Chemical depletion in the Large Magellanic Cloud: RV Tauri stars and the photospheric feedback from their dusty discs

Free Access

This article has an erratum: [https://doi.org/10.1051/0004-6361/200912982e]

Table 5:

Results of our SED disc modelling.
	Grain size	$R_{\rm in} - R_{\rm out}$	m	$\alpha$
	$\mu$ m	AU	$10^{-4}~M_{\odot}$
MACHO 79.5501.13	0.1-10	10-30	1	-1.5
MACHO 81.9728.14: S	5	7-100	2	-1.5
MACHO 81.9728.14: C	0.1-10	10-100	0.6	-1.0
MACHO 82.8405.15	0.1-10	17-200	6	-1.3

Note: Given are the used grain-size distribution, the inner and outer radius ( $R_{\rm in}$ - $R_{\rm out}$ ), the total disc mass m for the homogeneous disc model and the surface-density distribution power law $\alpha$ . For MACHO 81.9728.14 we give both the results of the silicate disc model (S), and the carbon disc model (C).

Source LaTeX | All tables | In the text

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.