EDP Sciences
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This article is an erratum for: [this article]

Volume 623, March 2019
Article Number C1
Number of page(s) 2
Section Planets and planetary systems
DOI https://doi.org/10.1051/0004-6361/201833435e
Published online 25 February 2019

The q axes of Figs. 1 and 3 are oriented downward, whereas they should be oriented upward. The figures themselves are correct, only the orientation of the axes is wrong.

© ESO 2019

All Figures

thumbnail Fig. 1

From top to bottom panels: distribution of comets in (a, q), (a, cos (iE), (a, ωG) and (a, ΩG) planes at four different epochs t = 250 Myr and 1, 2 and 4 Gyr. For visibility, the bin sizes are constant along any axis. However the density function is computed in number of comets per au for the perihelion distance and per au−1 for the semi-major axis. The data comes from the evolution of the I0 proto-Oort cloud.

Open with DEXTER
In the text
thumbnail Fig. 3

As Fig. 1 but for the D0 proto-Oort cloud.

Open with DEXTER
In the text

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