the_nu_wgv

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the_nu_wgv [2014/06/18 19:08] willcox |
the_nu_wgv [2014/07/01 14:24] (current) vassh |
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- | Members: Don Willcox, Nicole Vassh, Panos Gastis | + | ===== The $\nu$ WGV Group Members ===== |

+ | * Don Willcox (code/parameters) | ||

+ | * Nicole Vassh (parameters/analysis) | ||

+ | * Panos Gastis (code/analysis) | ||

+ | |||

+ | ===== Project Goal ===== | ||

+ | |||

+ | To examine the effect of the neutrino magnetic moment on the primordial abundances. This will be done by considering the magnetic moment as a free parameter (presumably larger than the standard model prediction). This additional magnetic moment coupling will then keep the neutrinos coupled to the electrons past the traditional $\sim 1$ MeV temperature. Here we preliminarily consider the effect on primordial abundances when the magnetic pair-production process $e^{+}+e^{-}\leftrightarrow \nu +\bar{\nu}$ is included into the big bang nucleosynthesis code of F. Timmes. | ||

===== Decoupling Temperature Calculation ===== | ===== Decoupling Temperature Calculation ===== | ||

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We can see that the last term is of order unity when $g_\nu\sim \frac{m_p}{M_{pl}^{1/3}M_W^{2/3}}\sim 10^{-8}$, allowing us to rewrite the equation as: | We can see that the last term is of order unity when $g_\nu\sim \frac{m_p}{M_{pl}^{1/3}M_W^{2/3}}\sim 10^{-8}$, allowing us to rewrite the equation as: | ||

$$\left(\frac{T}{T_0}\right)^3 = 1 - \left(\frac{g_\nu}{10^{-8}}\right)^2 \frac{T}{T_0}$$ | $$\left(\frac{T}{T_0}\right)^3 = 1 - \left(\frac{g_\nu}{10^{-8}}\right)^2 \frac{T}{T_0}$$ | ||

+ | |||

+ | ===== Preliminary Results and Presentation ===== | ||

+ | |||

+ | {{:bbnnmm.pdf|}} | ||

+ | |||

+ | ===== Revised Results and Conclusions ===== | ||

+ | |||

+ | {{:nmmabundtalent.pdf|}} | ||

the_nu_wgv.1403132910.txt.gz ยท Last modified: 2014/06/18 19:08 by willcox

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