Axion Gamma-Ray Signatures from Quark Matter in Neutron Stars. (arXiv:2004.08722v3 [astro-ph.HE] UPDATED)

<a href="http://arxiv.org/find/astro-ph/1/au:+Berenji_B/0/1/0/all/0/1">Bijan Berenji</a>

We present a theoretical model for detecting axions from neutron stars in a

QCD phase of quark matter, in which the gamma-rays are produced from decaying

axions. The axions would be produced from a quark-antiquark pair $ubar{u}$ or

$dbar{d}$. The chiral anomaly of QCD and the spontaneously broken symmetry are

invoked to explain the non-conservation of the axion current. The axion

quark-antiquark coupling can be computed via the Goldberger-Treiman relation,

relying on the two-loop coupling form factors from the QCD axion current. From

the coupling form factors, the axion emissivities $epsilon_a$ can be derived,

from which fluxes can be determined. A Monte Carlo simulation is used to

compute the emissivity for axions from said neutron stars, from which the

predicted gamma-ray signal from the Fermi Large Area Telescope (Fermi LAT) can

be computed. We predict a photon flux which may be detectable by Fermi LAT, and

limits on the QCD mass $m_a$. A signal from LIGO GWS 170817 could be produced

from the neutron star merger as well, which is compared to the expected signal

from the Fermi LAT. An upper bound $m_alesssim 10^{-10}$eV is thereby placed.

Very stringent limits on the axion mass of nearly $m_a simeq 10^{-14}$eV could

be placed using this model with the closest neutron stars near 100 kpc. Axions

could thus be detectable in gamma-rays for neutron stars as distant as 1 Mpc.

We present a theoretical model for detecting axions from neutron stars in a

QCD phase of quark matter, in which the gamma-rays are produced from decaying

axions. The axions would be produced from a quark-antiquark pair $ubar{u}$ or

$dbar{d}$. The chiral anomaly of QCD and the spontaneously broken symmetry are

invoked to explain the non-conservation of the axion current. The axion

quark-antiquark coupling can be computed via the Goldberger-Treiman relation,

relying on the two-loop coupling form factors from the QCD axion current. From

the coupling form factors, the axion emissivities $epsilon_a$ can be derived,

from which fluxes can be determined. A Monte Carlo simulation is used to

compute the emissivity for axions from said neutron stars, from which the

predicted gamma-ray signal from the Fermi Large Area Telescope (Fermi LAT) can

be computed. We predict a photon flux which may be detectable by Fermi LAT, and

limits on the QCD mass $m_a$. A signal from LIGO GWS 170817 could be produced

from the neutron star merger as well, which is compared to the expected signal

from the Fermi LAT. An upper bound $m_alesssim 10^{-10}$eV is thereby placed.

Very stringent limits on the axion mass of nearly $m_a simeq 10^{-14}$eV could

be placed using this model with the closest neutron stars near 100 kpc. Axions

could thus be detectable in gamma-rays for neutron stars as distant as 1 Mpc.

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