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tokens: has been observed. Detection of radio flare during the HIMS of GX 339−4 (2002 outburst) and the first and second flares in V404 Cyg, indicate similar characteristics. Since the source MAXI J1836−194 is not observed to have transited to a SIMS or HSS (Ferrigno et al. 2012 ; Russell, Soria Miller-Jones 2014 ), the system of jet ejection for such sources which have ‘failed outbursts’ seems to be different as compared to other BH sources. Although Russell et al. ( 2013 ) suggests the presence of a compact jet, the fact that QPOs are not observed suggests of a probable transient jet ejection event. A deeper look into the properties of the companions of these BHs suggests them to be of late F, G, K or M type (Sanchez-Fernandez et al. 1999 ; Hynes et al. 2003 ) which are in general magnetically active (Linsky 1985 ), with field strength around 1 kilogauss. This suggests that the models which specify the role of magnetic fields in formation of jets by evacuation of the Comptonized corona (see Section 4 and Nandi et al. 2001 ) are applicable for these sources, wherein the magnetic field from the companion flows along-with the matter into the accretion disc. This field probably gets amplified during the rising phase of the outburst (i.e. the LHS and HIMS) and finally collapses to push out the matter from the corona (Nandi et al. 2001 ; Fender et al. 2004 , 2009 ) forming jets/flares, as the source enters the SIMS. The time-scale required for amplification of the field is equivalent to the rising time of the source upto the end of the HIMS when the jet ejection occurs. A typical BH source with a fast rise and exponential decay light curve requires around 10 d to reach the transition point from HIMS to SIMS. For the sources studied in this paper which have a typical fast rise-time (XTE J1859+226, H 1743−322, XTE J1748−288, GRO J1655−40, XTE J1550−564), the time-scale required for the field amplification is found to vary from 5 to 15 d. In these sources, we find that the peak radio flux is higher and varies between 100 and 600 mJy, except the 2009 outburst of H 1743−322 and 2005 outburst of GRO J1655−40 which have very less radio flux during the moment of ejection (5.7 and 1.6 mJy, respectively) and also while in the peak. For the sources which have a slow rise towards the X-ray peak require more time to reach the transition point i.e. they take larger time-scale to amplify the magnetic field. As an example XTE J1752−223 requires 88 d, 48 d is taken by GX 339−4 during its 2002 outburst and 104 d for GX 339−4 during its 2010 outburst. For these sources, the peak radio flux is found to vary from 18 to 55 mJy. Fender et al. ( 2004 ) has performed detailed study on the estimation of the jet power based on the characteristics of the radio flare, like its rise time and flux density (see also Fender Munoz-Darias 2016 ). It is also possible to have a quantitative estimation of the kinetic jet power based on the X-ray characteristics of the source. Recently Aktar,