Axi-Higgs Cosmology. (arXiv:2102.11257v2 [hep-ph] UPDATED)
<a href="http://arxiv.org/find/hep-ph/1/au:+Fung_L/0/1/0/all/0/1">Leo WH Fung</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Li_L/0/1/0/all/0/1">Lingfeng Li</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Liu_T/0/1/0/all/0/1">Tao Liu</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Luu_H/0/1/0/all/0/1">Hoang Nhan Luu</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Qiu_Y/0/1/0/all/0/1">Yu-Cheng Qiu</a>, <a href="http://arxiv.org/find/hep-ph/1/au:+Tye_S/0/1/0/all/0/1">S.-H. Henry Tye</a>
If the electroweak Higgs vacuum expectation value $v$ in early universe is
$sim 1 %$ higher than its present value $v_0=246$ GeV, the $^7$Li puzzle in
BBN and the CMB/$Lambda$CDM tension with late-universe measurements on Hubble
parameter are mitigated. We propose a model of an axion coupled to the Higgs
field, named “axi-Higgs”, with its mass $m_a sim 10^{-30} – 10^{-29},{rm
eV}$ and decay constant $f_a sim 10^{17} – 10^{18},{rm GeV}$, to achieve
this goal. The axion initial value $a_{rm ini}$ yields an initial $Delta
v_{rm ini}/v_0 sim 0.01$ throughout the BBN-recombination epoch and a percent
level contribution to the total matter density today. Because of its very large
de Broglie wavelength, this axion matter density $omega_a$ suppresses the
matter power spectrum, alleviating the CMB/$Lambda$CDM $S_8/sigma_8$ tension
with the weak-lensing data. It also explains the recently reported isotropic
cosmic birefringence by its coupling with photons. Adding the axion ($m sim
10^{-22},$eV) in the fuzzy dark matter model to the axi-Higgs model allows
bigger $Delta v_{rm rec}$ and $omega_a$ to address the Hubble and
$S_8/sigma_8$ tensions simultaneously. The model predicts that $Delta v$ may
be detected by the spectral measurements of quasars, while its oscillation may
be observed in the atomic clock measurements.
If the electroweak Higgs vacuum expectation value $v$ in early universe is
$sim 1 %$ higher than its present value $v_0=246$ GeV, the $^7$Li puzzle in
BBN and the CMB/$Lambda$CDM tension with late-universe measurements on Hubble
parameter are mitigated. We propose a model of an axion coupled to the Higgs
field, named “axi-Higgs”, with its mass $m_a sim 10^{-30} – 10^{-29},{rm
eV}$ and decay constant $f_a sim 10^{17} – 10^{18},{rm GeV}$, to achieve
this goal. The axion initial value $a_{rm ini}$ yields an initial $Delta
v_{rm ini}/v_0 sim 0.01$ throughout the BBN-recombination epoch and a percent
level contribution to the total matter density today. Because of its very large
de Broglie wavelength, this axion matter density $omega_a$ suppresses the
matter power spectrum, alleviating the CMB/$Lambda$CDM $S_8/sigma_8$ tension
with the weak-lensing data. It also explains the recently reported isotropic
cosmic birefringence by its coupling with photons. Adding the axion ($m sim
10^{-22},$eV) in the fuzzy dark matter model to the axi-Higgs model allows
bigger $Delta v_{rm rec}$ and $omega_a$ to address the Hubble and
$S_8/sigma_8$ tensions simultaneously. The model predicts that $Delta v$ may
be detected by the spectral measurements of quasars, while its oscillation may
be observed in the atomic clock measurements.
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