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Abridged  Context: Snowlines during star and disk formation are responsible for a rangeof effects during the evolution of protostars, such as setting the chemicalcomposition of the envelope and disk. This in turn influences the formation ofplanets by changing the elemental compositions of solids and affecting thecollisional properties and outcomes of dust grains. Snowlines can also revealaccretion bursts, providing insight into the formation process of stars.  Methods: A numerical chemical network coupled with a grid ofcylindrical-symmetric physical models was used to identify what physicalparameters alter the CO and H$_2$O snowline locations. The investigatedparameters are the initial molecular abundances, binding energies of CO andH$_2$O, heating source, cloud core density, outflow cavity opening angle, anddisk geometry. Simulated molecular line emission maps were used to quantify thechange in the snowline location with each parameter.  Conclusions: The models presented in this work show that the CO and H$_2$Osnowline locations do not occur at a single, well-defined temperature as iscommonly assumed. Instead, the snowline position depends on luminosity, cloudcore density, and whether a disk is present or not. Inclination and spatialresolution affect the observability and successful measurement of snowlinelocations. We note that N$_2$H$^+$ and HCO$^+$ emission serve as goodobservational tracers of CO and H$_2$O snowline locations. However, constraintson whether or not a disk is present, the observation of additional moleculartracers, and estimating envelope density will help in accurately determiningthe cause of the observed snowline position. Plots of the N$_2$H$^+$ andHCO$^+$ peak emission radius versus luminosity are provided to compare themodels with observations of deeply embedded protostars aiming to measure the COand H$_2$O snowline locations.

Modeling snowline locations in protostars: The impact of the structure of protostellar cloud cores