# Difference between revisions of "Data Rates"

Line 17: | Line 17: | ||

== Reactions == | == Reactions == | ||

− | ν<sub>e</sub>+{{Ar40}} ⇒ e<sup>-</sup>+ | + | ν<sub>e</sub>+{{Ar40}} ⇒ e<sup>-</sup>+{{K40}}*</sup> |

{{Overline|ν}}<sub>e</sub>+{{Ar40}} ⇒ e<sup>+</sup>+<sup>40</sup>Cl<sup>*</sup> | {{Overline|ν}}<sub>e</sub>+{{Ar40}} ⇒ e<sup>+</sup>+<sup>40</sup>Cl<sup>*</sup> | ||

− | ν<sub>x</sub>+ | + | ν<sub>x</sub>+{{Ar40}} ⇒ ν<sub>x</sub>+{{Ar40}}<sup>*</sup> |

ν<sub>e,x</sub>+e<sup>-</sup> ⇒ ν<sub>e,x</sub>+e<sup>-</sup> | ν<sub>e,x</sub>+e<sup>-</sup> ⇒ ν<sub>e,x</sub>+e<sup>-</sup> |

## Revision as of 00:37, 10 March 2015

# Disclaimer

**This page is in initial stages of construction.**

# Overview

According to the physics goals of the experiment, we need to consider the following main sources of signal:

- The "beam neutrino" signal
- The Supernova Burst (SNB) signal
- Proton Decay
- Solar neutrinos

All these signals have distinct energy scales, topologies and other characteristics. In terms of buffering and processing data in real or near time, they pose different requirements.

# Beam Neutrinos

Because of the energy scale (~GeV range) neutrino interactions will be characterized by TPC signals well above radiological background. Zero-suppression will lead to significant reduction of data volume and rates (the detector will appear "empty" for the most part).

# SNB

## Reactions

ν_{e}+^{40}Ar ⇒ e^{-}+^{40}K*

ν
_{e}+^{40}Ar ⇒ e^{+}+^{40}Cl^{*}

ν_{x}+^{40}Ar ⇒ ν_{x}+^{40}Ar^{*}

ν_{e,x}+e^{-} ⇒ ν_{e,x}+e^{-}

## References

- DocDB 6977 - Software for low-energy signals
- DocDB 8481 - Summary of SNB Working Group Progress (February 2014)

Some reference curves from DocDB 6977:

In a nutshell:

- approximately 100 events per kiloton, spread over ~30 seconds, ~½ in first second
- all flavors, few tens of MeV

# Background

- DocDB 4482 - Craig Thorn's summary of Ar properties

^{39}Ar