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We observe a solar surge in NOAA AR11271 using SDO AIA 304 image data on 25August, 2011. The surge rises vertically from its origin upto a height of 65 Mmwith a terminal velocity of 100 km/s, and thereafter falls and fades gradually.The total life time of the surge was 20 min. We also measure the temperatureand density distribution of the observed surge during its maximum rise, andfound an average temperature and density of 2.0 MK and 4.1 x 109 cm-3,respectively. The temperature map shows the expansion and mixing of cool plasmalagging behind the hot coronal plasma along the surge. As SDO/HMI temporalimage data does not show any detectable evidence of the significantphotospheric magnetic field cancellation for the formation of the observedsurge, we infer that it is probably driven by magnetic reconnection generatedthermal energy in the lower chromosphere. The radiance (thus mass density)oscillations near the base of the surge are also evident, which may be the mostlikely signature of its formation by a reconnection generated pulse. In supportof the present observational base-line of the triggering of the surge due tochromospheric heating, we devise a numerical model with conceivableimplementation of VAL-C atmosphere and a thermal pulse as an initial trigger.We find that the pulse steepens into a slow shock at higher altitudes thattriggers plasma perturbations exhibiting the observed features of the surge,e.g., terminal velocity, height, width, life-time, and heated fine structuresnear its base.

Study of the Kinematics and Plasma Properties of A Solar Surge Triggered due to Chromospheric Activity in AR11271