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Deep and wide-field optical photometric observations along withmultiwavelength archival datasets have been employed to study the physicalproperties of the cluster NGC 6910. The study also examines the impact ofmassive stars to their environment. The age, distance and reddening of thecluster are estimated to be $\sim$4.5 Myr, $1.72\pm0.08$ kpc, and $E(B-V)_{min}= 0.95$ mag, respectively. The mass function slope ($\Gamma =-0.74\pm0.15$ in the cluster region is found to be flatter than the Salpetervalue (-1.35), indicating the presence of excess number of massive stars. Thecluster also shows mass segregation towards the central region due to theirformation processes. The distribution of warm dust emission is investigatedtowards the central region of the cluster, showing the signature of the impactof massive stars within the cluster region. Radio continuum clumps powered bymassive B-type stars (age range $\sim$ 0.07-0.12 Myr) are traced, which arelocated away from the center of the stellar cluster NGC 6910 (age $\sim$ 4.5Myr). Based on the values of different pressure components exerted by massivestars, the photoionized gas associated with the cluster is found to be thedominant feedback mechanism in the cluster. Overall, the massive stars in thecluster might have triggered the birth of young massive B-type stars in thecluster. This argument is supported with evidence of the observed age gradientbetween the cluster and the powering sources of the radio clumps.

Unveiling the physical conditions in NGC 6910