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The formation of the massive young stars surrounding SgrA* is still an openquestion. In this paper, we simulate the infall of a turbulent molecular cloudtowards the Galactic Center (GC). We adopt two different cloud masses (4.3x10^4and 1.3x10^5 solar masses). We run five simulations: the gas is assumed to beisothermal in four runs, whereas radiative cooling is included in the fifthrun. In all the simulations, the molecular cloud is tidally disrupted, spiralstowards the GC, and forms a small, dense and eccentric disk around SgrA*. Withhigh resolution simulations, we follow the fragmentation of the gaseous disk.Star candidates form in a ring at ~0.1-0.4 pc from the super-massive black hole(SMBH) and have moderately eccentric orbits (~0.2-0.4), in good agreement withthe observations. The mass function of star candidates is top-heavy only if thelocal gas temperature is high (>~100 K) during the star formation and if theparent cloud is sufficiently massive (>~10^5 solar masses). Thus, this studyindicates that the infall of a massive molecular cloud is a viable scenario forthe formation of massive stars around SgrA*, provided that the gas temperatureis kept sufficiently high (>~100 K).

In situ formation of SgrA* stars via disk fragmentation: parent cloud properties and thermodynamics