Spin-Dependent WIMP Capture

• Spin-dependent WIMP capture is the process where WIMPs scatter off nucleons via axial-vector interactions in astrophysical bodies, becoming gravitationally bound.
• This mechanism uses detailed nuclear structure inputs, combining chiral effective field theory and shell-model calculations to derive cross sections and capture rates.
• Experimental bounds from direct detection and neutrino telescopes tightly connect theory with astrophysical observations, refining dark matter interaction constraints.

Spin-dependent WIMP (Weakly Interacting Massive Particle) capture refers to the process by which WIMPs, through axial-vector (spin-dependent) interactions, scatter off nucleons inside astrophysical bodies—primarily the Sun and Earth—and lose sufficient kinetic energy to become gravitationally bound. This mechanism directly links the limits from direct detection experiments with indirect searches, such as neutrino telescopes, and is sensitive to the details of both nuclear structure and the particle physics underlying WIMP interactions.

1. Fundamental Formalism for Spin-Dependent WIMP Capture

The capture rate $C$ of WIMPs via spin-dependent (SD) elastic scattering in a body of radius $R$ is given, in the optically thin (single-scattering) limit, by integrating the local dark matter flux times differential cross section over the phase space, spatial distribution, and composition of the capturing body. The master equation, valid for arbitrary nuclear content and halo velocity distribution, is: $$C = \frac{\rho_\chi}{m_\chi} \int_0^R 4\pi r^2 dr \sum_A n_A(r) \int_0^\infty du\, \frac{f(u)}{u} \, w(u,r) \int_{E_{\min}}^{E_{\max}} dE_R \frac{d\sigma_A^{SD}}{dE_R}(w)$$ where:

• $\rho_\chi$ is the local DM density, $m_\chi$ the WIMP mass,
• $f(u)$ is the WIMP speed distribution at infinity,
• $w(u,r) = \sqrt{u^2 + v_{\rm esc}^2(r)}$ is the WIMP speed at radius $r$,
• $n_A(r)$ is the number density of nuclear species $A$ at $R$0,
• $R$1 (the minimum recoil energy for capture),
• $R$2 (the kinematic maximum for a WIMP–nucleus interaction; $R$3 is the reduced mass),
• $R$4 is the differential spin-dependent cross section.

The cross section encodes the particle physics and nuclear structure inputs essential for meaningful predictions and constraints.

2. Spin-Dependent WIMP–Nucleus Cross Section and Nuclear Structure Functions

The spin-dependent WIMP–nucleus cross section depends critically on nuclear spin structure and WIMP couplings. The zero–momentum-transfer differential cross section is typically expressed as: $R$5 where:

• $R$6 is the Fermi constant,
• $R$7 is the spin of the target nucleus,
• $R$8 is the WIMP–nucleus relative speed,
• $R$9 is the nuclear spin structure function.

The structure function decomposes as: $$C = \frac{\rho_\chi}{m_\chi} \int_0^R 4\pi r^2 dr \sum_A n_A(r) \int_0^\infty du\, \frac{f(u)}{u} \, w(u,r) \int_{E_{\min}}^{E_{\max}} dE_R \frac{d\sigma_A^{SD}}{dE_R}(w)$$0 with $$C = \frac{\rho_\chi}{m_\chi} \int_0^R 4\pi r^2 dr \sum_A n_A(r) \int_0^\infty du\, \frac{f(u)}{u} \, w(u,r) \int_{E_{\min}}^{E_{\max}} dE_R \frac{d\sigma_A^{SD}}{dE_R}(w)$$1 (isoscalar) and $$C = \frac{\rho_\chi}{m_\chi} \int_0^R 4\pi r^2 dr \sum_A n_A(r) \int_0^\infty du\, \frac{f(u)}{u} \, w(u,r) \int_{E_{\min}}^{E_{\max}} dE_R \frac{d\sigma_A^{SD}}{dE_R}(w)$$2 (isovector) WIMP–nucleon axial-vector couplings. For practical application, calculations such as those in "Large-scale nuclear structure calculations for spin-dependent WIMP scattering with chiral effective field theory currents" (Klos et al., 2013) provide $$C = \frac{\rho_\chi}{m_\chi} \int_0^R 4\pi r^2 dr \sum_A n_A(r) \int_0^\infty du\, \frac{f(u)}{u} \, w(u,r) \int_{E_{\min}}^{E_{\max}} dE_R \frac{d\sigma_A^{SD}}{dE_R}(w)$$3 for relevant isotopes, incorporating both state-of-the-art shell-model wavefunctions and leading long-range two-body chiral EFT currents. Two-body currents induce a universal suppression of the isovector coupling by $$C = \frac{\rho_\chi}{m_\chi} \int_0^R 4\pi r^2 dr \sum_A n_A(r) \int_0^\infty du\, \frac{f(u)}{u} \, w(u,r) \int_{E_{\min}}^{E_{\max}} dE_R \frac{d\sigma_A^{SD}}{dE_R}(w)$$415–30%, reducing the total SD cross section by $$C = \frac{\rho_\chi}{m_\chi} \int_0^R 4\pi r^2 dr \sum_A n_A(r) \int_0^\infty du\, \frac{f(u)}{u} \, w(u,r) \int_{E_{\min}}^{E_{\max}} dE_R \frac{d\sigma_A^{SD}}{dE_R}(w)$$5–$$C = \frac{\rho_\chi}{m_\chi} \int_0^R 4\pi r^2 dr \sum_A n_A(r) \int_0^\infty du\, \frac{f(u)}{u} \, w(u,r) \int_{E_{\min}}^{E_{\max}} dE_R \frac{d\sigma_A^{SD}}{dE_R}(w)$$6 (Divari et al., 2013, Menendez et al., 2012).

At zero momentum transfer ($$C = \frac{\rho_\chi}{m_\chi} \int_0^R 4\pi r^2 dr \sum_A n_A(r) \int_0^\infty du\, \frac{f(u)}{u} \, w(u,r) \int_{E_{\min}}^{E_{\max}} dE_R \frac{d\sigma_A^{SD}}{dE_R}(w)$$7), $$C = \frac{\rho_\chi}{m_\chi} \int_0^R 4\pi r^2 dr \sum_A n_A(r) \int_0^\infty du\, \frac{f(u)}{u} \, w(u,r) \int_{E_{\min}}^{E_{\max}} dE_R \frac{d\sigma_A^{SD}}{dE_R}(w)$$8 reduces to a form involving the proton and neutron spin expectation values $$C = \frac{\rho_\chi}{m_\chi} \int_0^R 4\pi r^2 dr \sum_A n_A(r) \int_0^\infty du\, \frac{f(u)}{u} \, w(u,r) \int_{E_{\min}}^{E_{\max}} dE_R \frac{d\sigma_A^{SD}}{dE_R}(w)$$9 and $\rho_\chi$0, leading to cross sections: $\rho_\chi$1 with $\rho_\chi$2 (proton) and $\rho_\chi$3 (neutron) couplings.

3. Effective Theory and Operator Structure in Spin-Dependent Scattering

Spin-dependent capture is controlled by a set of operators within the non-relativistic effective field theory (NREFT) framework, which systematically enumerates all allowed Galilean-invariant interactions for a WIMP with spin $\rho_\chi$4 (Kang et al., 2022, Widmark, 2017). Key SD operators include:

• $\rho_\chi$5 (axial–axial, "standard" SD),
• $\rho_\chi$6 (momentum-suppressed SD),
• $\rho_\chi$7 (spin-velocity),
• $\rho_\chi$8, $\rho_\chi$9, etc. (spin–momentum and mixed operators).

Each operator gives rise to a unique combination of nuclear response functions ($m_\chi$0 etc.), with the canonical SD interaction mediated by $m_\chi$1 channels. In the case of a massless mediator ($m_\chi$2 propagator), cross sections are IR-enhanced and require regularization (see Section 5).

The NREFT capture rate can be written as a bilinear in Wilson coefficients $m_\chi$3, integrated over response and halo functions: $m_\chi$4 as implemented in flexible codes such as WimPyC (Kang et al., 24 Oct 2025).

4. Experimental Direct Detection Constraints and Their Folding into Capture

Direct detection experiments (e.g., LUX, PICO, XENONnT) set upper limits on SD cross sections, usually quoted for pure proton ($m_\chi$5) and neutron ($m_\chi$6) couplings. For instance, LUX Run 3 reports 90% CL bounds at $m_\chi$7 GeV/c$m_\chi$8: $m_\chi$9 cm$f(u)$0 and $f(u)$1 cm$f(u)$2 (Collaboration et al., 2016). These constraints, together with nuclear spin values, map onto capture cross sections for target nuclei in astrophysical bodies.

To connect direct search results to capture, one translates per-nucleon cross section bounds into per-nucleus quantities using: $f(u)$3 and incorporates these into the full capture integrals.

The capture rate for hydrogen (dominant in the Sun) thus scales generically as: $f(u)$4 where $f(u)$5 encodes the solar potential and velocity integrals (Collaboration et al., 2016, Baum et al., 2016).

5. Astrophysical Capture Phenomenology and Halo-Independent Approaches

Capture by the Sun is extremely sensitive to spin-dependent WIMP–proton couplings due to the Sun's high $f(u)$6H abundance, and by neutron couplings in the case of neutron-rich elements in the Earth or in direct detection targets (Baum et al., 2016). Capture rates for the Sun with $f(u)$7 cm$f(u)$8 and $f(u)$9 GeV yield $w(u,r) = \sqrt{u^2 + v_{\rm esc}^2(r)}$0 s$w(u,r) = \sqrt{u^2 + v_{\rm esc}^2(r)}$1. For the Earth, including all relevant isotopes enhances the rate by a factor of three over previous tabulations (Baum et al., 2016).

Uncertainties in the local halo WIMP velocity distribution translate into uncertainties in capture rates and derived cross section limits. The Standard Halo Model (SHM)—a truncated Maxwell-Boltzmann velocity distribution—can yield bounds that are up to orders of magnitude stronger than those obtained using strictly halo-independent (single-stream) methods. In the latter, the most conservative bound on coupling constants $w(u,r) = \sqrt{u^2 + v_{\rm esc}^2(r)}$2 at fixed $w(u,r) = \sqrt{u^2 + v_{\rm esc}^2(r)}$3 is derived by maximizing over all possible $w(u,r) = \sqrt{u^2 + v_{\rm esc}^2(r)}$4 subject to normalization (Kang et al., 2022, Choi et al., 2024); for SD WIMP-proton couplings, the relaxation factor compared to SHM is generally $w(u,r) = \sqrt{u^2 + v_{\rm esc}^2(r)}$5 outside the 10–200 GeV region, where it can reach $w(u,r) = \sqrt{u^2 + v_{\rm esc}^2(r)}$6.

Massless mediator scenarios ($w(u,r) = \sqrt{u^2 + v_{\rm esc}^2(r)}$7 enhancement in the amplitude) lead to UV-finite but IR-divergent capture rates unless the maximum WIMP aphelion is limited (the "Jupiter cut"). The single-stream halo-independent method circumvents this sensitivity as it is independent of low-$w(u,r) = \sqrt{u^2 + v_{\rm esc}^2(r)}$8 tails (Choi et al., 2024).

6. Spin-Dependent Capture, Thermalization, and Indirect Detection Probes

After capture, WIMPs thermalize with the stellar nucleus distribution, settling to a density profile described by the solar core temperature and gravitational potential. Thermalization times range from $w(u,r) = \sqrt{u^2 + v_{\rm esc}^2(r)}$9 to $r$0 years depending on operator structure and $r$1; these are nearly always much less than the Solar age of $r$2 yr for cross sections at current experimental limits (Widmark, 2017). Thus, instantaneous thermalization is an excellent approximation except for severely suppressed (e.g., momentum-suppressed) cases.

Captured WIMPs may annihilate to Standard Model products (notably neutrinos for indirect searches). The relationship between capture rate $r$3 and annihilation rate $r$4 depends on the equilibrium condition: $r$5 with $r$6, $r$7 parameterizing the annihilation cross section and effective volume. For $r$8 (equilibrium), $r$9, and neutrino flux limits translate directly into constraints on $n_A(r)$0 and thereby $n_A(r)$1, $n_A(r)$2, or general NREFT couplings (Baum et al., 2016, Liang et al., 2013).

7. Nuclear Structure, Operator Uncertainties, and Renormalization

The nuclear physics underlying spin-dependent capture is characterized by:

• Large-scale shell-model wavefunctions,
• Chiral EFT-derived one-body and two-body axial currents (Menendez et al., 2012, Klos et al., 2013),
• Operator truncations and uncertainty bands arising from nuclear density $n_A(r)$3, low-energy constants $n_A(r)$4, $n_A(r)$5, and shell-model choices.

The dominant uncertainty on computed $n_A(r)$6 and thus on capture rates is $n_A(r)$715–35%, rooted both in nuclear-structure and current-operator truncation. Two-body currents suppress the effective isovector SD coupling by a nearly universal factor $n_A(r)$8–$n_A(r)$9, yielding a $A$00.5–0.6 overall suppression in cross section and capture rate, independent of the nuclear mass number $A$1 (Divari et al., 2013, Klos et al., 2013).

Summary Table: Spin-Dependent Capture—Core Quantities

Quantity	Physical Content	Reference Equation(s)
$A$2	SD differential cross section	$A$3 (Collaboration et al., 2016, Klos et al., 2013)
$A$4	Nuclear spin structure function	$A$5 (Menendez et al., 2012, Klos et al., 2013)
$A$6	Total SD cross section at $A$7	$A$8
$A$9	SD capture rate	See master equations above; e.g., Eq. (7) in (Collaboration et al., 2016)
Renorm. factor $R$00	Two-body-current suppression	$R$01 (Divari et al., 2013, Menendez et al., 2012)

Spin-dependent WIMP capture theory tightly integrates nuclear physics, particle physics operator structure, and astrophysical modeling. The most stringent constraints on $R$02 arise from solar capture (and thus solar neutrino fluxes), especially for contact and massless mediator interactions, while neutron cross section constraints are currently dominated by direct detection with neutron-odd targets. Two-body current effects and halo uncertainties are essential for robust interpretation. These capture rates underpin all indirect probes of WIMP annihilation in astrophysical bodies and constitute the bridge between experimental non-observations and theoretical models of DM scattering.