Constraining Chaplygin models using diffuse supernova neutrino background. (arXiv:1904.07510v1 [gr-qc])
<a href="http://arxiv.org/find/gr-qc/1/au:+Yang_N/0/1/0/all/0/1">Nan Yang</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Jia_J/0/1/0/all/0/1">Junji Jia</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Liu_X/0/1/0/all/0/1">Xionghui Liu</a>, <a href="http://arxiv.org/find/gr-qc/1/au:+Zhang_H/0/1/0/all/0/1">Hongbao Zhang</a>
In this work, we examine the possibility of using the diffuse supernova
neutrino background (DSNB) to test the Chaplygin gas (CG) models of the
Universe. With a typical star formation rate $psi(z)$, supernova rate
$R_{mathrm{SN}}(z)$ and single supernova neutrino spectrum $mathrm{d}
N(E_nu)/mathrm{d} E_nu$, the DSNB flux spectrum $n(E_nu)$ in three
categories of CG models, the generalized CG (GCG), modified CG (MCG) and
extended CG (ECG) models, are studied. It is found that generally the flux
spectra take a form similar to a Fermi-Dirac distribution with a peak centered
around 4.55-4.78 MeV. The spectrum shape and peak position are primarily
determined by $psi(z)$, $R_{mathrm{SN}}(z)$ and $mathrm{d}
N(E_nu)/mathrm{d} E_nu$ and only slightly affected by the CG models.
However, the height of the spectra in each category of the CG models can vary
dramatically for different models in each category, with variances 13.2%, 23.6%
and 14.9% for GCG, MCG and ECG categories respectively. The averaged total flux
in each category are also different, with the ECG model average 10% and 12%
higher than that of the GCG and MCG models. These suggest that the DSNB flux
spectrum height and total flux can be used to constrain the CG model
parameters, and if the measured to a sub-10% accuracy, might be used to rule
out some models.
In this work, we examine the possibility of using the diffuse supernova
neutrino background (DSNB) to test the Chaplygin gas (CG) models of the
Universe. With a typical star formation rate $psi(z)$, supernova rate
$R_{mathrm{SN}}(z)$ and single supernova neutrino spectrum $mathrm{d}
N(E_nu)/mathrm{d} E_nu$, the DSNB flux spectrum $n(E_nu)$ in three
categories of CG models, the generalized CG (GCG), modified CG (MCG) and
extended CG (ECG) models, are studied. It is found that generally the flux
spectra take a form similar to a Fermi-Dirac distribution with a peak centered
around 4.55-4.78 MeV. The spectrum shape and peak position are primarily
determined by $psi(z)$, $R_{mathrm{SN}}(z)$ and $mathrm{d}
N(E_nu)/mathrm{d} E_nu$ and only slightly affected by the CG models.
However, the height of the spectra in each category of the CG models can vary
dramatically for different models in each category, with variances 13.2%, 23.6%
and 14.9% for GCG, MCG and ECG categories respectively. The averaged total flux
in each category are also different, with the ECG model average 10% and 12%
higher than that of the GCG and MCG models. These suggest that the DSNB flux
spectrum height and total flux can be used to constrain the CG model
parameters, and if the measured to a sub-10% accuracy, might be used to rule
out some models.
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