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Ultra-High Energy Astro-Particle Physics

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A Search for Ultra-High Energy Neutrinos and Cosmic-Rays with ANITA-2

Part of the book series: Springer Theses ((Springer Theses))

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Abstract

Understanding the high energy Universe has been a long standing goal of astro-particle physics.

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Notes

  1. 1.

    \(\gamma \gamma \rightarrow e^+e^-\) will begin to limit the photon horizon at \(10^{14}\) eV.

  2. 2.

    The energy spectrum produced by supernovae shock fronts is \(\gamma \sim 2\). However, when combined with the confinement time in the Galaxy, a spectrum of \(\gamma \sim 2.6\) is produced.

  3. 3.

    1 erg = \(10^{-7}\) J.

  4. 4.

    It is also possible that the observed high energy cut-off is caused by the end of the energy spectrum that UHECR sources are able to generate.

  5. 5.

    The radiation length is the length over which a particle will lose all but 1/\(e\) of its energy.

  6. 6.

    The critical energy is the energy at which an electron’s rate of energy loss due to ionisation is equal to the rate of energy loss due to bremsstrahlung radiation. Ionisation interactions do not create any new particles, while bremsstrahlung energy losses result in a photon, which may proceed to pair produce, thus adding to the total number of particles in the shower. Therefore, at \(E<E_c\), particles will not be added to the shower.

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Authors and Affiliations

  1. University College London, London, UK

    Matthew Joseph Mottram

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  1. Matthew Joseph Mottram
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Correspondence to Matthew Joseph Mottram .

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Mottram, M.J. (2012). Ultra-High Energy Astro-Particle Physics. In: A Search for Ultra-High Energy Neutrinos and Cosmic-Rays with ANITA-2. Springer Theses. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-642-30032-5_3

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  • DOI: https://doi.org/10.1007/978-3-642-30032-5_3

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