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Whether BDs form as stars through gravitational collapse ("star-like") or BDsand some very low-mass stars constitute a separate population which formalongside stars comparable to the population of planets, e.g. throughcircumstellar disk ("peripheral") fragmentation, is one of the key questions ofthe star-formation problem. For young stars in Taurus-Auriga the binaryfraction is large with little dependence on primary mass above ~0.2Msun, whilefor BDs it is <10%. We investigate a case in which BDs in Taurus formeddominantly through peripheral fragmentation. The decline of the binaryfrequency in the transition region between star-like and peripheral formationis modelled. A dynamical population synthesis model is employed in whichstellar binary formation is universal. Peripheral objects form separately incircumstellar disks with a distinctive initial mass function (IMF), own orbitalparameter distributions for binaries and a low binary fraction. A small amountof dynamical processing of the stellar component is accounted for asappropriate for the low-density Taurus-Auriga embedded clusters. The binaryfraction declines strongly between the mass-limits for star-like and peripheralformation. The location of characteristic features and the steepness depend onthese mass-limits. Such a trend might be unique to low density regions hostingdynamically unprocessed binary populations. The existence of a strong declinein the binary fraction -- primary mass diagram will become verifiable in futuresurveys on BD and VLMS binarity in the Taurus-Auriga star forming region. It isa test of the (non-)continuity of star formation along the mass-scale, theseparateness of the stellar and BD populations and the dominant formationchannel for BDs and BD binaries in regions of low stellar density hostingdynamically unprocessed populations.

Using binary statistics in Taurus-Auriga to distinguish between brown dwarf formation processes