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EUHFORIA Heliosphere (1.1)

EUropean Heliospheric FORecasting Information Asset Heliosphere

Model Description

The EUHFORIA Heliosphere model is a 3D heliospheric model. It computes the time-dependent evolution of the MHD variables from the interface radius (0.1au) to typically up to 2au. It can accept boundary conditions from a variety of coronal models such as the EUHFORIA coronal model, the MULTI-VP model, the COCONUT model,... CMEs are injected at the interface radius using a hydrodynamic cone-like model using parameters constrained from fits to coronal imaging observations. In order to account for the modification of the heliosphere due to the presence of earlier CMEs, the standard run scenario includes CMEs launched five days prior to the start of the forecast, while the duration of the forecast extends up to seven days.

Model Figure(s) :

Model Inputs Description

Heliospheric component, Time-dependent 3D ideal-MHD model of the inner heliosphere:
2D (longitude-latitude) map of the solar wind MHD parameters at 0.1 AU
Optional: input details of the chosen CMEs (time at inner boundary, latitude, longitude, half-width, speed).

Model Outputs Description

Solar component, Semi-empirical WSA-based model of the solar corona used in combination with the PFSS and the Schatten Current Sheet models:
2D (longitude-latitude) map of the solar wind MHD parameters (vr, Br, n, T) at 0.1 AU, 2D (longitude-latitude) map of the open/closed magnetic field regions, 2D (longitude-latitude) map of the flux tube expansion factor

Heliospheric component, Time-dependent 3D ideal-MHD model of the inner heliosphere:
3D output of the full heliospheric domain (normally upon request); 2D results on the equatorial and meridional plane containing the Earth, in png format; time series at main planetary/spacecraft locations

Model Caveats

Solar component, Semi-empirical WSA-based model of the solar corona used in combination with the PFSS and the Schatten Current Sheet models:
Incidental crashes of the coronal model with the error "Too many NaNs in an array". The error occurs during the calculation of the flux tube expansion factor when too many nan values are bunched together in the magnetic map. A simple averaging procedure that is called to deal with these "bad" values, cannot fix the problem. Other magnetograms during the same day (and of the same provider) are then used, but sometimes the problem remains; therefore, there could be no euhforia run for that day.

Change Log

Model Acknowledgement/Publication Policy (if any)

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Source code of the model is publicly available?

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Linked to Other Spase Resource(s) (example: another SimulationModel) :

Curator: Chiu Wiegand | NASA Official: Dr. Masha Kuznetsova | Privacy and Security Notices | Accessibility | CCMC Data Collection Consent Agreement