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Ellerman bombs (EBs) and UV bursts are both small-scale solar activities thatoccur in active regions. They are now believed to form at different heights inthe lower atmosphere. In this paper, we use one-dimensional radiativehydrodynamic simulations to calculate various line profiles in response toheating in different atmospheric layers. We confirm that heating in the upperphotosphere to the lower chromosphere can generate spectral features of typicalEBs, while heating in the mid to upper chromosphere can generate spectralfeatures of typical UV bursts. The intensity evolution of the H$\alpha$ linewing in EBs shows a rise--plateau pattern, while that of the Si IV 1403 \r{A}line center in UV bursts shows a rise--fall pattern. However, the predictedenhancement of FUV continuum near 1400 \r{A} for EBs is rarely reported andrequires further observations to check it. With two heating sources or anextended heating source in the atmosphere, both EB and UV burst features couldbe reproduced simultaneously.

Revisiting the Spectral Features of Ellerman Bombs and UV Bursts. I. Radiative Hydrodynamic Simulations