Warming nuclear pasta with dark matter: kinetic and annihilation heating of neutron star crusts

Abstract

Neutron stars serve as excellent next-generation thermal detectors of dark matter, heated by the scattering and annihilation of dark matter accelerated to relativistic speeds in their deep gravitational wells. However, the dynamics of neutron star cores are uncertain, making it difficult at present to unequivocally compute dark matter scattering in this region. On the other hand, the physics of an outer layer of the neutron star, the crust, is more robustly understood. We show that dark matter scattering solely with the low-density crust still kinetically heats neutron stars to infrared temperatures detectable by forthcoming telescopes. We find that for both spin-independent and spin-dependent scattering on nucleons, the crust-only cross section sensitivity is 10 −43 − 10 −41 cm 2 for dark matter masses of 100 MeV − 1 PeV, with the best sensitivity arising from dark matter scattering with a crust constituent called nuclear pasta (including gnocchi, spaghetti, and lasagna phases). For dark matter masses from 10 eV to 1 MeV, the sensitivity is 10 −39 − 10 −34 cm 2 , arising from exciting collective phonon modes in a neutron superfluid in the inner crust. Furthermore, for any s-wave or p-wave annihilating dark matter, we show that dark matter will efficiently annihilate by thermalizing just with the neutron star crust, regardless of whether the dark matter ever scatters with the neutron star core. This implies efficient annihilation in neutron stars for any electroweakly interacting dark matter with inelastic mass splittings of up to 200 MeV, including Higgsinos. We conclude that neutron star crusts play a key role in dark matter scattering and annihilation in neutron stars. *

Analytic multi-Baryonic solutions in the SU(N)-Skyrme model at finite density

“…This is standard and given by the matrices in Eqs. ( 13), ( 14) and (15). In particular, we see that we get a Bosonic representation for N odd and a Fermionic representation for N even.…”

“…The properties of nuclear pasta attracted a lot of attention recently (see [6], [7], [8], [13], [14], [15] and references therein), but, due to both the very large Baryon number typical of this phase as well as to the strong interactions between them, only numerical results are available. Moreover, to obtain meaningful numerical results is extremely challenging in these complex systems and a very high computing power is required (as it can be deduced from the references mentioned above).…”

Astroparticle Physics with Compact Objects

“…The constraints on the DM from the kinetic heating have been worked out in detail in Refs. [21,[38][39][40][41].…”

Analytic multi-Baryonic solutions in the SU(N)-Skyrme model at finite density

“…The properties of nuclear pasta attracted a lot of attention recently (see [6][7][8][13][14][15]] and references therein), but, due to both the very large Baryon number typical of this phase as well as to the strong interactions between them, only numerical results are available. Moreover, to obtain meaningful numerical results is extremely challenging in these complex JHEP12(2021)150 systems and a very high computing power is required (as it can be deduced from the references mentioned above).…”