization of $\mathrm{\Lambda }$s produced in the corona is negligible, and so now ${\mathcal{P}}_{REC}^{\mathrm{\Lambda }}\ne 0$ (in the case of $\overline{\mathrm{\Lambda }}$, there is no available data at those energies). In fact, from existing data, we know that the contribution can be significant for mid-central or peripheral collisions where $N_{\mathrm{\Lambda }QGP}/N_{\mathrm{\Lambda }REC}\to 0$, and particle production is mainly by pp interactions. In this type of reaction, the transverse polarization does not vanish and the mean polarization in the energy range $\sqrt{s_{NN}}$ = 10–63 GeV reaches values of $\mathcal{P}=-0.38\pm 0.06$ [20].

In Figure 7, we compute ${\mathcal{P}}^{\mathrm{\Lambda }}$ at $\sqrt{s_{NN}}=3$ GeV as a function of centrality, where the shaded areas correspond to the values of the intrinsic polarization z computed with Equation (5). We test the sensitivity of the model to a non-negligible ${\mathcal{P}}_{REC}^{\mathrm{\Lambda }}$ and plot the $\mathrm{\Lambda }$ global polarization with and without a constant contribution of ${\mathcal{P}}_{REC}^{\mathrm{\Lambda }}=4$%. We can already see that there is an improvement in the contributions from the highest centrality intervals when comparing to data for Au + Au at $\sqrt{s_{NN}}=3$ GeV [16].

If we want to go beyond this test and include a more realistic contribution, we should keep in mind that ${\mathcal{P}}_{REC}^{\mathrm{\Lambda }}$ is not constant, but, instead, it is a function of centrality and of the collision energy. One way to improve our model in this direction is to take into account the projection of the well-known transverse polarization of $\mathrm{\Lambda }$s produced in the corona (assuming that is similar to the polarization produced in pp collisions) along the direction of the total angular momentum. As we reported in Ref. [21], we found that a non-vanishing average transverse polarization could be linked with a non-vanishing even component of the directed flow. At NICA energies, we have tested this using the MPDroot framework [26,27] and, in a partial analysis, we found non-negligible contributions. This is a work in progress, and a full analysis will be reported elsewhere.

7. Conclusions

We have developed a two-component source model dubbed a core-corona model, to explain the excitation function of $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$ global polarizations. The essential ingredient of this model is the behaviour of the relative abundances $N_{\mathrm{\Lambda }QGP}/N_{\mathrm{\Lambda }REC}$ in the core and the corona as a function of the collision energy. The intrinsic $\mathrm{\Lambda }$ and $\overline{\mathrm{\Lambda }}$ polarizations z and $\overline{z}$, respectively, are computed by means of the relaxation time evaluated from a field theoretical calculation of the quark self-energy in a thermal QCD medium with an effective coupling between the thermal vorticity and the s-quark spin. We obtain different average global polarization for $\mathrm{\Lambda }$s and $\overline{\mathrm{\Lambda }}$s, a feature that is not usually found with other approaches. The model also predicts maxima for the polarization excitation functions at HADES and CBM at FAIR and NICA energies. The improvement of the model is a work in progress, and this includes quantifying the contribution from the polarization of the $\mathrm{\Lambda }$s and $\overline{\mathrm{\Lambda }}$s coming from the corona region as well as varying the parameters of the model in a consistent manner.