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)
• 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

Selecting the CR spectra

Power law in momentum
$\dpi{140}&space;\bg_grey&space;f_{CR}(p)&space;=&space;K_N&space;\left(\frac{p}{p_{br}}&space;\right)^{-s}&space;$
s = p0= eV/c
KN = (cm*eV/c)^{-3}

Broken power law in momentum
$\dpi{140}&space;\bg_grey&space;f_{CR}(p)&space;=&space;K_N&space;\left(\frac{p}{p_{br}}&space;\right)^{-s_2}&space;\left[&space;1&space;+&space;\left(&space;\frac{p}{p_{br}}&space;\right)^{s_2-s_1}&space;\right]^{-1}$
s1 = s2 =
pbr= eV/c KN = (cm*eV/c)^{-3}

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

Power law in momentum
$\dpi{140}&space;\bg_grey&space;f_{CR}(p)&space;=&space;K_N&space;\left(\frac{p}{p_{br}}&space;\right)^{-s}&space;$
s = p0= eV/c
KN = (cm*eV/c)^{-3}

Broken power law in momentum
$\dpi{120}&space;\bg_grey&space;f_{CR}(p)&space;=&space;K_N&space;\left(\frac{p}{p_{br}}&space;\right)^{-s_2}&space;\left[&space;1&space;+&space;\left(&space;\frac{p}{p_{br}}&space;\right)^{s_2-s_1}&space;\right]^{-1}$
s1 = s2 =
pbr= eV/c KN = (cm*eV/c)^{-3}

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

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)