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To investigate the physical processes, we present observational results ofthe sites S234, V582, and IRAS 05231+3512 situated toward l = 171.7 - 174.1degrees. Based on the CO line data, we find that these sites are not physicallyconnected, and contain at least one filament (with length > 7 pc). The observedline masses (M_line,obs) of the filaments associated with V582 and IRAS05231+3512 are ~37 and ~28 M_sun/pc, respectively. These filaments arecharacterized as thermally supercritical, and harbor several clumps. Groups ofinfrared-excess sources and massive B-type stars are observed toward thefilament containing V582, while a very little star formation (SF) activity isfound around IRAS 05231+3512. Our results favour radial collapse scenario inthe filaments harboring V582 and IRAS 05231+3512. In the site S234, twofilaments (i.e. ns1 (M_line,obs ~130 M_sun/pc) and ns2 (M_line,obs ~45M_sun/pc)) are identified as thermally supercritical. An extended temperaturestructure at 27-30 K surrounds a relatively cold (~19 K) ~8.9 pc long filamentns1. At least four condensations (M_clump ~70-300 M_sun) are seen in ns1, andare devoid of the GMRT 610 MHz radio emission. The filament ns2 hosting clumpsis devoid of ongoing SF, and could be at an early stage of fragmentation. Anintense SF activity, having the SF efficiency ~3.3% and SF rate ~40-20M_sun/Myr (for t_sf ~1-2 Myr), is observed in ns1. The feedback of massivestars in S234 seems to explain the observed SF in the filament ns1.

Filamentary Structures and Star Formation Activities in the Sites S234, V582, and IRAS 05231+3512