  There may be a chance of small-scale ephemeral liquid water formation on
present day Mars, even though the current climate does not support the
existence of larger bodies of water. Through a process called deliquescence,
hygroscopic salts can enter solution by absorbing water vapor directly from the
atmosphere. Due to the absence of in-situ deliquescence experiments so far, the
most reliable way to forecast deliquescence is through atmospherical modeling,
however, the locations and times when salty liquid water could emerge are not
yet well known. In this paper we present our results of likely brine formation
on Mars, their proposed locations and seasons, as well as the possible limiting
factors. For our calculations we used the data of Laboratoire de
M\'et\'eorologie Dynamique Mars General Circulation Model version 5. The
results show that from L$_s$ 35$^\circ$ - L$_s$ 160$^\circ$, between 9 PM and
11 PM there is a good chance for calcium perchlorate deliquescence above
30$^\circ$ N, while in this zone the ideal regions are concentrated mostly to
Acidalia Planitia and Utopia Planitia between 1 AM and 3 AM. We found that in
the Southern Hemisphere, between L$_s$ 195$^\circ$ and L$_s$ 320$^\circ$, there
is a noticeable, but weaker band in the vicinity of 60$^\circ$ S, and both
Argyre Planitia and Hellas Planitia show some chance for brine formation.
According to our statistics the key limiting factor of deliquescence could be
relative humidity in most cases. Our results suggest that during summer --
early fall seasons, there could be deliquescence in both hemispheres in
specific areas from the late evening until the early morning hours. There are
only few studies detailing the geological and temporal distribution of brine
formation through deliquescence, thus this work could be used as a good guide
for future landing site analysis or in choosing a specific location for further
research.
