Astronomy & Astrophysics

All Figures

$\begin{figure} \par\psfig{file=3343f1.eps,height=110mm,width=88mm}\end{figure}$ Figure 1: Evolution of the luminosity L and effective temperature $T_{\rm eff}$ as a function of time (in yr) for different masses. Substellar objects are indicated by solid lines and stars by short-dashed lines. The horizontal long-dashed line indicates the limit ( $T_{\rm eff}\sim$ 1300 K) below which the COND models are appropriate for the photometric and spectroscopic description of T-dwarfs and EGPs (see text).
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In the text

$\begin{figure} \par\psfig{file=3343f2.eps,height=110mm,width=88mm}\end{figure}$ Figure 2: Color - Magnitude diagram (J-K) - $M_{\rm K}$ . Observations are taken from Leggett (1992) (mostly for M-dwarfs) and Dahn et al. (2002). Also shown: LHS 102B (Goldman et al. 1999), GL86 (Els et al. 2001). M-dwarfs are shown by dots, L-dwarfs by filled squares and T-dwarfs by triangles. DUSTY isochrones (Chabrier et al. 2000b) are displayed in the upper right part of the figure, for different ages, as indicated. The COND isochrones are displayed in the left part of the figure. Some masses (in $M_\odot$ ) and their corresponding $T_{\rm eff}$ are indicated on the 1 Gyr isochrones by open squares (COND) and open circles (DUSTY). The names of two L/T transition objects and of the faintest T-dwarf known with parallax are indicated.
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In the text

$\begin{figure} \par\psfig{file=3343f3.eps,height=110mm,width=88mm}\end{figure}$ Figure 3: Color - Magnitude diagram (K-L') - $M_{\rm K}$ . K is in the MKO-NIR system. Observations are from Leggett et al. (2002a). Symbols are the same as in Fig. 2. A DUSTY isochrone of 1 Gyr (Chabrier et al. 2000b) is indicated by the long-dashed line. The COND isochrones are displayed for 0.1 Gyr (dash), 1 Gyr (solid) and 10 Gyr (dash-dot). Some masses (in $M_\odot$ ) and their corresponding $T_{\rm eff}$ are indicated on the 1 Gyr COND isochrone by open squares.
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In the text

$\begin{figure} \par\psfig{file=3343f4.eps,height=110mm,width=88mm}\end{figure}$ Figure 4: Color - Magnitude diagram (I-J) - $M_{\rm J}$ . Observations are from Leggett (1992) and Dahn et al. (2002). Symbols and curves are the same as in Fig. 3.
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In the text

$\begin{figure} \par\psfig{file=3343f5.eps,height=110mm,width=88mm}\end{figure}$ Figure 5: Effect of irradiation on atmosphere profiles, T (K) versus P (dyn/cm²), characterized by a surface gravity $\log g = 3.0$ , $T_{\rm eff}$ = 1000 K (upper panel) and $T_{\rm eff}$ = 100 K (lower panel). Dashed lines correspond to nonirradiated structures. Solid lines are irradiated models at a separation a = 0.046 AU from a primary with $T_{{{\rm eff}}_\star }$ = 6000 K. The corresponding equilibrium temperature is $T_{\rm eq} \sim 1630~{\rm K}$ . The squares on the curve refer to optical depth, defined at $\lambda = 1.2~\mu$ m, $\tau _{\rm std}$ = 1 and the circles to $\tau _{\rm std}$ = 100. The triangles indicate the top of the convective zone.
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In the text

$\begin{figure} \par\psfig{file=3343f6.eps,height=110mm,width=88mm}\end{figure}$ Figure 6: Radius (in $R_{\rm J}$ ) versus age (in yr) for EGP masses of 1 $M_{\rm J}$ (lower panel) and 10 $M_{\rm J}$ (upper panel). The dashed lines are nonirradiated models. The solid lines are irradiated models at a separation a = 0.046 AU from the parent star with $T_{{{\rm eff}}_\star }$ = 6000 K. The dotted lines are nonirradiated models from Burrows et al. (1997).
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In the text

$\begin{figure} \par\psfig{file=3343f7.eps,height=110mm,width=88mm}\end{figure}$ Figure 7: Effect of irradiation on the evolution of a planet with $m_{\rm p}=0.69~M_{\rm J}$ at a separation a = 0.046 AU from its parent star with $T_{\rm eff}$ = 6000 K. The panels from top to bottom display respectively the intrinsic luminosity $L_{\rm int}$ , the effective temperature (in K) and the radius versus time (in yr). The solid curves correspond to the irradiated case and the dashed curves to the nonirradiated counterpart. We recall that in the case of irradiation, $T_{\rm eff}$ and $L_{\rm int}$ do not characterize the total flux emitted by the planet. The position of HD 209458b in the lower panel is from Cody & Sasselov (2002).
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In the text

$\begin{figure} \par\psfig{file=3343f8.eps,height=110mm,width=88mm}\end{figure}$ Figure 8: Effect of extra source of energy dissipation on the evolution of a planet with mass $m_{\rm p}=0.69~M_{\rm J}$ . The solid and long-dashed lines correspond to the irradiated and non-irradiated sequences respectively, with no extra source of energy dissipation. The other curves correspond to irradiated sequences with a total amount of additional energy $L_{\rm extra}$ (in erg s^-1) deposited in layers between the surface and the mass shell $m_{\rm p} - \Delta m$ , as indicated in figure (see text).
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In the text

$\begin{figure} \par\psfig{file=3343f4.eps,height=110mm,width=88mm}\end{figure}$	Figure 4: Color - Magnitude diagram (I-J) - $M_{\rm J}$ . Observations are from Leggett (1992) and Dahn et al. (2002). Symbols and curves are the same as in Fig. 3.
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$\begin{figure} \par\psfig{file=3343f6.eps,height=110mm,width=88mm}\end{figure}$	Figure 6: Radius (in $R_{\rm J}$ ) versus age (in yr) for EGP masses of 1 $M_{\rm J}$ (lower panel) and 10 $M_{\rm J}$ (upper panel). The dashed lines are nonirradiated models. The solid lines are irradiated models at a separation a = 0.046 AU from the parent star with $T_{{{\rm eff}}_\star }$ = 6000 K. The dotted lines are nonirradiated models from Burrows et al. (1997).
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