Astronomy & Astrophysics

All Figures

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=-90,clip=]{EFEri_501_PN_MOS_spec_wabs_mekal_1_1.ps}}\end{figure}$ Figure 1: Mean X-ray spectrum of EF Eri (observation E501) and best-fit thermal plasma model.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{7.5cm}{!}{\includegraphics[angle=-90,clip=]{EFEri_201_OM_V_lc_p.ps}}\end{figure}$ Figure 2: OM light curve through V-filter from observation E201. The bin size is 243 s corresponding to 0.05 phase units.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip=]{sed_uv_opt.ps}}\end{figure}$ Figure 3: Ultraviolet to infrared spectral energy distribution of EF Eri in the low state. Shown are an optical low-state spectrum and infrared JHK photometry adapted from Harrison et al. (2004), GALEX-UV and optical BVRI photometry from Szkody et al. (2006, blue dots), OM V-band and UVW1-photometry (red dots), and the result of our spectral synthesis with a two-temperature model (see text for details) Whenever possible, orbital minimum and maximum brightness are indicated and connected by lines
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip=]{sed_ir_x_mod.ps}}\end{figure}$ Figure 4: Infrared to X-ray spectral energy distribution of EF Eri in the low state. Shown are radiation components which are associated with the accretion process, i.e. corrected for stellar photospheric radiation, at orbital maximum. The red arrow indicates the cyclotron fundamental for B=14 MG.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[angle=-90,clip=]{EFEri_501_PN_MOS_spec_wabs_mekal_1_1.ps}}\end{figure}$	Figure 1: Mean X-ray spectrum of EF Eri (observation E501) and best-fit thermal plasma model.
Open with DEXTER

$\begin{figure} \par\resizebox{7.5cm}{!}{\includegraphics[angle=-90,clip=]{EFEri_201_OM_V_lc_p.ps}}\end{figure}$	Figure 2: OM light curve through V-filter from observation E201. The bin size is 243 s corresponding to 0.05 phase units.
Open with DEXTER

$\begin{figure} \par\resizebox{8.5cm}{!}{\includegraphics[clip=]{sed_ir_x_mod.ps}}\end{figure}$	Figure 4: Infrared to X-ray spectral energy distribution of EF Eri in the low state. Shown are radiation components which are associated with the accretion process, i.e. corrected for stellar photospheric radiation, at orbital maximum. The red arrow indicates the cyclotron fundamental for B=14 MG.
Open with DEXTER