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High-resolution H$\alpha$ observations indicate that filaments consist of anassembly of thin threads. In quiescent filaments, the threads are generallyshort, whereas in active region filaments, the threads are generally long. Inorder to explain these observational features, we performed one-dimensionalradiative hydrodynamic simulations of filament formation along a dippedmagnetic flux tube in the framework of the chromospheric evaporation-coronalcondensation model. The geometry of a dipped magnetic flux tube ischaracterized by three parameters, i.e., the depth ($D$), the half-width ($w$),and the altitude ($h$) of the magnetic dip. The parameter survey in thenumerical simulations shows that allowing the filament thread to grow in 5days, the maximum length ($L_{th}$) of the filament thread increases linearlywith $w$, and decreases linearly with $D$ and $h$. The dependence is fittedinto a linear function $L_{th}=0.84w-0.88D-2.78h+17.31$ Mm. Such a relation canqualitatively explain why quiescent filaments have shorter threads and activeregion filaments have longer threads.

Dependence of the Length of Solar Filament Threads on the Magnetic Configuration