The first in-situ measurements of the altitude profile of martian upper atmospheric density and composition were carried out by the Viking lander missions in 1976. The MAVEN and MOM spacecraft launched in September 2014 with mass spectrometers and solar radiation measuring payloads have vastly expanded this initial data base. Using a rare set of near-simultaneous data from these two orbiters, we find that there is either an increasing (e.g., for πΆπ2 & π΄π) or a decreasing (e.g., for π) trend of the density profiles by a factor of 2 between June 1 to June 15, 2018 in the height region of βΌ150-300 km. A time series analysis of the concurrent in-situ solar EUV spectral flux and the π»+ ion velocities of the incident solar wind measured near MAVEN periapsis showed the former going through a decrease of only βΌ10% compared to the latterβs decrease by a factor of 4 within the same non-solar-flare period of observation. The estimates of standard errors and the use of the linear regression analysis for the correlation coefficients between densities and solar radiation components have been carried out. Invoking simple photochemical equilibrium conditions with the dissociation of πΆπ2 (producing πΆπ and π) through solar EUV radiation and the solar wind π»+ ion impact process, the day-to-day variations of these constituents are estimated. The high and significant anticorrelation between the density variations of πΆπ2 and π due to the dissociation of πΆπ2 by the solar wind particle radiation is clearly demonstrated. The cause for the increasing densities of π΄π like that of πΆπ2 during this period is more complex and would likely be governed by the temperature variations due to absoption of solar EUV/charged particle radiation and other interacting dynamical effects. Gathering of more such events from future data and development of a more advanced photochemical model of the phenomenon being pursued by us would help to confirm these preliminary results.