WebRun

The webrun service allows you to run a simulation directly from your web browser. You do not need to download, install and run any code on your computer. In this way we invite the community to use our tools for their needs.

Status and features of the WebRun

For a given cosmic ray spectrum the simulation provides the the expected degree of ionization inside a Molecular Cloud. Furthermore, the gamma-ray emission observed at Earth is calculated resulting from the assumed CR spectrum. A detailed documentaion will provided soon, till then you find a list of the most prominent features below.

Webrun features

Input spectra

  • Individual input spectra for electrons/protons
  • power law or broken power law in momentum
  • Min/Max models for "CR sea" spectra

Ionisation

  • calculation for CR protons and/or electrons
  • fully relativistic differential cross sections
  • selfconsitent calculation of secondary ionisations
  • assumed target cloud consists of pure molecular hydrogen
  • straight line propagation (energy losses) to the column density of interrest
  • determination of the part of the CR spectrum responsible for 90% of the ionisation

Gamma-ray emission

  • calculation for proton proton interactions (based on Kafexhui et al. 2014)
  • different cross section models for high energies
  • nuclear enhancement factor

In the near future the following updates will be implemented.

  • arbitrary input spectra via file upload
  • leptonic processes (Bremsstrahlung and Inverse Compton)
  • result acess via email/download
  • detailed documentation
  • Webrun Interface

    --- mouse over options/input-fields to get a compact explanation ---

    How to:
    1.) Chose your CR proton and/or electron spectrum
    2.) Select what you want to calculate (Ionisation and/or gamma-rays)
    3.) Chose among the additional options for the individual calculations
    4.) Click submit, your results will be ready in 10-40 seconds

    Selecting the CR spectra

    Chose your CR-proton spectrum

    Power law in momentum

    s = p0= eV/c
    KN = (cm*eV/c)^{-3}

    Broken power law in momentum

    s1 = s2 =
    pbr= eV/c KN = (cm*eV/c)^{-3}

    Models for the average CR spectra in the galaxy ("CR sea")

    Minimum model (see Padovani 2009)
    Maximum model (see Padovani 2009)
    Upload (in preparation)
    Select file to upload:

    Chose your CR-electron spectrum

    Power law in momentum

    s = p0= eV/c
    KN = (cm*eV/c)^{-3}

    Broken power law in momentum

    s1 = s2 =
    pbr= eV/c KN = (cm*eV/c)^{-3}

    Models for the average CR spectra in the galaxy ("CR sea")

    Minimum model (see Padovani 2009)
    Maximum model (see Padovani 2009)
    Upload (in preparation)
    Select file to upload:

    Settings for CR ionization

    Calculate Ionization
    Emin= eV
    CR species
    Straight line propagation
    Column denisty H2: cm^2

    Settings for Gamma-ray emission

    Calculate Gamma ray flux at Earth (pp)
    Emax= eV
    Distance= kpc
    Mass of the molecular cloud= Solar Masses
    Cross-section Model
    nuclear enhancement factor (cloud + CR)

    Request simulation

    After specifiying your CR spectra and which calculations you are interested in, click the submit button below. A calculation takes 10-40 seconds to be carried out. Therefore, please be patient for the results to be displayed below.

    Send results by email (in preparation)

    You can get the results of your run by email. Write your email address below and press the button.

    Email address:

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