Exploring the singlet scalar dark matter from direct detections and neutrino signals via its annihilation in the Sun

TL;DR

This paper investigates singlet scalar dark matter models through direct detection experiments and neutrino signals from solar annihilation, analyzing their compatibility with current experimental limits and potential signals in neutrino telescopes.

Contribution

It compares two singlet scalar dark matter models, assessing their neutrino signals and direct detection constraints, and explores parameter adjustments to evade experimental bounds.

Findings

Predicted neutrino fluxes slightly exceed Super-Kamiokande limits for certain masses in SSDM-SM.

Current direct detection experiments exclude some parameter regions.

Predicted muon fluxes are below experimental upper bounds for allowed parameter space.

Abstract

We explore the singlet scalar dark matter (DM) from direct detections and high energy neutrino signals generated by the solar DM annihilation. Two singlet scalar DM models are discussed, one is the real singlet scalar DM model as the simple extension of the standard model (SSDM-SM) with a discrete Z_2 symmetry, and another is the complex singlet scalar DM model as the simple extension of the left-right symmetric two Higgs bidoublet model (SSDM-2HBDM) with $P$ and CP symmetries. To derive the Sun capture rate, we consider the uncertainties in the hadronic matrix elements and calculate the spin-independent DM-nucleon elastic scattering cross section. We find that the predicted neutrino induced upgoing muon fluxes in the region 3.7 GeV < m_D < 4.2 GeV slightly exceed the Super-Kamiokande limit in the SSDM-SM. However, this exceeded region can be excluded by the current DM direct detection experiments. For the SSDM-2HBDM, one may adjust the Yukawa couplings to avoid the direct detection limits and enhance the predicted muon fluxes. For the allowed parameter space of the SSDM-SM and SSDM-2HBDM, the produced muon fluxes in the Super-Kamiokande and muon event rates in the IceCube are less than the experiment upper bound and atmosphere background, respectively.