We analyzed the B and V light curves of two EA-type binaries V211 and NV358 using the WD code for the first time .
Our analysis shows that V211 is a typical Algol-type binary and NV358 is a well detached binary system .
As the two binaries are definite proper motion members of \omega Centauri , we estimated their physical parameters , obtaining M _ { 1 } = 1.13 \pm 0.03 M _ { \odot } , R _ { 1 } = 0.98 \pm 0.01 R _ { \odot } and M _ { 2 } = 0.33 \pm 0.01 M _ { \odot } , R _ { 2 } = 0.92 \pm 0.01 R _ { \odot } for V211 ; M _ { 1 } = 1.30 \pm 0.05 M _ { \odot } , R _ { 1 } = 1.03 \pm 0.01 R _ { \odot } and M _ { 2 } = 0.58 \pm 0.02 M _ { \odot } , R _ { 2 } = 0.78 \pm 0.01 R _ { \odot } for NV358 .
On the color-magnitude diagram of \omega Centauri , V211 is located in the faint blue straggler region and its primary component is more massive than a star at the main-sequence turnoff .
Therefore , V211 is a blue straggler and should be formed by mass transfer from the secondary component to the primary .
The age of NV358 is less than 1.93 Gyr , indicating that it is much younger than first-generation stars in \omega Centauri .
As NV364 in \omega Centauri , NV358 should be a second-generation binary .