A scenario of planet erosion by coronal radiation (Corrigendum)^*

J. Sanz-Forcada¹, I. Ribas², G. Micela³, A. M. T. Pollock⁴, D. García-Álvarez^5,6, E. Solano^1,7 and C. Eiroa⁸

¹ Laboratorio de Astrofísica Estelar y Exoplanetas, Centro de Astrobiología / CSIC-INTA, LAEFF Campus, PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain e-mail: jsanz@cab.inta-csic.es
² Institut de Ciènces de l'Espai (CSIC-IEEC), Campus UAB, Fac. de Ciències, Torre C5-parell-2a planta, 08193 Bellaterra, Spain
³ INAF – Osservatorio Astronomico di Palermo G. S. Vaiana, Piazza del Parlamento 1, 90134 Palermo, Italy
⁴ SOC, European Space Agency, ESAC, Apartado 78, 28691 Villanueva de la Cañada, Madrid, Spain
⁵ Instituto de Astrofísica de Canarias, 38205 La Laguna, Spain
⁶ Grantecan CALP, 38712 Breña Baja, La Palma, Spain
⁷ Spanish Virtual Observatory, Centro de Astrobiología / CSIC-INTA, LAEFF Campus, Madrid, Spain
⁸ Dpto. de Física Teórica, C-XI, Facultad de Ciencias, Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain

Abstract

In the notes to Table 1, a unit conversion was incorrect. The text should read 1 M_J Gyr^-1 = 6.02e+13 g s^-1. As a consequence in the 3rd paragraph of Sect. 3, the mass loss taking place in τ Boo b should be = 0.011 M_J Gyr^-1 for ρ = 1 g cm^-3, or = 3.4  Gyr^-1 in Earth mass units. 
Independently, the values of “ accumulated”, in Col. 12 of Table 1 were calculated using an obsolete formula and were thus slightly underestimated, generally by 0.2. As a consequence Fig. 2 should show all values at a slightly higher position, although this is of no relevance for the conclusions of the paper. Table 1 and Fig. 2 are reproduced in their correct version here. At the end of 5th paragraph of Sect. 2, the hard limit of X-ray flux accumulated after 10 Gyr should be ~10^22.14 erg cm^-2, instead of ~10^21.76 erg cm^-2, and our highest flux is now 10^21.23 erg cm^-2 instead of 10^21.05 erg cm^-2.