ExPRES HD 189733 Radio Emission Simulations Dataset
Wednesday 3 September 2025, by Corentin Louis
This dataset is composed of pre-computed Star-Planet Interaction simulation runs of the ExPRES code for the HD 189733 Exoplanetary System with various set of parameters as described in Chebly et al. (2025).
Data directories are hierarchically organised by Poynting flux values, and electron energy. See the Description section below for more details.
Description
This datasets contains pre-computed ExPRES Star-Planet Interaction simulation runs for the HD 189733 exoplanetary system, used in Chebly et al. (2025), with various parameter sets:
Magnetic Field and density Models based on ZDI maps from AWSoM stellar wind simulations (see Chebly et al., 2023). Different cases are proposed based on four different poynting flux.
Electron energy: 1, 20 or 100 keV. Note that for the different values of Poynting flux explored (other than 1e6) , only on simulation at 20 keV was computed.
CMI Mechanism that controls the beaming pattern beaming: Loss Cone
Beaming thickness: 1°
Waves in RX mode.
Near-source refraction are taken into account as the density can be very high close to the studied stars.
Sources are set on magnetic field line connecting the star to the exoplanet at each time step.
The observer is set at Earth.
ExPRES Version 1.4 (Louis et al. 2025) was used.
The data files contain the modelled following parameters: polarization, theta, fp, fc, obs latitude, CML (obs longitude), obs distance, srcfreqmax, srcLongitude, src pos (source position). Detailed informations are available in Louis et al., 2019.
The data files are provided in CDF format, and the ExPRES input files are JSON files. The magnetic field and density models are supplied in csv format (1 file per field line, in a zip file).
Coverage
June 2006 to December 2006 for HD 189733
Results
Different electron energy exploration
HD 189733
Figure B.3
Frequency–time diagrams for the HD189733 system, shown across the 7 simulations epochs (from June 2006 to December 2006, top to bottom). Each row corresponds to one epoch. The first three columns represent different electron energies for a loss cone distribution: 1 keV, 20 keV, and 100 keV (from left to right).
Poynting flux exploration
HD 189733
Figure C.3
Simulated time-frequency diagrams for three different cases of Poynting flux (S/B) in the HD 189733 system. From left to right, the columns represent low, medium, and high S/B. Each of the seven rows corresponds to a different observational epoch, spanning from June to December 2006.
Acknowledgments
The authors acknowledge funding from the ERC under the European Union’s Horizon 2020 research and innovation program (grant agreement no 101020459 - Exoradio). J. J. C. and A.S. acknowledge funding from the European Research Council project ExoMagnets (grant agreement no. 101125367) and the PLATO/CNES grant at CEA/IRFU/DAp.
References
Chebly, J. J, J. D. Alvarado-Gómez, K. Poppenhäger, C. Garraffo. 2023. "Numerical quantification of the wind properties of cool main sequence stars". Monthly Notices of the Royal Astronomical Society, Volume 524 (October), Issue 4 , Pages 5060–5079, doi:10.1093/mnras/stad2100.
Chebly, J. J., C.K. Louis, A. Strugarek, J. D. Alvarado-Gómez, P. Zarka. 2025. "Predicting realistic radio emission from compact star-planet systems". Astronomy & Astrophysics. doi:tba
Louis, C K, S L G Hess, B Cecconi, P Zarka, L Lamy, S Aicardi, and A Loh. 2019. “ExPRES: an Exoplanetary and Planetary Radio Emissions Simulator.” Astronomy and Astrophysics 627 (May): A30. doi:10.1051/0004-6361/201935161.
Louis, C. K., Hess, S. L. G., Cecconi, B., Zarka, P., Lamy, L., Aicardi, S., & Loh, A. (2025). maserlib/ExPRES: Version 1.4.0 (1.4.0). Zenodo. https://doi.org/10.5281/zenodo.17047296
