Cascade of polarized Compton scattering and Breit-Wheeler pair production

Cascaded Compton scattering and Breit-Wheeler (BW) processes play fundamental roles in high-energy astrophysical sources and laser-driven quantum electrodynamics (QED) plasmas. A thorough comprehension of the polarization transfer in these cascaded processes is essential for elucidating the polarization mechanism of high-energy cosmic gamma rays and laser-driven QED plasmas. In this study, we employ analytical cross-sectional calculations and Monte Carlo (MC) numerical simulations to investigate the polarization transfer in the cascade of electron-seeded inverse Compton scattering (ICS) and BW process. Theoretical analysis indicates that the polarization of background photons can effectively transfer to final-state particles in the first-generation cascade due to helicity transfer. Through MC simulations involving polarized background photons and non-polarized seed electrons, we reveal the characteristic polarization curves as a function of particle energy produced by the cascaded processes of ICS and BW pair production. Our results demonstrate that the first-generation photons from ICS exhibit the non-decayed stair-shape polarization curves, in contrast to the linearly decayed ones of the first-generation electrons. Interestingly, this polarization curve trend can be reversed in the second-generation cascade, facilitated by the presence of polarized first-generation BW pairs with fluctuant polarization curves. The cascade culminates with the production of second-generation BW pairs, due to diminished energy of second-generation photons below the threshold of BW process. Our findings provide crucial insights into the cascaded processes of Compton scattering and BW process, significantly contributing to the understanding and further exploration of laser-driven QED plasma creation in laboratory settings and high-energy astrophysics research.


I. INTRODUCTION
Electron-positron (e + e − ) pair plasmas play a crucial role in the realm of high-energy astrophysics, particularly in the most extreme celestial sources such as active galactic nuclei, gamma-ray bursts (GRBs), black hole binaries, and pulsars [1][2][3][4].Moreover, the creation of pair plasmas holds significant potential in the forthcoming generation of tens-petawatt lasers, which boast intensities surpassing 10 23 W/cm 2 [5,6].The formation of pair plasmas hinges upon the cascaded interactions of Compton scattering and Breit-Wheeler (BW) pair production, which are recognized as the two fundamental mechanisms [7][8][9][10][11].For instance, within the black hole magnetosphere, relativistic leptons undergo acceleration within unscreened electrostatic gaps generated by the black hole's rotation, attaining relativistic energies.Subsequently, the relativistic leptons engage in inverse Compton scattering (ICS) with soft background photons emitted by the accretion disk.This process yields high-energy gamma-ray photons, which, in turn, collide with other background photons, resulting in the production of e + e − pairs.These cascading processes continually replenish the pair plasma, thereby sustaining the force-free magnetosphere, which serves as a model for plasma jet launching in black holes.
Relativistic jets encompass various astrophysical phenomena, with GRBs being one notable example.Accurate measurement of the polarization in GRBs is crucial for attaining a comprehensive understanding of the physical characteristics of these jets, including the energy dissipation locations and radiation mechanisms [12][13][14].High levels of linear polarization have been observed in the prompt emissions of GRBs at high-energy bands.For instance, RHESSI observations have reported polarization levels of up to 80% [15], while INTE-GRAL observations have detected polarization of 98% within the energy range of 100-350 keV [16].Furthermore, circular polarization of approximately 60% has been observed in the optical afterglow [17].The polarization in GRBs is commonly interpreted through synchrotron emission, which can arise from various magnetic field configurations within structured GRB jets, including aligned, toroidal, and random magnetic fields [18].Notably, polarized synchrotron soft photons can undergo ICS by cold relativistic electrons within the outflow, resulting in the production of hard gamma-ray photons [19].
The advent of petawatt laser facilities around the world [6,[20][21][22] has opened the door to ultra-relativistic laser-plasma interactions in the regime dominated by strong-field quantum electrodynamics (QED).In this regime, nonlinear QED processes can give rise to the production of abundant gamma-ray photons and electron-positron (e + e − ) pairs [23,24].The electromagnetic QED cascade, characterized by the emission of multiple photons and their subsequent conversion into e + e − pairs, has been extensively investigated in vacuum, with a particular focus on laser intensities approaching the critical field strength for vacuum pair production [25][26][27][28].Accounting for the polarization of photons and e + e − pairs, the electromagnetic QED cascade in vacuum can produce highly polarized particles and induce asymmetries in the polarization distribution [29,30].The coupling between relativistic collective plasma dynamics and electromagnetic QED cascade processes can lead to the creation of dense pair plasmas [31][32][33][34][35][36][37], enabling laboratory investigations of high-energy astrophysical phenomena, such as GRBs, using upcoming tens-petawatt lasers.Recent studies have shown considerable interest in polarized strongfield QED processes in laser-driven plasma [24,38,39], which have been incorporated into particle-in-cell (PIC) simulations to explore polarization effects within strong electromagnetic plasma environments.Moreover, QED-PIC simulations indicate that irradiating solid targets with petawatt lasers at peak intensities exceeding 10 23 W/cm 2 can lead to the production of dense polarized gamma-ray photons and polarized e + e − pairs [40][41][42][43][44].
The production of laser-driven QED plasmas, characterized by high-density polarized gamma-ray photons and e + e − pairs exceeding 10 16 / cm −3 [33], highlights the significance of binary QED collisions through the cascade of Compton scattering and BW pair production in the subsequent dynamic evolution of pair plasma.Preliminary investigations employing 3D PIC simulations suggest that the linear BW process could dominate pair production during the creation of laserdriven QED plasmas [45,46].Hence, in order to attain a comprehensive understanding of the polarization physics in GRBs and perform accurate simulations of laser-driven pair plasmas, it is crucial to establish complete knowledge of the cascade between polarized Compton scattering and BW process.The complete polarization effects of the BW process have been investigated using fully angle-and spin-resolved Monte Carlo (MC) numerical methods [47,48].To model the cascade between polarized Compton scattering and BW process, the former can be described utilizing the same numerical method with fully polarized cross sections [49].Prior to undertaking fully consistent simulations with the QED-PIC method [44], it is necessary to carefully examine the polarization-associated physics of cascaded processes of Compton scattering and BW pair production within a charge-free space.
In this paper, we investigate the cascaded processes of polarized Compton scattering and BW pair production using analytical cross sections and MC numerical simulations.The polarization transfer in the cascade of multiple Compton scattering and BW process is examined in the center-of-momentum (c.m.) frame through theoretical calculations.These calculations reveal that the polarization transfer can be enhanced in the cascaded processes through the helicity transfer of photons and electrons.We visualize the electron-seeded cascade of ICS and BW process using multi-parameter MC simulations, assuming non-polarized seed electrons and background soft photons with different polarization.The resulting first-generation gammaray photons from multiple ICS exhibit non-decayed stair-shape polarization curves with respect to photon energy, in contrast to the linearly decayed polarization of first-generation electrons.The first-generation BW pairs, produced from collisions between first-generation photons and background photons, possess energy-dependent fluctuant polarization curves.The characteristic polarization and spectrum of the produced BW pairs, upon colliding with background photons, give rise to an exponential spectrum of second-generation photons with linearly decayed polarization curves.Additionally, the resulting secondgeneration electrons exhibit saturated polarization curves.This comprehensive understanding of the cascaded processes of Compton scattering and BW pair production is highly bene- ficial for investigating upcoming laser-driven QED plasmas in the laboratory and for associated research in high-energy astrophysics.
The paper is organized as follows: In Sec.II, we analytically investigate the polarization transfer in the cascaded processes of Compton scattering and BW pair production using completely polarized cross sections.In Sec.III, we employ MC simulations to explore the energy-dependent polarization of the produced gamma-ray photons and BW pairs in the cascade of multiple ICS and BW process.Finally, we present a concise summary of our findings in Sec.IV.
In order to theoretically model this cascaded processes, the cross sections of Compton scattering and BW process with arbitrary polarization should be formulated.The cross section for the BW process, accounting for arbitrary initial photon polarization and final electron (positron) spins, has been developed utilizing photon and lepton density matrices [47,48].Similarly, employing analogous theoretical techniques, the cross section for polarized Compton scattering, considering arbitrary polarization of initial and final particles, can be obtained (see Appendix for details).In addition to the theoretical analysis, the availability of cross sections for arbitrarily polarized Comp-ton scattering and BW process is advantageous for modeling realistic binary QED collisions using MC sampling.
With the formulated cross sections in c.m. frame, the polarization transfer in the cascaded processes can be analytically investigated.In electron-seeded multiple Compton scattering, the polarization state of incident photon, namely, background photon γ 0 , is fixed and described by Stokes parameters (ξ (0) 1 , ξ (0) 2 , ξ (0) 3 ).While the polarization of incident electron, described by spin vector (ζ 1 , ζ 2 , ζ 3 ), transits in each scattering.From the spin-dependent cross section of Compton scattering [see Eq. (A.3)], one obtains the Stokes parameters of final-state photon and spin components of final-state electron Here, F c represents the cross section with summation over the final electron spin.The coefficients G e i and G γ i determine the transition probabilities of the polarization of the final-state electron and electron in MC sampling.The explicit expressions for these coefficients can be found in the Appendix.Because of the multiple Compton scattering, It is important to note that, in c.m. frame, the quantities ξ γ,2 and ζ e,2 represent the mean helicity of the photon and electron, respectively.On the other hand, (ξ γ,1 , ξ γ,3 ) and (ζ e,1 , ζ e,3 ) correspond to the linear polarization of the photon and the transverse spin polarization of the electron.The Stokes parameters and spin vector of the incident photon and electron share the same interpretation and significance.
With the Stokes parameters of γ 0 and scattered photon, the spin components of the final electron in the BW process can be expressed as where the explicit expressions for the coefficients G − i can be found in Eq. (A.10).Note that the polarization of BW positron is the same to BW electron and thus only BW electron is used in analysis below.Finally, the total polarization can be analytically calculated using the following equations: where ξ γ corresponds to the total polarization of the scattered Compton photons, ζ e represents the total polarization of the scattered electrons, and ζ − denotes the total polarization of the BW electrons.
With the analytical polarization equations of Eqs. ( 4)-( 6), the polarization transfer in the cascaded processes can be illustrated in c.m. frame with ω of photon energy and cos θ of scattering angle.For the production of first-generation photons and electron from multiple ICS of seed electrons, the final-state spin of electron in the previous scattering is used to calculate the one in the next scattering, e.g., ζ ′ e of e ′ from Eq. ( 5) is used to calculate ξ ′′ γ of γ ′′ by Eq. ( 4).Stokes parameters of final-state gamma photon in each ICS are used to calculate the spins of first-generation BW pairs by Eq. ( 6), e.g., ξ ′ γ and ξ ′′   The polarization scenario of γ 0 with both degree of linear polarization and circular polarization are also considered; see in Fig. 3.In this case, the produced γ ′ with ξ ′ γ can be polarized via both single ξ 2 -associated terms in G  3(c) and (d).Therefore, these analytical calculations indicate that the polarization of background photons can be transferred throughout the electron-seeded cascade of ICS and BW process.

III. POLARIZATION TRANSFER IN THE CASCADED PROCESSES FROM MC SIMULATIONS
To numerically model the cascaded processes suggested in Fig. 1, we perform numerical simulations with multi-parameter MC method developed in our previous works [47,50].This approach permits the incorporation of beam effects of colliding particles with arbitrary energy and polarization distribution, and the angle and polarization of final-state particles are also resolved by MC sampling of polarized cross sections, as illustrated in details.Briefly, our developed MC simulation method pairs colliding photons and electrons or positrons into a three-dimensional cell to calculate a series of single Compton scattering or BW process.The energy and momenta of the paired particles in the laboratory frame are transformed to the c.m. frame to calculate the cross section.The scattering angle cos θ and azimuthal angle ψ of the final-state particles are determined by MC sampling from the differential cross section, and the determined c.m. energy and momenta can be transformed back to the laboratory frame to obtain the scattered photon or lepton.In the laboratory frame, we denote ε γ and ε e as the energy of the photon and the kinetic energy of the electron from ICS, respectively, and ε pair as the energy of the electron (positron) in the BW process.
We denote the statistical polarization of ICS photons and electrons from MC simulations as P γ and P e , respectively.With the determined energy and momenta of the final-state particles, the statistical polarization can be determined by MC sampling with transition probabilities of polarization given by the differential cross section, as shown in Eq. (A.3).Specifically, we obtain where ξ′ i and ζ′ i are the averaged components of the Stokes parameter and spin components over the particle number.These components are obtained by MC sampling according to the transition probabilities in Eq. (A.3).We obtain the statistical polarization of BW electrons (positrons) in a similar way, which we denote as P pair .
In the setups of the electron-seeded cascade between the polarized processes of ICS and BW, we randomize the background soft photons by a spectral distribution of I γ = I γ,0 (ε γ /ε min ) −α with ε min = 0.001 MeV and a spectral index of α = 1.2.This mimics the spectral distribution of the M87 black hole [8] and has an average energy of εγ 0 = 0.0361 MeV.The background soft photons have a uniform density of ∼ 1.4×10 16 cm −3 .We initialize 10 7 seed electrons with a spatially uniform density of ∼ 1.8 × 10 16 cm −3 , and assume the interaction region to be homogeneous and infinite to neglect the boundary effects of space charge force.We assume a Gaussian spectral distribution of I e = I e,0 exp [−(ε e − E 0 )/2σ 2 0 ] for the seed electrons.Relativistic electrons collide with the background soft photons with counter-propagation direction to produce gamma-ray photons via ICS, which later trigger the cascaded BW pair productions by collisions with background photons.We can tune the interaction time (denoted as IT) to terminate the cascade.In the simulations, the seed electrons are nonpolarized, and we can initialize the background soft photons with different polarization scenarios to mimic polarized ones produced in jet structures by synchrotron radiation [18].This leads to the production of polarized photons and electrons in ICS, as discussed in Sec.II.
The energy spectra of scattered photons and electrons from ICS are shown in Fig. 4,and each spectrum contains more than 10 6 scattered photons or scattered electrons.Since the total cross section only can be modified by the multiplied initial polarization of photon and electron, namely, ξ 2 ζ 2 and ξ 2 ζ 3 [see Eq. (A.4) and Fig. 8], the single polarization of background photons has no modification to the spectra and the later only depend on the initial spectrum of seed electrons.Due to the rapid down ramp of σ c near ω = 0.1m e , ICS results in the broaden saddle-shaped spectra of scattered electrons from the initial quasienergetic spectrum of seed electrons, and the double-ramp spectra of scattered photons; see Figs. 4(a) and  (b).In the correlated energy spectrum of ε e and ε γ , the linear distribution with energy spread of initial electrons implies the energy conservation from the single scattering of each seed electron, and the diffusion distribution below the linear one originates from the multiple ICS; see Fig. 4(c).Note that the ratio of scattered particles from multiple ICS to ones from single ICS increases with the interaction time, which will lead to the enhancement of polarization of photons and electrons according to the theoretical prediction in Sec.II.
The analytical polarization transfer discussed in Sec.II can be retrieved by the statistical polarization from realistic MC simulations in both c.m. frame and laboratory frame.For polarized γ 0 with ξ (0) 2 = 1 and ξ (0) 2 = ξ (0) 3 = 0.71, polarization curves of P e and P γ versus cos θ present the similar behavior to the analytical ones shown in Figs. 2 and 3, except for the different amplitudes due to the effects of broaden and diffused energy spectra of scattered particles in multiple ICS; see Figs. 5(a) and  (c).In terms of laboratory energy ε e , the scattered electrons are polarized at maximum in the energy region of deep ICS, namely, the energy of seed electrons are broaden downward to the left saddle of the spectrum shown in Fig. 4(b), after that P e decays linearly to zero at the elastic scattering limit where there is no energy transfer; see Fig. 5(b) and (d).In comparison, the scattered photons in ICS have the stair-type polarization curves versus energy ε γ , and the polarization of background photons can be more easily transferred to scattered photons even at elastic scattering limit.In terms of polarized γ 0 with ξ (0) 3 = 1, the polarization transfer still occurs between incident and scattered photons through non-zero single ξ 3 -associated term in G γ 3 , leading to the production of photons with linear polarization, while the polarization transfer to scattered electrons is prohibited due to the vanish of helicity transfer; see Fig. 5

(e) and (f).
The cascaded collisions between polarized first-generation gamma-ray photons and background photons result in the production of first-generation BW pairs; see Fig. 6.According to Eq. ( 3), the polarization of BW electron originates from helicity transfer through both helicity of a single photon and cross product of ξ (1) and ξ (2) of two colliding photons.For polarized γ 0 with ξ (0) 2 = 1, collisions between γ 0 and first-generation gamma-ray photons with circular polarization of right-hand he- licities result in the productions of longitudinally polarized BW electrons (positrons), and the asymmetric distribution of P pair results from the cos θ-dependent ζ ′ γ and ζ ′′ γ of first-generation gamma-ray photons; see Figs 6(a).For polarized γ 0 with ξ (0) 2 = ξ (0) 3 = 0.71, collisions between γ 0 and first-generation gamma-ray photons result in the similar distribution of P pair but the diminished polarization; see Fig. 6(b).Because of the zero contribution of dot product of ξ (1) and ξ (2) to the final polarization of BW pairs, for polarized γ 0 with linear polarization of ξ (0) 3 = 1, the cascaded collisions between γ 0 and first-generation γ-ray photons with linear polarization [see Fig. 5(f)] produce the non-polarized pairs.The polarization curves of BW electrons versus ε pair are none-decayed and fluctuant because of the stair-shape ones of first-generation gamma-ray photons and the varying tendency of P pair is caused by the stair-type P γ with corresponding ε γ above the threshold energy of BW process; Fig. 6(c).Since the longitudinal polarization is dominated in the produced first-generation BW electrons, the decrease of ξ (0) 2 leads to the decreased P pair .The produced first-generation BW electrons (positrons) proceed to collide with background photons to produce the second-generation photons and electrons via ICS.The secondgeneration photons are produced with exponential spectrum compared to the double-ramp one of first-generation photons, and the average energy of the spectrum is about εγ ≃ 7.5 MeV which terminates the second-generation BW process significantly since the c.m. energy ω ≈ εγ 0 εγ /m e ≃ 1.In comparison to the non-decayed polarization curve of firstgeneration photons shown in Fig. 5, P γ of second-generation photons decay linearly versus ε γ ; see Fig. 7(a).Because of the left-hand helicities (negative ζ −,2 ) of BW electrons, P γ of second-generation photons produced by polarized γ 0 with ξ (0) 2 = 1 is diminished compared to one produced by polarized γ 0 with ξ (0) 2 = ξ (0) 3 = 0.71.This is because that the polarization transfer from negative helicities of BW electrons and positive helicity of γ 0 leads to the cancelation each other according to Eq. (A.8), while for partially linear polarization of γ 0 , the ξ 3 -associated term in Eq. (A.8) leads to the production of highly-polarized second-generation photons.The spectrum of second-generation electrons are peaked due to the typical spectrum of BW pairs; see Fig. 7(b).The polarization curves P e of second-generation electrons are saturated at high-energy region compared to the decayed one of first-generation electrons.P e of second-generation electrons produced by γ 0 with ξ (0) 2 = 1 is higher than the one from ξ (0) 2 = ξ (0) 3 = 0.71 due to the helicity-dominated polarization transfer for electrons.Therefore, in terms of produced photons from ICS, the saturated polarization curves in first-generation cascade can be transformed to the linearly decayed one in second-generation cascade, and it is the inverse case for produced electrons from ICS.

IV. CONCLUSION
In summary, we investigate the polarization transfer in the cascaded processes of ICS and BW pair production through theoretical analysis and numerical simulations.Analytical analysis show that in the cascade of multiple ICS and BW process, the polarization of background soft photons can be effectively transferred to the final-state particles of the first-generation cascade owing to helicity transfer.With multi-parameter MC numerical simulations, we clarify the energy-dependent polarization curves in the electron-seeded cascade of ICS and BW process in detail.The circular polarization of background photons is transferred to gamma-ray photons via multiple ICS, leading to the production of first-generation gamma-ray photons with non-decayed polarization curves and first-generation electrons with linearly decayed ones.The polarized gammaray photons trigger the production of polarized BW pairs with fluctuant polarization curves, and the degree of polarization depends merely on the circular polarization of background photons.The first-generation BW electrons (positrons) trigger the second-generation cascade via ICS, which produces distinct polarization curves of photons and electrons compared to those in the first-generation cascade.The energy loss of second-generation photons leads to the termination of the cascade, thus precluding the production of second-generation BW pairs.This understanding of the polarized cascade between ICS and BW process is beneficial for investigating high-intensity laser-driven QED plasmas and related research on high-energy astrophysical phenomena such as gamma-ray bursts and active galactic nuclei.

Appendix: Completely polarized cross section of Compton scattering
The polarized cross section of Compton scattering is formulated in the center of mass (c.m.) frame as (relativistic units with ℏ = c = 1 are used throughout) [49] where r e is classical electron radius, |M f i | 2 is scattering amplitude expressed by photon and electron density matrixes.s and t are normalized Mandelstam invariants defined as where ζ ′ i and ξ ′ i are components of ζ ′ and ξ ′ .After integration over y (between x/(x + 1) and x) and ψ, one obtains the total cross section of Compton scattering

γ
are used to calculate ζ ′ − and ζ ′′ − of BW electrons.Considering γ 0 with ξ (0) 2 = 1 and non-polarized electron e, the polarization transfer in the first-generation cascade are shown in Fig. 2. According to Eqs. (A.8) and (A.9), the produced γ ′ with ξ ′ γ and e ′ with ζ ′ e can be polarized merely through helicity transfer of photon via single ξ 2 -associated terms in G γ2and G e 2 .As a result, γ ′ and e ′ are polarized with remarkably cos θ-dependent circular polarization and longitudinal polarization, respectively, as shown in Figs.2(a) and (c), which is originated from the distributions of helicity in c.m. frame [see Fig.9].In the next scattering of e ′ and γ 0 , the produced γ ′′ with ξ ′′ γ and e ′′ with ζ ′′ e can be polarized through both helicities of e ′ and γ 0 via the single or multiplied terms of ζ 2 and
ξ 2 in G γ 2 , G e 2 and G γ 3 , G e 3 , resulting in the almost completely polarized γ ′′ [see Figs.2(a) and (b)] and the enhancement of cos θ-dependent polarization of e ′′ [see Figs.2(c) and (d)].The slight energy-dependence of ξ ′ γ , ξ ′′ γ and ζ ′ e , ζ ′′ e , as shown in Figs.2(b) and (d), is induced by the non-zero linear polarization from G γ 3 which involves a term independent of polarization.The collisions between polarized γ ′ or γ ′′ and γ 0 result in the production of BW electron (positron) with highly longitudinal polarization induced by distributed left-hand helicity, as indicated by the sketch of helicity transfer in BW process in Fig. 1.The steep variation of ζ ′ − and ζ ′′ − near threshold energy (ω = 1) originates from the intrinsic helicity transfer of BW process with two right-hand photons [48].

γ 2 and single ξ 3 -
associated term in G γ 3 , namely, γ ′ is produced with the decrease of circular polarization and meanwhile the increase of linear polarization, leading to the slight diminishment of cos θ-dependent ξ ′ γ ; 3(a) and (b).While the produced e ′ with ζ ′ e is mainly polarized through helicity transfer of photon via single ξ 2 -associated terms in G e 2 since the minor contribution from single ξ 2 -associated terms in G e 3 [see Fig. 9(d)], leading to the remarkable diminishment of ζ ′ ; see 3(c) and (d).The resulted enhancement of ξ ′′ and ζ ′′ in this case is similar to the polarization transfer in the case of Fig. 2. Due to the diminished polarization of γ ′ and γ ′′ with both circular and linear polarization shown in 3(a) and (b), ζ ′ e and ζ ′′ e become remarkably cos θand ω-dependent; see Figs.

FIG 4 . 2 = 1 ,
FIG 4. Normalized energy spectra of scattered photons (a) and electrons (b) from ICS in laboratory frame, three lines correspond to seed electrons with peak energy of E 0 = 50, 100, 150 MeV with energy spread of 5%, respectively.(c) Correlated spectra of scattered photons and electrons, corresponding to E 0 = 150 MeV.The background photons are initialized with ξ (0) 2 = 1, and IT≃ 1 ms is run in the simulations.
The work is supported by the National Natural Science Foundation of China (Grants No. 12022506, No. U2267204, 12275209, 12105217), the Foundation of Science and Technology on Plasma Physics Laboratory (No. JCKYS2021212008), the Open Foundation of Key Laboratory of High Power Laser and Physics, Chinese Academy of Sciences (SGKF202101), and the Shaanxi Fundamental Science Research Project for Mathematics and Physics (Grant No. 22JSY014).
FIG 8.The total cross section of Compton scattering, calculated from Eq. (A.4), corresponding to different initial polarization of photon and electron.