The morphologies of steep-sided domes (pancake domes) on Venus are distinctive, circular in plain view, steep-sided, relatively flat-topped, and large summit diameter/basal diameter ratio, which make them strikingly different from other types of volcanoes in the solar system. It has been proposed that their morphologies could have resulted from the eruption of viscous lava. However, the formation mechanism of steep-sided domes is still on debate. The volcano morphology of volcanoes depends on magma composition, eruption mechanism, gravity and ambient environment (e.g., atmospheric pressure). We have collected and calculated morphologic parameters of different volcanoes, including irregularity index (ii), height/basal diameter ratio (H/WB), summit/basal diameter ratio (WS/WB), max slope height fraction (HSmax), summit height/summit diameter ratio (HS/WS), and eruption volume (V), and have quantitively compared Venusian steep-sided domes with composite volcanoes, shield volcanoes, cinder cones, lava domes (Peleean-type and Coulees-type domes), submarine volcanoes, and mud volcanoes on Earth. The Coulees-type lava domes, submarine flat-topped cones, and mud volcanoes all have some morphologic aspects similar to the steep-sided domes. The profiles of Coulees-type lava domes are the closest to that of steep-sided domes, indicating that the emplacement of steep-sided domes could be similar to that of Coulees-type lava domes. On the other hand, the flank concave shapes of submarine flat-topped volcanoes indicate that the emplacement is different from that of steep-sided domes. Therefore, steep-sided domes might have resulted from the continuous eruption of relatively viscous magma with high effusion rates.