This article has an erratum: [https://doi.org/10.1051/0004-6361/200913670e]
Volume 511, February 2010
|Number of page(s)||6|
|Published online||10 March 2010|
Letter to the Editor
A scenario of planet erosion by coronal radiation*
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: email@example.com
2 Institut de Ciènces de l'Espai (CSIC-IEEC), Campus UAB, Fac. de Ciències, Torre C5-parell-2 planta, 08193 Bellaterra, Spain
3 INAF – Osservatorio Astronomico di Palermo G. S. Vaiana, Piazza del Parlamento, 1, 90134 Palermo, Italy
4 XMM-Newton 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
Accepted: 8 February 2010
Context. According to theory, high-energy emission from the coronae of cool stars can severely erode the atmospheres of orbiting planets. No observational tests of the long-term erosion effects have been made yet.
Aims. We analyze the current distribution of planetary mass with X-ray irradiation of the atmospheres to make an observational assessment of the consequences of erosion by coronal radiation.
Methods. We studied a large sample of planet-hosting stars with XMM-Newton, Chandra, and ROSAT, carefully identified the X-ray counterparts, and fit their spectra to accurately measure the stellar X-ray flux.
Results. The distribution of the planetary masses with X-ray flux suggests that erosion has taken place. Most surviving massive planets (Mp sin i > 1.5 MJ) have been exposed to lower accumulated irradiation. Heavy erosion during the initial stages of stellar evolution is followed by a phase of much weaker erosion. A line dividing these two phases could be present, showing a strong dependence on planet mass. Although a larger sample will be required to establish a well-defined erosion line, the distribution found is very suggestive.
Conclusions. The distribution of planetary mass with X-ray flux is consistent with a scenario in which planet atmospheres have suffered the effects of erosion by coronal X-ray and EUV emission. The erosion line is an observational constraint for models of atmospheric erosion.
Key words: planetary systems / stars: coronae / astrobiology / X-rays: stars
Table 1 is only available in electronic form at http://www.aanda.org
© ESO, 2010
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