Study of the Influence of an Evolving Galactic Potential on the Orbital
  Properties of 152 Globular clusters with Data from the Gaia EDR3 Catalogue
  We have studied the influence of an evolving gravitational potential of the
Milky Way Galaxy on the orbital motion of 152 globular clusters with proper
motions from the Gaia EDR3 catalogue and mean distances from Baumgardt and
Vasiliev (2021). To construct a semicosmological evolving model potential with
changing masses and sizes of the Galactic components, we have used the
algorithm described in Haghi et al. (2015). The adopted axisymmetric
three-component model potential of the Galaxy includes a spherical bulge, a
flat Miyamoto--Nagai disk, and a spherical Navarro--Frenk--White dark matter
halo.The orbits are integrated backward in time. We compare the orbital
parameters of globular clusters derived in static and evolving potentials when
integrating the orbits for 5 and 12 Gyr backward. For the first time we have
studied the influence of separately a change in the masses and a change in the
sizes of the Galactic components. The changes in the masses and sizes of the
components are shown to act on the orbital parameters in the opposite way. At
small Galactocentric distances this influence is maximally compensated for. The
orbits of distant globular clusters and those with a large apocenter distance
undergo the biggest changes. We show that on time scales up to $-5$~Gyr the
orbits of globular clusters in the case of a potential with both changing
masses and changing sizes of the components undergo, on average, minor changes
compared to the case of a static potential. These changes fit into the limits
of the statistical uncertainties caused by the errors in the data. So, on these
time scales the Galactic potential may be deemed static. We provide tables with
the orbital parameters of globular clusters derived in both static and evolving
potentials.
