Gravitational form factors of a baryon with spin-3/2

The energy–momentum tensor (EMT) for a spin-3/2 baryon is related to seven mechanical quantities. In this work, we provide the general form of the gravitational form factors (GFFs) for a spin-3/2 baryon by using the multipole expansion and interesting relations between the EMT densities and the GFFs. To verify those general relations, we study the nucleon and the Δ\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\Delta $$\end{document} GFFs within the SU(2) Skyrme model based on the large Nc\documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$N_{c}$$\end{document} limit.


Introduction
The energy-momentum tensor (EMT) of the nucleon contains fundamental information on its three mechanical properties, i.e., the mass, spin, and D-term of the nucleon. These mechanical properties are related to three gravitational form factors (GFFs) at zero momentum transfer. While the mass and spin of the nucleon are relatively well known, the D-term, which provides essential information on how the nucleon experiences the internal force by its constituents, is much less known [1][2][3]. Thus, it is of great importance to investigate the D-term of the nucleon. The GFFs were at first considered [4,5] as a merely academic subject, since it was impossible to measure them directly. The reason is that the graviton indeed weakly interacts with the nucleon. However, the generalized parton distributions (GPDs) shed novel light on the GFFs of the nucleon, since the GFFs are identified as the second Mellin moments of the unpolarized GPDs [6][7][8][9], which get accessible experimentally in hard exclusive reactions. In fact, there are several ongoing and planned facilities that are ideal to measure the GPDs, such as the newly upgraded 12 GeV Continuous Electron Beam Accelerator Facility (CEBAF) at the Jefferson Lab, the Electron-Ion Collider (EIC) that will be constructed at Brookhaven National a e-mail: Jun-Young.Kim@ruhr-uni-bochum.de (corresponding author) b e-mail: sunbd@sdu.edu.cn Laboratory (BNL) [10], and the planned Electron-Ion Collider in China (EicC) [11]. The EIC experiments will produce unprecedented experimental results on the GPDs [12].
Another interesting object is the isobar, which is the first excited baryon with spin-3/2. While the electromagnetic properties of the have been extensively investigated both experimentally and theoretically, there are only a few theoretical works on the GFFs of the . In Ref. [13], the relevant structure for the GFFs of the was sorted out. The general properties of the pressure and shear forces for the isobar were derived in the large-N c limit [14]. Compared to the GFFs of the nucleon, the GFFs of the isobar have a far more complicated structure: ten different kinds of the GFFs together with the EMT-nonconserving form factors. Thus, it is rather difficult to grasp the physical meaning of the GFFs of the isobar. In this sense, the multipole expansion of the EMT matrix elements of the will reveal the physical implications of the GFFs. The GFFs of the nucleon were first extracted from the GPDs [15], by using the data on deeply virtual Compton scattering (DVCS) of the nucleon. On the other hand, it is rather difficult to measure experimentally the GFFs of the or to extract them from the corresponding GPDs because of its short-lived nature. In the meantime, we anticipate that lattice QCD will provide a clue to understanding the GFFs of the .
In the present work, we aim at how the EMT matrix elements of the can be compactly expressed in terms of the GFFs, using the multipole expansion. By doing that, we are able to find interesting relations between the EMT densities and these GFFs. We want to emphasize that the relations obtained in the present work are model-independent. We will verify these general relations within the framework of the SU(2) Skyrme model. The model is known to be one of the simplest ones for describing the lowest-lying baryons based on the large N c expansion. In the limit of N c → ∞ [16,17], a baryon arises as a topological soliton with an effective mesonic degrees of freedom. In addition, the model satis-fies the essential properties of QCD such as chiral symmetry and its spontaneous breaking. The model describes very well important properties of the nucleon in low-energy regimes. Furthermore, the model has explained numerous observables for the baryons [18,19] and has even described well general properties of the nucleon GFFs. Thus, we will use the Skyrme model to examine those of the GFFs.
We sketch the present work as follows: In Sect. 2 we define the hadronic matrix elements of the EMT as the GFFs and reorganize the GFFs in terms of the multipole expansion. We also define the EMT densities of a baryon with spin-3/2 in terms of the multipole expansion and present the relations between the GFFs and the EMT densities. In order to verify the general requirements and relations proposed in Sect. 2, the GFFs and the EMT multipole densities of the are obtained within the Skyrme model in Sect. 3 and the numerical results are showed and discussed in Sect. 4. In the final Sect. 5, we present a summary and conclusions.
Here, σ (σ ) is the initial (final) spin projections. The normalization of the Rarita-Schwinger spinors is taken to be u α σ ( p)g α α u α σ ( p) = −2mδ σ σ . The index a runs from a gluon to quark flavors. The quark and gluon form factors F a i,k (i = 1, 2, 4, 5) are individually conserved, whereas F a i,k (i = 3, 6) are not conserved. Note that we name the GFFs of a baryon with spin-3/2 according to Ref. [13] and reparametrize them to be analogous with those with spin-1/2 and spin-1. The separate quark and gluon GFFs depend on the renormalization scale μ, which is suppressed for simplicity. Because of the EMT conservation, the nonconservation terms F a i,k (i = 3, 6) have constraints, i.e., a F a i,k = 0 (i = 3, 6). The scale-invariant total GFFs are obtained as F i,k = a F a i,k (i = 1, 2, 4, 5).

Gravitational form factors in Breit frame
Before discussing the GFFs, we define the n-rank irreducible tensors and the multipole operators. The n-rank irreducible tensors in coordinate (or momentum) space are given by 2 In order to be in line with the definition of the matrix elements of the EMT current for a spin-1/2 baryon, we reparametrized the expressions given in Ref. [13] as (F a 1,0 , F a 1,1 , F a 2,0 , F a 2,1 , Note that there is a typo in Ref. [13], and it should be corrected as g μν α α F T 5,0 → 2g μν α α F T 5,0 .
In the Breit frame the average of the baryon momenta and the momentum transfer are respectively defined by P μ = ( p μ + p μ )/2 = (E, 0, 0, 0) and μ = p μ − p μ = (0, ) with the initial (final) momentum p ( p ). The momentum squared is defined as 2 = − 2 = t = 4(m 2 − E 2 ) with the baryon mass m. The explicit expressions of the Rarita-Schwinger spinor and the polarization vector are given in Appendix A. In this frame, the matrix elements of the EMT current are expressed in terms of the gravitational multipole form factors (GMFFs) as J a One can refer to Appendix A in detail. The sum of the quark and gluon contributions to the GMFFs is also scale-invariant: The EMT density T μν (r, σ , σ ) is given by the Fourier transform of the matrix element of the EMT current in momentum space:

Energy density
The temporal component of the EMT T 00 (r, σ , σ ) is related to the energy density. The mutipole expansion of the energy density is defined by where the monopole and quadrupole densities ε 0,2 (r ) are respectively given by with At the same time, the energy multipole form factors E 0,2 (t) can be expressed in terms of the energy densities ε 0,2 (r ) in coordinate space: For a particle of arbitrary spin, the general tensor quantity is introduced in Refs. [21,44] by The monopole moment corresponds to the mass of a baryon, accordingly one arrives at the apparent relation which gives the normalization The constraint F 1,0 (0) = 1 for the spin-3/2 baryon coincides with that for the spin-1/2 and spin-1 hadrons. The gravitational quadrupole density of a baryon describes how the energy density is deformed from spherically symmetric shape. This quantity does not appear in the spherically symmetric hadrons. It can be quantitatively estimated as Another interesting property is the mass radius of a baryon. It can be derived by the r 2 -weighted energy density in the Breit frame. The expression of the mass radius is found to be

Angular momentum density
The spin density is given by The angular momentum density is obtained from the 0kcomponents of the EMT, which is decomposed into the 0-, 2-and 4-multipole components (see also Refs. [45,46]). The sum of the angular momentum contributions from quark and gluons to the spin-3/2 baryon is obtained by which yields the spin operator of the baryon with the constraint F 4,0 (0) = 3/2. Since our interest lies in the monopole angular momentum density in this work, we separately define it as accordingly the averaged angular momentum density is given by with spin S = 3/2. The angular momentum form factor can be expressed in terms of the averaged angular momentum density as

Pressure and shear force densities
The pressure and shear force densities are related to the i jcomponents of the static EMT. These densities are firstly defined in Refs. [20,44] and newly parametrized in Refs. [14,43] to conveniently express the strong forces in a hadron acting on the radial area element. Following Refs. [14,43] we can express the stress tensor in terms of the pressure and shear forces densities by From the EMT conservation ∂ i T i j (r, σ , σ ) = 0, the following equilibrium relations between the pressure and shear force densities are derived: ds n (r ) dr + 2 s n (r ) r + dp n (r ) dr = 0, with n = 0, 2, 3. (27) This differential equation guarantees the stability condition. The functions p 0 (r ) and s 0 (r ) correspond to the pressure and shear force densities appearing in the spherically symmetric hadrons. The functions p 2 (r ) and p 3 (r ) are named the quadrupole pressure densities, and the s 2 (r ) and s 3 (r ) are called the quadrupole shear force densities according to Ref. [14]. These densities p n (r ) and s n (r ) are respectively written as Similarly, the form factors D 0,2,3, (t) can be expressed in terms of the pressure and shear force densities in coordinate space: The pressure densities p n (r ) satisfying the relation given in Eq. (28) comply with the von Laue condition Note that the dimensionless constants (generalized D-terms) are defined by [14] D n ≡ d 3 rD n (r ) = m d 3 r r 2 p n (r ) The generalized D-terms D 0,2,3 introduced in Ref. [14] are related to the form factors D 0,2,3 (t) as follows: Interestingly, the strong forces carried by constituents can be interpreted as a certain combination of pressure and shear force densities [1]. The spherical components of the strong 3 A typo in Ref. [43] is corrected in Eq. (29).
forces (d F r , d F θ and d F φ ) acting on the radial area element (d S = d S rêr + d S θêθ + d S φêφ ) are expressed as follows [14]: Here, as defined in Ref. [2], the mechanical radius can be given by As for the unpolarized spin-3/2 hadron, since the normal force acting on the radial area element (d F r /d S r ) is solely due to p 0 (r )+ 2 3 s 0 (r ), it should comply with the local stability criterion given in Ref. [2] as

Gravitational form factors of the in the Skyrme model
The Skyrme Lagrangian density is given by where U is the SU(2) chiral field, and e stands for a dimensionless parameter and tr F is trace over flavors. The F π and the m π are the pion decay constant and the pion mass, respectively.
In the large-N c limit, we have the parameter scales , so as to have L = O(N c ). In this limit, the chiral field is assumed to be a static one. Here, the static chiral field is written as U (r ) = exp[r i τ i P(r )], withr i = r i /|r| and the isospin Pauli matrices τ i , by adopting the hedgehog ansatz where P(r ) indicates a profile function with the boundary conditions P(0) → π and P(∞) → 0.
The classical soliton mass is defined by M sol = − d 3 r L, which is expressed with respect to the profile function and the model parameters by The profile function is obtained by minimizing the classical soliton mass and has an asymptotic behavior in the limiting case r → ∞, where the constant R 0 is determined by the profile function derived by minimizing the classical soliton mass and is given in terms of the axial coupling constant in the chiral limit [31,47].
In order to assign the quantum number to the soliton, the time-dependent chiral field should be considered as Having quantized the collective coordinates ( i →Ĵ i /2I ), one obtains the collective Hamiltonian [48] with the moment of inertia The collective Hamiltonian acts on the collective baryon wave functions given in Ref. [48]. In principle F π and e are model parameters. However, the parameters are fixed to reproduce the following observables [31] M N + M ≡ 2M sol = 2171 MeV, and the model parameters are consequently found to be m π = 138 MeV, F π = 131.3 MeV, e = 4.628.
From the above parameters, the classical soliton mass and the moment of inertia are determined by M sol = 1085 MeV, I = 1.01 fm. (45) In this work, we strictly follow the set of parameters used in Ref. [31] to keep consistency. The canonical EMT in the Skyrme model can be derived by where φ a is a time-dependent mesonic field with U (t, r ) = φ 0 + iτ · φ. The degree of freedom of the mesonic field is reduced to three (a = 1, 2, 3) by the constraint φ 2 0 + φ 2 = 1. With the constraint, the canonical EMT in the Skyrme model is found to be symmetric. The respective components of the EMT densities is expressed as (1 − cosP(r )) , (1 − cosP(r )) , The rotational corrections to the EMT densities are obtained by The rotational corrections to the 0k-components of the EMT densities δ rot T 0k (r, σ , σ ) are found to be null in the current Skyrme Lagrangian. The corrections appear in the higherorder derivative terms that generate 3 However, the corrections are strongly suppressed in the large-N c expansion. Thus, we can safely neglect the rotational corrections to the 0k-component of the EMT densities.
As given in Eqs. (12), (24) and (26), the multipole densities can be extracted from the EMT densities in Eq. (47): In the same manner, the rotational corrections are derived from Eq. (48): Interestingly, in the chiral soliton picture the rotational corrections to the EMT densities in Eq. (50) are related to the quadrupole densities, which was firstly found in Ref. [14]. The quadrupole energy density ε 2 (r ) is found to be In other words, the quadrupole energy density ε 2 (r ) is related to the energy densities of the nucleon ε N 0 (r ) and the ε 0 (r ) with Also, the usual sizes of the quadrupole density ε 2 (r ) is estimated by As for the quadrupole pressure and shear force densities, the remarkable general relation in a chiral soliton picture is derived in Ref. [14] By comparing Eq. (26) with Eq. (48) we reproduce this relation in the Skyrme model. The above relation (55), together with the EMT conservation (27), implies the null results of the quadrupole densities s 2 (r ) and p 2 (r ), and the similar relations to Eq. (51) for the pressure and shear force densities are obtained [14]: Therefore, we arrive at the similar expressions as Eq. (52) with Here, one has to bear in mind that due to the EMT densities with the included rotational corrections the pressure p n (r ) and the shear force s n (r ) densities do not uniquely exist and should be reasonably determined. Let us first recall that the leading-order (LO) result of p 0 (r ) satisfies the von Laue condition that is equivalent to the equation of motion [31]. However, once one considers the next-to-leading-order (NLO) result of p 0 (r ), it breaks the von Laue condition. Thus, one might introduce the "variation after quantization" methodminimizing the baryon mass after quantizing the soliton -as a prescription. However, this method also has a drawback: the chiral symmetry in the large-r region is not satisfied [47].
To preserve the chiral symmetry and satisfy the von Laue condition, we first adopt the "quantization after variation" method-quantizing the soliton after minimizing the soliton mass -and treat the rotational corrections to the EMT densities as a small perturbation. Of course, the von Laue condition is broken. Thus, instead of directly using the model result of p 0 (r ), we solve the equilibrium equation given in Eq. (27) with the approximated shear force density s 0 (r ) and reconstruct the pressure p 0 (r )| reconst , which then automatically complies with the stability condition [47]. We also derive the reconstructed quadrupole pressure p 3 (r )| reconst in the same manner.
Before discussing the GFFs, it is important to discuss the large distance properties of the EMT densities. The large distance behaviors of the EMT densities for the spherically symmetric baryon were investigated and presented within the Skyrme model in Refs. [31,47]. For completeness, we present the large distance properties of the quadrupole densities in the chiral limit as The · · · indicates the contributions strongly suppressed in the large-r region. Interestingly, the quadrupole densities ε 2 (r ) and p 3 (r ) are weakly suppressed in the large distance, which have the analogous behavior with the angular momentum density ρ J (r ) ∝ 1 r 4 . Keep in mind that in order to respect the chiral physics and the stability condition, we discard the result of p 3 (r ) and adopt the newly reconstructed p 3 (r )| reconst by solving the differential equation (27). As a result, the discrepancy between p 3 (r )| reconst and p 3 (r ) arises from the fulfillment of both the chiral physics and the stability condition and is inevitable. For finite pion mass, the densities are exponentially suppressed.
Since this model is based on the large-N c expansion, it is necessary to clarify the large-N c behaviors of the GMFFs of the . The large-N c expansion is valid in the region |t| M 2 . In the limit of N c → ∞, we have the following large-N c behaviors and the scales of the GMFFs are found to be or according to Ref. [14] the generalized D-terms have the scales as It is found that the GMFFs have the orders of ∼ N 0 c except for the form factors D 0 (t) and D 3 (t), which have the orders of ∼ N 2 c , whereas the generalized D-terms D 0 , D 2 and D 3 have the orders of ∼ N 2 c , ∼ N 0 c and ∼ N 0 c , respectively.

Numerical results and discussion
In this section, we present the numerical results and discuss them. We first examine the monopole and quadrupole energy densities arising from the temporal component of the EMT. Note that the LO monopole energy densities ε 0 (r ) of the nucleon and the are degenerate. To lift the degeneracy, we need to take into account the rotational corrections 2 In the left panel of Fig. 1, we draw the numerical results on the monopole energy densities of the classical soliton (LO), the nucleon (NLO) and the (NLO) as functions of radius r . The values of the three monopole energy densities at r = 0 are all found to be ε 0 (0) = ε N , 0 (0) = 2.27 GeV · fm −3 . The reason is that the value of δ rot ε (J ) 0 , which is proportional to the quadrupole energy density ε 2 (r ) depicted in the right panel of Fig. 1, becomes zero at r = 0. The left panel of Fig. 1 exhibits As given in Eq. (64), the value of the mass radius of the is larger than those of the classical soliton and nucleon. It reflects the fact that the monopole energy density of the has a broader shape in comparison with those of the classical soliton and nucleon. In the case of the finite pion mass, the NLO mass radii of the nucleon and the are found to be finite, since the energy densities are exponentially suppressed in the large distance. However, in the chiral limit, those mass radii diverge because the rotational corrections to the energy densities are proportional to 1/r 4 in the large-r , i.e., r 2 E ∝ ∞ 0 dr r 4 ε N , 0 (r ) as given in Eqs. (56) and (59), which is similar to the isovector charge radius of the nucleon in Ref. [48]. In the right panel of Fig. 1, the numerical result for the quadrupole energy density ε 2 (r ) of the is drawn as a function of radius r . The quantity ε 2 (r ) provides information on how the energy density is deformed from the spherically symmetric shape. It has a peak at around r = 0.4 fm with a negative sign and its strength is very small compared with ε 0 (r ). By integrating ε 2 (r ) over r , we can estimate the typical size of ε 2 (r ) as We confirm the relation numerically, first obtained in the large N c limit [14]. The value of the integration of ε 2 (r ) over r is approximately 10% ∼ O(1/N 2 c ) of that of ε 0 (r ). Another interesting property is the mass quadrupole moment given in Eq. (19). Its value exhibits how the energy density is deformed from the spherically symmetric shape quantitatively and is found to be In the chiral limit, the mass quadrupole moment diverges by the same reason as the NLO mass radius, i.e, ε 2 (r ) ∝ 1 r 4 . Figure 2 shows the result for the averaged angular momentum density ρ J (r ) normalized by the corresponding baryon spin S. As shown in Eqs. (21) and (24), ρ J (r ) is related to the 0k-components of the EMT. The integration of ρ J (r ) over r yields the constraints on the form factors J 1 (0) and F 4,0 (0) We obtain the numerical results for the mean square radius r 2 J of the nucleon and the as The results r 2 J for the nucleon and the are degenerate. Since in Eq. (50) higher-order corrections to the EMT densities δ rot T 0k (r, σ , σ ) are absent, the averaged angular momentum density of the differs from that of the nucleon by factor three, and its mean square radius of the is the same as that of the nucleon. 4 As mentioned in the previous section, the higher-order corrections to the averaged angular momentum δ rot ρ The left panel of Fig. 3 shows the results of the pressure densities for the classical soliton (LO), the nucleon (NLO), and the (NLO) as functions of radius r . The LO pressure naturally complies with the von Laue condition that is equivalent to the equation of motion. However, as discussed in the previous section the NLO pressures do not satisfy the stability condition. Thus, we adopt a strategy that preserves the chiral symmetry and satisfies the stability condition. We first take the variation of the soliton mass, and then quantize the soliton. By treating the rotational corrections as a small perturbation, we then obtain the approximated shear force density s 0 (r ). With using s 0 (r ), we reconstruct the pressure p 0 (r )| reconst from Eq. (27), so that the pressure density meets the stability condition. Thus, the LO and NLO pressures in Fig. 3 satisfy the stability condition. In the meantime, satisfying the stability condition implies that the pressure density has at least one nodal point (r 0 ) where the pressure density vanishes. For the inner part of r 0 ( p 0 > 0) repulsive force dominates, whereas for the outer part of r 0 ( p 0 < 0) attractive force governs. Thus, we obtain the nodal points r 0 for the classical soliton, nucleon and numerically as follows: (69) 4 Note that in the chiral limit the averaged angular momentum density ρ J (r ) decrease as r −4 in large distance, so the radius diverges.
While the value of r 0 for the nucleon and the classical soliton are comparable, that for the is found to be much larger than the results for the nucleon and the classical soliton. It indicates that the is mechanically spreading more widely compared with them. The right panel of Fig. 3 illustrates the results of the approximated shear force densities for the , the nucleon and the classical soliton. To comply with the stability condition the D-term D 0 (0) should be negative, which means that the integral (weighted by r 2 ) of the shear force densities over all values of r should be positive. (see Eq. (32)). Indeed, the shear force densities for them are always positive. While the s 0 (r ) for the has a wide-spreading shape in comparison with those for the classical soliton and nucleon, the magnitude of s 0 (r ) for the is considerably small compared with those for the others. Figure 4 shows the result of the quadrupole pressure (shear force) density for the . The quadrupole pressure p 3 (r )| reconst is reconstructed, as the NLO pressures p N , 0 (r )| reconst were derived from Eq. (27). Thus, p 3 (r )| reconst also complies with the stability condition given in Eq. (31), and has a nodal point located at r 0 = 0.56 fm. The shapes of p 3 (r )| reconst and s 3 (r ) are similar to those of p 0 (r ) and s 0 (r ), respectively.
The left panel of Fig. 5 presents the results of the monopole normal force components p 0 (r )| reconst + 2 3 s 0 (r ) acting on the radial area element for the classical soliton, the nucleon and the unpolarized . When it comes to a spherically symmetric baryon, the monopole normal force can be directly related to the local stability condition (36) stating that the force is always directed outwards. As for the polarized , the contributions of the quadrupole densities to the normal force come into play. The result of the quadrupole normal force p 3 (r )| reconst + 2 3 s 3 (r ) is shown in the right panel of Fig. 5, except for that of the nullified densities s 2 (r ) and p 2 (r ). It is found that the monopole and quadrupole normal forces are positive over the whole region of r . For the large distance in the chiral limit, the monopole normal force keeps the positivity, which means that the local stability condition is satisfied. Note that the quadrupole normal force has a positive sign However, we do not know how the quadrupole normal force is related to the local stability conditions so far. Another interesting quantity is the mechanical radius. As defined in Ref. [2], the mechanical radius is obtained by Similar to Eqs. (64) and (69) the value of r 2 0 mech for the is larger than those for the classical soliton and nucleon, which verifies that indeed is mechanically spreading more widely compared with those for the classical soliton and the nucleon. Furthermore, we define the quadrupole mechanical radius r 2 3 mech in Eq. (35), and its numerical value is found to be The quadrupole normal force is very compact in comparison with monopole one. Finally, we discuss the GFFs and GMFFs. As shown in Sect. 2, the GMFFs are expressed in terms of the GFFs and related the EMT densities as shown in Eqs. (15), (25) and (30). In the Skyrme model, the energy E 0 (t) and angular momentum J 1 (t) form factors satisfy the constraints E 0 (0) = F 1,0 (0) = 1 and J 1 (0) = 1 3 F 4,0 (0) = 1 2 . Besides the octupole angular momentum form factor J 3 (t) is assume to be zero, i.e., J 3 (0) = − 1 6 [F 4,0 (0) + F 4,1 (0)] = 0, because the corresponding density is suppressed in the large-N c expansion. As a result, we get the relation F 4,1 (0) = −F 4,0 (0) = −3/2. There is no additional constraint on E 2 (t), D 0 (t), D 2 (t) and D 3 (t). Therefore, we determine the moments of the GMFFs from Eqs. (15), (25) and (30) 5 By assuming that the pressure p n (r ) and shear force s n (r ) densities vanish at large-r faster than any power of r , one can arrive at the general relation between them as follows [29]: ∞ 0 dr r N s n (r ) = − 3(N +1) 2(N −2) ∞ 0 dr r N p n (r ) for N > −1, which arise from the differential equation (27).
The energy quadrupole form factor is obtained as E 2 (0) = 0.34, and it is related to the mass quadrupole moment given in Eq. (19). The value of the D-term 6 D 0 (0) of the is found to be −3.53. The quadrupole form factors D 2 (0) and D 3 (0) turn out to be −0.20 and 0.24, respectively. Those quadrupole form factors are related to the generalized D-terms given in Eq. (33) and determined as The generalized D-terms of the present work are comparable with those of Refs. [14,47]. The numerical results for the GMFFs and GFFs as functions of t are shown in Figs. 6 and 7, respectively. We restrict ourselves in the range of 0 < (−t) < 1 GeV 2 because of the validity of the large-N c expansion, i.e., |t| M 2 . We find that typical sizes of the quadrupole form factors E 2 (t) D 2 (t) and D 3 (t) are relatively small in comparison with those of the monopole form factors E 0 (t) and D 0 (t).

Summary and conclusions
In the present work, we aimed at providing the general form of the GFFs for a spin-3/2 baryon in terms of the multipole expansion and finding interesting relations between the EMT densities and these GFFs. We first defined the matrix elements of the EMT current given in Ref. [13] in terms of the GFFs, and then we expressed these GFFs by using the multipole expansion and related them with the EMT densities. The temporal component of the EMT density includes information on the mass m, its radius r 2 E and the gravitational quadrupole moment Q i j σ σ . The explicit relations between the multipole mass form factors E 0,2 (t) and the multipole energy densities ε 0,2 (r ) were provided. The spin density was related to the dipole and octupole spin form factors J 1,3 (t). The integration of the spin density over r yielded the constraint, which is analogous to a spin-1/2 baryon, for the dipole spin form factor J 1 (t). The stress tensor, parametrized in terms of the pressure p n (r ) and shear force s n (r ) densities (for n = 0, 2, 3), was related to the form factors D n (t). Interestingly, those densities should comply with the equilibrium equation (27) to have the conserved EMT, which means that the respective pressures p n (r ) have their own von Laue conditions and the corresponding generalized D-terms. Thus, we found a connection between the generalized D-terms D n Fig. 6 Gravitational multipole form factors of the as functions of squared momentum transfer t and the form factors D n (0). In addition, we obtained the expressions for the strong forces in terms of p n (r ) and s n (r ) inside a baryon and defined the generalized mechanical radii r 2 n mech . To examine the general relations proposed in Sect. 2, we used the SU(2) Skyrme model based on the large-N c expansion. Since this model satisfies chiral symmetry and its spontaneous breaking, and described well the general properties of the nucleon GFFs, the model is suitable for investigating the GFFs of the . We first derived all the expressions for the EMT densities up to 2 ∼ O(N −2 c ) and reproduced the large-N c relations proposed in Ref. [14] within the Skyrme model. One of the remarkable relations was the null results of p 2 (r ) and s 2 (r ), which makes D 2 vanishes. We also studied the N c behaviors of the GMFFs and the generalized D-terms.
In the Skyrme model, while the masses of the nucleon and the were overestimated, they satisfied the constraint E 0 (0) = F 1,0 (0) = 1. We found that the energy density of the is spreading more widely in comparison with that of the nucleon. We obtained the mass quadrupole moment for the as Q i j σ σ = −0.0181Q i j σ σ GeV · fm 2 that is related to the mass quadrupole form factor E 2 (0) = 0.34. For the angular momentum density normalized by the corresponding baryon spin, we got the degenerate results on those for the nucleon and the . The angular momentum form factor for the satisfied the constraint J 1 (0) = F 4,0 (0)/3 = 1/2. Moreover, the null result of the octupole spin form factor J 3 (t) = 0 gave the additional constraint F 4,1 (0) = −F 4,0 (0) = −3/2. When treating the pressure and shear force densities with included rotational corrections, we reconstructed the pressure densities p n (r ) from the approximated shear force den- We predicted t dependence on the GFFs and the GMFFs for the in the range of 0 < (−t) < 1 GeV 2 . We found that the typical sizes of the quadrupole form factors E 2 (t), D 2 (t) and D 3 (t) are relatively small in comparison with those of the monopole form factors E 0 (t) and D 0 (t).
As suggested in Ref. [14] the lattice measurements of the GFFs can be used to check whether -baryon is a rotating soliton. Here, we provided the first numerical estimates of corresponding GFFs in the soliton picture using the Skyrme model. We expect that the results of the lattice QCD or the theoretical model will soon come out.