51st Lunar and Planetary Science Conference (2020) 1798.pdf MARE DOMES IN MARE TRANQUILLITATIS: IDENTIFICATION, DISTRIBUTION, CHARACTERISTICS, AND IMPLICATIONS FOR THEIR ORIGIN AND THE OLDEST LUNAR VOLCANISM. L. Qiao1, J. W. Head2, L. Wilson3 and Z. Ling1, 1Inst. Space Sci., Shandong Univ., Weihai, Shan- dong, 264209, China (
[email protected]), 2Dep. Earth, Env. & Planet. Sci., Brown Univ., Providence, RI, 02912, USA, 3Lancaster Env. Centre, Lancaster Univ., Lancaster LA1 4YQ, UK. Introduction: Volcanism is one of the major geo- General Characteristics and Identification Crite- logical process on the Moon, directly reflecting the ria of Mare Domes. A preliminary survey of previous- composition and thermal state of lunar interior and its ly-catalogued mare domes [1-4] reveals some of their evolution, and serves as an important window into the fundamental characteristics. A typical well-developed geological and thermal evolution of the Moon. Mare mare dome is characterized by a domical raised struc- domes, small (<~30 km diameter) and generally circu- ture with a generally convex-shape and low-slope (<5°) lar structures with convex-upward shapes [1], are profile and a (quasi-)circular or elliptical outline. Some among the most common volcanic landforms on the domes have summit pit craters, while many lack them, Moon. Over 300 mare domes have been previously possibly being filled up by the last eruptions. The de- identified, using mainly telescope and orbital photo- velopment of the circular mound shape of mare domes graphs [e.g., 1-4].