See Rodrigues et al. (2017) to know how you can combine your available parameters for a star in a useful way! :)
Warning: for PARSEC models, Δν are computed using scaling relations, while for MESA models, they come from individual radial-mode frequencies computed along the tracks.
Warning: ΔP is only taken into consideration for MESA models.
Mass-loss on RGB using the Reimers formula with ηReimers= .
Solar values: Δν☉= μHz, νmax☉= μHz