In this paper we study the Cepheids distribution in the Large Magellanic Cloud ( LMC ) as a function of their ages using data from the OGLE III photometric catalogue .
To determine age of the Pop I Cepheids , we derived a period - age ( PA ) relationship using the Cepheids found in the LMC star clusters .
We find two peaks in the period distribution at \log P = 0.49 \pm 0.01 and \log P = 0.28 \pm 0.01 days which correspond to fundamental and first overtone pulsation modes , respectively .
Ages of the Cepheids are used to understand star formation scenario in the LMC in last 30 – 600 Myr .
The age distribution of the LMC Cepheids is found to have a peak at log ( Age ) =8.2 \pm 0.1 .
This suggests that major star formation event took place at about 125-200 Myr ago which may have been triggered by a close encounter between the SMC and the LMC .
Cepheids are found to be asymmetrically distributed throughout the LMC and many of them lie in clumpy structures along the bar .
The frequency distribution of Cepheids suggests that most of the clumps are located to the eastern side of the LMC optical center .