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To address how the galaxy Hubble sequence is established and what physicalprocesses are involved, we studied morphological properties and internalstructures of field galaxies in the past (0.4<z<1). In addition to structuralparameters derived from bulge+disk decomposition, Zheng et al. (2004)introduced color maps in recognizing galaxies and properly classifiedmorphologies of 36 luminous infrared galaxies (LIRGs, Lir(8-1000um)>=10^11L_sun). Here we presented morphological classification of a parallel 75non-LIRG sample. Our examination revealed that a significant fraction of thegalaxies shows remarkable morphological evolution, most likely related to thepresent-day spiral galaxies. Comparison of the morphological properties betweenLIRGs and non-LIRGs shows that the LIRGs contain a higher fraction of ongoingmajor mergers and systems with signs of merging/interaction. This suggests thatthe merging process is one of the major mechanisms to trigger star formation.We found that spiral LIRGs probably host much fewer bars than spiral non-LIRGs,suggesting that a bar is not efficient in triggering violent star formation.Differing from Abraham et al. (1999), no dramatic change of the bar frequencyis detected up to redshift ~0.8. The bar frequency of the distant spirals issimilar to (and may be higher than) the present-day spirals in the rest-frame$B$ band. We conclude that bar-driven secular evolution is not a majormechanism to drive morphological evolution of field galaxies, especially theirbulge formation, which is more likely related to multiple intense starformation episodes during which the galaxies appear as LIRGs (Hammer et al.2005).Comment: 19 pages, 6 figures and 2 tables, A&A in pres

HST/WFPC2 morphologies and bar structures of field galaxies at 0.4 $\mathsf{<}$z$\mathsf{<}$ 1