  We combine an unprecedented MaNGA sample of over 3,000 passive galaxies in
the stellar mass range 10^{9}-10^{12} Msun with the Sloan Digital Sky Survey
group catalog by Tinker to quantify how central and satellite formation,
quantified by radial profiles in stellar age, [Fe/H], and [Mg/Fe], depends on
the stellar mass of the galaxy (M*) and the mass of the host halo (Mh). After
controlling for M* and Mh, the stacked spectra of centrals and satellites
beyond the effective radius (r_e) show small, yet significant differences in
multiple spectral features at the 1% level. According to spectral fitting with
the code alf, a primary driver of these differences appears to be [Mg/Fe]
variations, suggesting that stellar populations in the outskirts of satellites
formed more rapidly than the outer populations of centrals. To probe the
physical mechanisms that may be responsible for this signal, we examined how
satellite stellar populations depend on Mh. We find that satellites in high-Mh
halos show older stellar ages, lower [Fe/H], and higher [Mg/Fe] compared to
satellites in low-Mh halos, especially for M*=10^{9.5}-10^{10.5} Msun. These
signals lend support to environmentally driven processes that quench satellite
galaxies, although variations in the merger histories of central and satellite
galaxies also emerge as a viable explanation.
