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We study the internal radial gradients of stellar population propertieswithin $1.5\;R_{\rm e}$ and analyse the impact of galaxy environment. We use arepresentative sample of 721 galaxies with masses ranging between$10^{9}\;M_{\odot}$ to $10^{11.5}\;M_{\odot}$ from the SDSS-IV survey MaNGA. Wesplit this sample by morphology into early-type and late-type galaxies. Usingthe full spectral fitting code FIREFLY, we derive the light and mass-weightedstellar population properties age and metallicity, and calculate the gradientsof these properties. We use three independent methods to quantify galaxyenvironment, namely the $N^{th}$ nearest neighbour, the tidal strengthparameter $Q$ and distinguish between central and satellite galaxies. In ouranalysis, we find that early-type galaxies generally exhibit shallowlight-weighted age gradients in agreement with the literature and mass-weightedmedian age gradients tend to be slightly positive. Late-type galaxies, instead,have negative light-weighted age gradients. We detect negative metallicitygradients in both early and late-type galaxies that correlate with galaxy mass,with the gradients being steeper and the correlation with mass being strongerin late-types. We find, however, that stellar population gradients, for bothmorphological classifications, have no significant correlation with galaxyenvironment for all three characterisations of environment. Our results suggestthat galaxy mass is the main driver of stellar population gradients in bothearly and late-type galaxies, and any environmental dependence, if present atall, must be very subtle.

SDSS-IV MaNGA: stellar population gradients as a function of galaxy environment