Ejecta emplacement of the Martian impact crater Bamburg

The paper examines the ejecta emplacement of the Martian impact crater Bamburg. During ejecta emplacement, secondary crater formation preceeded the deposition of mobile surface flows, which are overrun by more viscous flows characterized by longitudinal grooves and transverse ridges. Many areas of flat terrain on the ejecta deposits may indicate that the sediment-laden melt water percolated out of the volatile-rich ejecta and the crater rim. The number of secondary craters associated with Bamburg is less than one third the value for lunar and Mercurian craters of equivalent size; this is attributed to preferential destruction of ejecta blocks sufficiently large to form secondary craters or to the subsequent burial of such craters.