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tokens: ( MK; Maggio et al. 2000 ). The abundances during the flares F1 and F2 are found to enhance ∼9 and ∼2 times more than those of the minimum values observed. During other superflares, abundances were found to increase between two to three times more than that of the quiescent level (Favata Schmitt 1999 ; Favata et al. 2000 ; Maggio et al. 2000 ). However, in the case of the superflare observed with Swift in EV Lac, the abundances were found to remain constant throughout the flare. From Figure 3 , it is evident that the abundance peaks after the temperature and luminosity peaks, which is consistent with a current idea in the literature (see Reale 2007 ). This could be due to the heating and evaporation of the chromospheric gas, which increases the metal abundances in the flaring loop. For both flares, the temperature peaked before the EM did. A similar delay was also observed in many other solar and stellar flares (e.g., Sylwester et al. 1993 ; Favata Schmitt 1999 ; Favata et al. 2000 ; Pandey Singh 2008 ). The temperature increases due to beam driven plasma heating and later subsequent evaporation of the plasma into upper parts of the coronal loop that increases its density, and therefore EM (). Later coronal plasma cools down by thermal conduction and then via radiative losses (e.g., Cargill Klimchuk 2004 ). 4.2. Coronal Loop Properties The derived loop lengths for the flares F1 and F2 are larger than previously observed flares by Crespo-Chacón et al. ( 2007 ) on CC Eri. The loop lengths are also in between the loop lengths derived for other G–K dwarfs, dMe stars, and RS CVn type binaries (e.g., Favata Micela 2003 ; Pandey Singh 2008 , 2012 ). Instead of ∼3 times larger peak luminosity in flare F1 than that of the flare F2, the derived loop length for flare F2 is two times larger than that of flare F1, which might be interpreted as a result of an ∼1.4 times more sustained heating rate in the decay phase of flare F1 than that of flare F2. The heating rate during flare F1 is also found to be ∼49% of the bolometric luminosity of the CC Eri system, whereas during flare F2 the heating rate is only ∼35% of the combined bolometric luminosity. The derived heating rate is also found to be more than the maximum X-ray luminosity for both flares. This result is compatible with X-ray radiation being one of the major energy loss terms during the flares. Present analysis allows us to make some relevant estimation of the magnetic field strength that would be required to accumulate the emitted energy and to keep the plasma confined in a stable magnetic loop configuration. Under the assumptions that the energy release is indeed of magnetic origin, the total non-potential magnetic field involved in a flare energy release within an active region of the star can be obtained from the relationAssuming that the loop geometry does not change during the flare, is estimated to be >12 and >2 kG for the flares F1 and F2, respectively. Bopp Evans ( 1973 ) also estimated a