Other
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p31e1732k&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P31E-1732
Other
[5480] Planetary Sciences: Solid Surface Planets / Volcanism, [6250] Planetary Sciences: Solar System Objects / Moon
Scientific paper
The relationship between mare volcanism and impact basins has long been recognized, although the degree of influence basin formation has on volcanism remains a point of contention. For example, did melting of magma sources result from thermal energy imparted by a basin-forming event? Did basin impacts initiate mantle overturn of the unstable LMO cumulate pile, causing dense ilmenite to sink and drag radioactive KREEPy material to provide the thermal energy to initiate melting of the mare sources? Did the dramatically altered stress states provide pathways ideally suited for magma ascent? The chemistry of sampled lunar volcanic glasses indicates that they experienced very little fractional crystallization during their ascent to the surface - they have pristine melt compositions. Volatile abundances, including recent measurements of OH [1,2] suggest that the mantle source of at least the OH-analyzed glasses have a water abundance of ~700 ppm - comparable to that of Earth's upper mantle. More recently, [3] showed that the abundance of OH and other volatiles measured in these glasses is positively correlated with trace element abundances, which is expected since water is incompatible in a magma. Volatile enrichment in a deep mantle source would lower the melting temperature and provide the thrust for magma ascent through 500 km of mantle and crust [4]. We are exploring the idea that such basin-related lunar pyroclastic volcanism may represent the last phase of basaltic volcanism in a given region. Remote sensing studies have shown volcanic glasses are fairly common, and often found along the perimeter of mare-filled basins [5]. Recent modeling of the stresses related to the basin-forming process [6,7] show that basin margins provide the ideal conduit for low-volume lunar pyroclastic volcanism (compared with the high output of mare volcanism). Schrödinger's basin floor is largely composed of a compositionally uniform impact breccia. The exceptions are two distinct and spatially isolated volcanic units, both confined within the central peak ring. One is a thin mare deposit to the north, and to the south is a 8.5 km long pyroclastic vent. The basin also a series of fractures, which exhibit complex cross-cutting relationships with each other and the basin floor materials, thereby offering clues about the timing of their formation. Some of these fractures widen as they cut across the uplifted peak ring, indicating that they are the surface manifestations of deep faulting and are younger. An orthogonal system of fractures in the southern basin floor outside of the peak ring is of particular interest because of its possible relationship to Schrodinger's basin volcanism. We are exploring the hypothesis that an expanding magma chamber once resided in this location, uplifted the basin floor, and formed these orthogonal fractures. Post-inflation, the reservoir was emptied via a propagating dike and sill complex that eventually surfaced at the location of the pyroclastic vent. [1] Saal et al. (2008) Nature; [2] Hauri et al. (2011) Science; [3] Saal et al. (2011) NASA Lunar Sci. Inst. Forum; [4] Delano (1986) JGR; [5] Head (1976) Rev. Geophys. Space Phys.; [6] McGovern & Litherland (2011) LPSC 42;McGovern et al. (2011) AGU Fall Session
Kramer Georgiana Y.
Kring David A.
McGovern Patrick J.
Nahm Amanda
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