We use photometric and spectroscopic observations of the detached eclipsing binaries V40 and V41 in the globular cluster NGC 6362 to derive masses , radii , and luminosities of the component stars .
The orbital periods of these systems are 5.30 and 17.89 d , respectively .
The measured masses of the primary and secondary components ( M _ { p } , M _ { s } ) are ( 0.8337 \pm 0.0063 , 0.7947 \pm 0.0048 ) M _ { \odot } for V40 and ( 0.8215 \pm 0.0058 , 0.7280 \pm 0.0047 ) M _ { \odot } for V41 .
The measured radii ( R _ { p } , R _ { s } ) are ( 1.3253 \pm 0.0075 , 0.997 \pm 0.013 ) R _ { \odot } for V40 and ( 1.0739 \pm 0.0048 , 0.7307 \pm 0.0046 ) R _ { \odot } for V41 .
Based on the derived luminosities , we find that the distance modulus of the cluster is 14.74 \pm 0.04 mag – in good agreement with 14.72 mag obtained from CMD fitting .
We compare the absolute parameters of component stars with theoretical isochrones in mass-radius and mass-luminosity diagrams .
For assumed abundances [ Fe/H ] = -1.07 , [ \alpha /Fe ] = 0.4 , and Y = 0.25 we find the most probable age of V40 to be 11.7 \pm 0.2 Gyr , compatible with the age of the cluster derived from CMD fitting ( 12.5 \pm 0.5 Gyr ) .
V41 seems to be markedly younger than V40 .
If independently confirmed , this result will suggest that V41 belongs to the younger of the two stellar populations recently discovered in NGC 6362 .
The orbits of both systems are eccentric .
Given the orbital period and age of V40 , its orbit should have been tidally circularized some \sim 7 Gyr ago .
The observed eccentricity is most likely the result of a relatively recent close stellar encounter .

Key words : binaries : eclipsing – binaries : spectroscopic – globular clusters : individual ( NGC 6362 ) – stars : individual ( V40 NGC 6362 , V41 NGC 6362 )

†Deceased ^ { \mathrm { \ast } } This paper includes data gathered with the 6.5-m Magellan Baade and Clay Telescopes , and the 2.5-m du Pont Telescope located at Las Campanas Observatory , Chile .