EDP Sciences
The CoRoT space mission: early results
Free Access
Issue
A&A
Volume 506, Number 1, October IV 2009
The CoRoT space mission: early results
Page(s) 15 - 32
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361/200911657
Published online 03 September 2009

Online Material

Table 10:   HD 49933 frequencies and height-to-noise posterior estimates for l=0 and l=1 modes for the $M^2_{\rm A}$ model. n is given supposing $\epsilon \in [1,2]$. H/N represents the height-to-noise ratio in the power spectrum.

Table 11:   Height and width posterior estimates for HD 49933 for the model $M^2_{\rm A}$. n is given for the l=0 modes.

Table 12:   Energy posterior estimates for HD 49933, model $M^2_{\rm A}$. n is given for the l=0 modes.

Table 13:   HD 49933 frequencies and height-to-noise posterior estimates for the l=0 and l=1 modes for the $M^2_{\rm B}$ model. n is given supposing $\epsilon \in [1,2]$. H/N represents the height-to-noise ratio in the power spectrum.

Table 14:   Height and width posterior estimates for HD 49933 for the model $M^2_{\rm B}$. n is given for the l=0 modes.

Table 15:   Energy posterior estimates for HD 49933, model $M^2_{\rm B}$. n is given for the l=0 modes.

 \begin{figure}
\par\subfigure{\epsfig{figure=11657_ZD.ps,width=6.cm,height=18cm,angle=90} }
\par
\end{figure} Figure 11:

HD 49933 power spectrum and echelle diagram for $M^2_{\rm A}$ model (identification A with l=2 modes). The superimposed dashed line is the best fit according to the median value of the parameters.

Open with DEXTER

 \begin{figure}
\par\subfigure{\epsfig{figure=11657_ZE.ps,width=6.cm,height=18cm,angle=90} }
\par
\end{figure} Figure 12:

HD 49933 power spectrum and echelle diagram for $M^1_{\rm B}$ model (identification B without l=2 modes). The superimposed dashed line is the best fit according to the median value of the parameters.

Open with DEXTER


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