  On Mars it is possible that after the recession of the seasonal polar ice
cap, small icy patches left behind in shady places due to the low thermal
conductivity of the Martian surface and atmosphere, are met by direct sunlight
during the summer. These patches might warm up substantially and we analyzed
below how could a liquid phase emerge in these places, surveying HiRISE images.
730 images that fit the selection criteria of location and season were
analyzed, and we identified 148 images with smaller ice patches on them. Their
separation from other bright patches, like clouds or lighter shades of layers
and rocks were possible by their bluish color and strong connection to local
topographic shading. These areas range between 140{\deg} and 200{\deg} solar
longitude in the latitude band between -40{\deg} and -60{\deg}. The diameter of
the ice patches ranges between 1.5-300 meters, and they remain on the surface
even after the seasonal polar cap has passed over the area for the duration
range of 19-133 martian days.
  With the help of The Mars Climate Database (MCD) we simulated the surface
temperature and predicted CO2 and H2O ice cover at 22 analyzed areas. Judging
by the models, the average noon temperature does not reach the melting point of
water, which is 273 K, therefore the occurrence of liquid water on the
macroscopic scale is highly unlikely, however there is a possibility that an
interfacial premelting of ice (a few nanometers thick waterlayer) might form
between the layered and the water ice.
