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Acknowledgement

Project acknowledgement

Please cite the original paper: Perri et al. 2020 (JSWSC)

Please visit the MEDOC database for access to the original data: https://www.idoc.osups.universite-paris-saclay.fr/wind_predict_cr/


Galactica database acknowledgement

If you use it in your own work, you may acknowledge the origin of the data obtained on the Galactica database like so:

This work reused datasets available on the Galactica simulations database
(http://www.galactica-simulations.eu)
                            
Cite me
Barbara PERRI  

Cosmic Rays

Summary

This webpage provides output data from MHD simulations performed using the Wind Predict model (Réville et al. 2015. Perri et al. 2018), based on the PLUTO code (Mignone et al. 2007), to simulate the 3D state of the inner heliosphere from the solar surface to the orbit of the Earth. They also include cosmic rays diffusion coefficients parallel and perpendicular to the magnetic field lines, computed using a post-processing Python pipeline. The data is also hosted at the MEDOC database center here.

Available simulations

D1: Dipole of low magnetic amplitude

D10: Dipole of strong magnetic amplitude

Q1: Quadrupole of low magnetic amplitude

MIN: 3D minimum of activity (October 1995)

MAX: 3D maximum of activity (August 1999)

Data description

'Cosmic Rays' project result datafile download

Select the datafiles you wish to export from this project (a zip file containing the requested datafiles will be prepared) :






































































































































Experiment Result Datafile File types File size
D1: Dipole of low magnetic amplitude Physical Quantities PNG 83.9 kB
PNG 54.5 kB
PNG 56.4 kB
PNG 22.2 kB
PNG 18.9 kB
PNG 21.9 kB
PNG 69.7 kB
PNG 54.0 kB
Zoomed physical Quantities PNG 140.9 kB
PNG 158.6 kB
PNG 155.3 kB
PNG 28.7 kB
PNG 36.5 kB
PNG 56.3 kB
PNG 114.1 kB
PNG 115.2 kB
Parallel Mean Free Path (mfp) PNG 150.9 kB
PNG 154.8 kB
PNG 151.5 kB
PNG 154.3 kB
PNG 151.4 kB
PNG 154.5 kB
PNG 151.2 kB
PNG 154.5 kB
PNG 151.6 kB
PNG 154.4 kB
PNG 165.7 kB
PNG 141.6 kB
PNG 141.1 kB
PNG 121.1 kB
Perpendicular Mean Free Path (mfp) PNG 89.8 kB
PNG 133.2 kB
PNG 90.7 kB
PNG 133.6 kB
PNG 90.7 kB
PNG 133.1 kB
PNG 91.1 kB
PNG 132.6 kB
PNG 89.9 kB
PNG 132.6 kB
PNG 91.0 kB
PNG 129.5 kB
PNG 95.1 kB
PNG 125.3 kB
Full Datacube (VTK) TARGZ 218.1 MB
D10: Dipole of strong magnetic amplitude Physical Quantities PNG 109.5 kB
PNG 74.4 kB
PNG 145.7 kB
PNG 46.7 kB
PNG 18.2 kB
PNG 28.7 kB
PNG 88.2 kB
PNG 84.6 kB
Zoomed physical Quantities PNG 137.8 kB
PNG 183.0 kB
PNG 140.8 kB
PNG 27.7 kB
PNG 36.2 kB
PNG 60.0 kB
PNG 116.9 kB
PNG 123.0 kB
Parallel Mean Free Path (mfp) PNG 294.9 kB
PNG 182.5 kB
PNG 294.7 kB
PNG 182.4 kB
PNG 295.3 kB
PNG 182.3 kB
PNG 294.8 kB
PNG 182.8 kB
PNG 294.9 kB
PNG 182.8 kB
PNG 303.7 kB
PNG 177.4 kB
PNG 262.8 kB
PNG 129.6 kB
Perpendicular Mean Free Path (mfp) PNG 126.3 kB
PNG 147.4 kB
PNG 125.6 kB
PNG 147.0 kB
PNG 126.3 kB
PNG 147.4 kB
PNG 127.2 kB
PNG 148.4 kB
PNG 126.1 kB
PNG 147.3 kB
PNG 126.4 kB
PNG 147.2 kB
PNG 127.3 kB
PNG 141.0 kB
Q1: Quadrupole of low magnetic amplitude Physical Quantities PNG 84.1 kB
PNG 76.7 kB
PNG 60.4 kB
PNG 37.6 kB
PNG 20.7 kB
PNG 21.1 kB
PNG 69.6 kB
PNG 52.6 kB
Zoomed physical Quantities PNG 136.7 kB
PNG 145.5 kB
PNG 192.6 kB
PNG 29.6 kB
PNG 30.3 kB
PNG 62.6 kB
PNG 106.9 kB
PNG 105.6 kB
Parallel Mean Free Path (mfp) PNG 243.5 kB
PNG 243.5 kB
PNG 268.9 kB
PNG 243.2 kB
PNG 268.2 kB
PNG 243.4 kB
PNG 268.3 kB
PNG 243.9 kB
PNG 267.6 kB
PNG 244.2 kB
PNG 269.3 kB
PNG 273.6 kB
PNG 237.6 kB
PNG 231.9 kB
PNG 226.7 kB
Perpendicular Mean Free Path (mfp) PNG 127.5 kB
PNG 208.8 kB
PNG 126.5 kB
PNG 207.9 kB
PNG 126.9 kB
PNG 208.9 kB
PNG 126.9 kB
PNG 209.1 kB
PNG 127.4 kB
PNG 209.5 kB
PNG 129.4 kB
PNG 205.5 kB
PNG 133.4 kB
PNG 207.5 kB
Full Datacube (VTK) TARGZ 218.4 MB
MIN: 3D minimum of activity (October 1995) Physical Quantities PNG 71.6 kB
PNG 79.0 kB
PNG 87.8 kB
PNG 41.7 kB
PNG 52.5 kB
PNG 50.6 kB
PNG 30.1 kB
PNG 37.8 kB
PNG 19.4 kB
PNG 17.9 kB
PNG 18.3 kB
PNG 17.8 kB
PNG 72.0 kB
PNG 71.9 kB
PNG 72.8 kB
PNG 72.0 kB
Zoomed physical Quantities PNG 124.8 kB
PNG 137.5 kB
PNG 174.5 kB
PNG 225.9 kB
PNG 143.6 kB
PNG 236.4 kB
PNG 23.6 kB
PNG 29.7 kB
PNG 23.6 kB
PNG 36.3 kB
PNG 17.8 kB
PNG 30.8 kB
PNG 113.3 kB
PNG 126.2 kB
PNG 113.6 kB
PNG 126.4 kB
Parallel Mean Free Path (mfp) PNG 137.7 kB
PNG 115.0 kB
PNG 127.3 kB
PNG 148.5 kB
PNG 138.0 kB
PNG 115.0 kB
PNG 127.6 kB
PNG 148.1 kB
PNG 137.7 kB
PNG 115.0 kB
PNG 127.6 kB
PNG 148.4 kB
PNG 138.6 kB
PNG 115.0 kB
PNG 127.3 kB
PNG 148.5 kB
PNG 137.6 kB
PNG 115.4 kB
PNG 127.0 kB
PNG 148.2 kB
PNG 144.5 kB
PNG 144.6 kB
PNG 119.0 kB
PNG 125.1 kB
PNG 114.9 kB
PNG 154.3 kB
PNG 91.8 kB
PNG 95.5 kB
Perpendicular Mean Free Path (mfp) PNG 93.6 kB
PNG 91.1 kB
PNG 127.3 kB
PNG 145.3 kB
PNG 93.1 kB
PNG 90.6 kB
PNG 126.9 kB
PNG 144.9 kB
PNG 93.4 kB
PNG 90.9 kB
PNG 127.3 kB
PNG 145.3 kB
PNG 94.0 kB
PNG 91.6 kB
PNG 128.1 kB
PNG 145.5 kB
PNG 94.0 kB
PNG 90.8 kB
PNG 127.6 kB
PNG 144.6 kB
PNG 94.2 kB
PNG 94.4 kB
PNG 124.6 kB
PNG 141.9 kB
PNG 98.6 kB
PNG 98.6 kB
PNG 118.9 kB
PNG 133.3 kB
Full Datacube (VTK) TARGZ 349.3 MB
MAX: 3D maximum of activity (August 1999) Physical Quantities PNG 100.1 kB
PNG 100.3 kB
PNG 89.0 kB
PNG 99.2 kB
PNG 76.1 kB
PNG 85.6 kB
PNG 60.2 kB
PNG 51.2 kB
PNG 18.3 kB
PNG 17.7 kB
PNG 18.6 kB
PNG 17.6 kB
PNG 71.6 kB
PNG 73.0 kB
PNG 71.4 kB
PNG 71.0 kB
Zoomed physical Quantities PNG 176.7 kB
PNG 165.3 kB
PNG 187.8 kB
PNG 270.0 kB
PNG 183.2 kB
PNG 257.6 kB
PNG 21.7 kB
PNG 50.9 kB
PNG 20.6 kB
PNG 57.0 kB
PNG 19.9 kB
PNG 38.5 kB
PNG 116.6 kB
PNG 130.0 kB
PNG 114.9 kB
PNG 130.7 kB
Parallel Mean Free Path (mfp) PNG 180.7 kB
PNG 190.6 kB
PNG 174.9 kB
PNG 207.2 kB
PNG 180.2 kB
PNG 190.6 kB
PNG 175.2 kB
PNG 207.1 kB
PNG 181.3 kB
PNG 190.9 kB
PNG 175.2 kB
PNG 207.0 kB
PNG 182.1 kB
PNG 190.5 kB
PNG 175.7 kB
PNG 207.4 kB
PNG 182.9 kB
PNG 191.4 kB
PNG 175.4 kB
PNG 208.1 kB
PNG 190.8 kB
PNG 181.3 kB
PNG 163.5 kB
PNG 191.4 kB
PNG 177.4 kB
PNG 174.8 kB
PNG 126.3 kB
PNG 124.8 kB
Perpendicular Mean Free Path (mfp) PNG 113.6 kB
PNG 122.6 kB
PNG 162.2 kB
PNG 179.0 kB
PNG 113.0 kB
PNG 121.9 kB
PNG 161.6 kB
PNG 178.3 kB
PNG 113.9 kB
PNG 122.6 kB
PNG 162.4 kB
PNG 178.6 kB
PNG 113.7 kB
PNG 122.5 kB
PNG 162.4 kB
PNG 179.0 kB
PNG 113.6 kB
PNG 122.1 kB
PNG 162.1 kB
PNG 178.7 kB
PNG 115.1 kB
PNG 124.5 kB
PNG 159.7 kB
PNG 174.5 kB
PNG 120.9 kB
PNG 129.8 kB
PNG 156.4 kB
PNG 165.8 kB
Full Datacube (VTK) TARGZ 349.9 MB

This data-set includes 5 simulations, 3 of them performed in 2.5D and 2 of them performed in 3D. All simulations correspond to a relaxed state of the wind for a given magnetic field configuration, there is hence no time evolution. The 2.5D simulations are theoretical studies of the influence of the magnetic field on the cosmic rays diffusion: the corona is set at 1.5 M K, and only the magnetic field parameters are changed. Case D1 is a dipole of low amplitude (0.5 G at the surface at the equator), case Q1 is a quadrupole of low amplitude and case D10 is a dipole of strong amplitude (5 G at the surface at the equator). The 3D simulations are set using synoptic maps of a minimum of activity (October 1995) and a maximum of activity (August 1999), already published in another study (Réville & Brun 2017), and run up to 1 AU. Thus we provide 3D maps of the diffusion coefficient of cosmic rays in the inner heliosphere for realistic complex configurations.

The diffusion coefficients are computed using analytical formulae, from Zank et al. 1998 for the parallel diffusion, and from Shalchi et al. 2004 for the perpendicular diffusion. We have selected 7 rigidities for which we perform the computation, at 1, 10, 100, 445, 1e3, 1e4 and 1e5 MV, ranging thus from SEPs to GCRs.

More details can be found in B. Perri, A. S. Brun, A. Strugarek and V. Réville, JSWSC, Topical issue “Space climate: The past and future of solar activity”.

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This material is Open Data