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We propose that cold filamentary accretion in massive galaxies at highredshift can lead to the formation of star-forming clumps in the halos of thesegalaxies without the presence of dark matter sub-structure. In certain cases,these clumps can be the birth places of metal poor globular-clusters (MP GCs).Using cosmological simulations, we show that narrow streams of dense gasfeeding massive galaxies from the cosmic web can fragment, producingstar-forming clumps. We then derive an analytical model for the properties ofstreams as a function of halo mass and redshift, and assess when these aregravitationally unstable, when this can lead to collapse and star-formation inthe halo, and when it may result in the formation of MP GCs. For streammetalicities >~1% solar, this is likely to occur at z>4.5. At z~6, thecollapsing clouds have masses of (5-10)x10^7 M_{sun} and the average streampressure is ~10^6 K cm^{-3}. The conditions for GC formation are met in theextremely turbulent "eyewall" at ~0.3 R_{vir}, where counter-rotating streamscan collide, driving very large densities. Our scenario can account for theobserved kinematics and spatial distribution of MP GCs, the correlation betweentheir mass and metalicity, and the mass ratio between the GC system and thehost halo. For MW mass halos, we infer that ~30% of MP GCs could have formed inthis way, the remainder likely accreted in mergers. Our predictions for GCformation along circumgalactic filaments at high-redshift are testable withJWST.

Cold Filamentary Accretion and the Formation of Metal Poor Globular Clusters and Halo Stars