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ExPRES Tau Bootis 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 Tau Bootis Exoplanetary Systems with various set of parameters as described in Chebly et al. (2025).

Link to data repository

Data directories are hierarchically organised by electron energy. See the Description section below for more details.

Description

This datasets contains pre-computed ExPRES Star-Planet Interaction simulation runs for the Tau Bootis 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).
  • Electron energy: 1, 20 or 100 keV.
  • 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

  • October 2010 to April 2011 for Tau Bootis
  • October 2009 to April 2010 for HD179949
  • June 2006 to December 2006 for HD189733

Results

Different electron energy exploration
Tau Bootis

Figure B.1
Frequency–time diagrams for the Tau Boo system, shown across the 7 simulations epochs (from October 2010 to April 2011, 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).

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

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