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tokens: the quick knowledge of effectiveness and the computational methods (like extrapolations and flux-rope fitting) for further determining the magnitude of the CME impact. Bothmer Schwenn ( 1998 ) compared the helicity of a set of quiescent filaments using the hemispheric helicity preference (Rust Kumar 1994 ) with their ICME counterparts. They found a significant agreement in quiescent filaments to the rule (89%; a total of 9 filaments). Savani et al. ( 2015 ) also used the hemispheric helicity rule for obtaining the axis orientation for eight events but they warn that extra care must be taken while determining axis orientation of filaments that are between multiple active regions. Several statistical surveys on the hemispheric preference of helicity show varying degrees of compliance (for example, see HaiQing et al. 2009 ). In some of these studies (e.g., Martin et al. 1994 ), quiet regions show a higher degree of preference compared to the active regions. However, none of the studies show a 100% compliance with the hemispheric helicity rule indicating that independently obtaining the field direction at each source region is important. In order to avoid errors arising from exceptions in the hemispheric helicity rule and/or issues in disambiguation techniques, we have relied solely on filament observations and LOS magnetograms for obtaining the required parameters. We believe our method has performed well and has given reliable results. The human eye performs well in obtaining the chirality with images of reasonable resolution, but it is impractical to have human eyes analyze each and every filament. The advent of computer vision in solar physics is promising: automating filament chirality determination using machine-learning techniques (Martens et al. 2012 ; Aggarwal et al. 2018 ) will help in preparing computationally efficient and effective measures against severe space weather effects. Knowing whether there will be a geomagnetic effect or not is of primary importance to start taking precautionary measures. However, precautionary measures during a false alarm and the resulting expenditures can be avoided with the method used in this paper. Furthermore, our method of determining the axial field direction is more quick and straightforward than computationally expensive methods such as force free extrapolations and determining helicity (Bothmer Schwenn 1998 ; Yurchyshyn et al. 2001 etc.). In the current study we consider only the north–south component of the axial magnetic field of the filament. This is deemed useful as a first step in omitting ICMEs that will not be geoeffective. However, it is necessary to know the exact, quantitative direction and strength to determine where an ICME might reconnect with the magnetosphere and its severity. Utilizing vector magnetograms to determine the exact orientation and further study the field in the corresponding flux ropes at L1 will be useful in determining their orientations. Active region filaments