Constraints on millicharged particles by neutron stars

Abstract

We have constrained the charge-mass ($\varepsilon-m$) phase space of millicharged particles through the simulation of the rotational evolution of neutron stars, where an extra slow-down effect due to the accretions of millicharged dark matter particles is considered. For a canonical neutron star of $M=1.4~M_{\odot}$ and $R=10~{\rm km}$ with typical magnetic field strength $B_{0}=10^{12}$ G, we have shown an upper limit of millicharged particles, which is compatible with recently experimental and observational bounds. Meanwhile, we have also explored the influences on the $\varepsilon-m$ phase space of millicharged particles for different magnetic fields $B_{0}$ and dark matter density $\rho_{\rm{DM}}$ in the vicinity of the neutron star.Comment: 5 pages, 3 figure

Bondi accretion of dark matter by neutron stars

“…The main conclusions of this paper [29] are that the released energy due to WIMP annihilation inside the NS might affect the temperature of the star older than 10 7 years, appearing the plateau of surface temperature at ∼ 10 4 K for a typical NS. By the way, besides the above-mentioned heating effects owing to the annihilation of trapped DM particles onto the NS [29][30][31][32][33][34], the rotation effect on the NS was also studied in our previous work [35], based on an enhanced slow-down of neutron stars due to an extra current yield by the accretions of millicharged dark matter particles (MCDM) [36]. We constrained the charge-mass phase space of MC particles through the simulation of the rotational evolution of neutron stars [35].…”

“…By the way, besides the above-mentioned heating effects owing to the annihilation of trapped DM particles onto the NS [29][30][31][32][33][34], the rotation effect on the NS was also studied in our previous work [35], based on an enhanced slow-down of neutron stars due to an extra current yield by the accretions of millicharged dark matter particles (MCDM) [36]. We constrained the charge-mass phase space of MC particles through the simulation of the rotational evolution of neutron stars [35].…”

First Limit on the Direct Detection of Lightly Ionizing Particles for Electric Charge as Low as e/1000 with the Majorana Demonstrator

“…Although the masses of these particles can lie above the reach of current accelerators, experimental constraints on masses and charges of mCPs have been derived from fixed target accelerators [13][14][15][16][17][18][19][20], colliders [21][22][23][24][25][26][27][28], stellar models [3,[29][30][31], cosmic microwave background [29,30,[32][33][34][35][36][37], big-bang nucleosynthesis [30], Supernova 1987A [30,38], neutron stars [39,40], pulsars and gamma ray bursts [41], galaxy clusters [42], the Lamb shift [29,43,44], dark cosmic ray searches [45], positronium decay [46], reactor neutrinos [47,48], and the µ magnetic moment [29]. An early levitation experiment [49] found an indication for the existence for fractional charges that was not confirmed by following efforts [50,…”