University of Hertfordshire

From the same journal

From the same journal

By the same authors


  • Roberto Galván-Madrid
  • Hauyu Baobab Liu
  • Carlo Felice Manara
  • Jan Forbrich
  • Ilaria Pascucci
  • Carlos Carrasco-González
  • Ciriaco Goddi
  • Yasuhiro Hasegawa
  • Michihiro Takami
  • Leonardo Testi
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Original languageEnglish
Article numberL9
Number of pages5
JournalAstronomy & Astrophysics
Publication statusPublished - 21 Oct 2014


Photoevaporation due to high-energy stellar photons is thought to be one of the main drivers of protoplanetary disk dispersal. The fully or partially ionized disk surface is expected to produce free-free continuum emission at centimeter (cm) wavelengths that can be routinely detected with interferometers such as the upgraded Very Large Array (VLA). We use deep (rms noise down to 8 $\mu$Jy beam$^{-1}$ in the field of view center) 3.5 cm maps of the nearby (130 pc) Corona Australis (CrA) star formation (SF) region to constrain disk photoevaporation models. We find that the radio emission from disk sources in CrA is surprisingly faint. Only 3 out of 10 sources within the field of view are detected, with flux densities of order $10^2$ $\mu$Jy. However, a significant fraction of their emission is non-thermal. Typical upper limits for non-detections are $3\sigma\sim 60~\mu$Jy beam$^{-1}$. Assuming analytic expressions for the free-free emission from extreme-UV (EUV) irradiation, we derive stringent upper limits to the ionizing photon luminosity impinging on the disk surface $\Phi_\mathrm{EUV}


R. Galván-Madrid, et al., “Constraints on photoevaporation models from (lack of) radio emission in the Corona Australis protoplanetary disks”, Astronomy & Astrophysics, Vol. 570, October 2014. This version of record is available online at: Reproduced with Permission from Astronomy and Astrophysics, © ESO 2014.

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