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Geotechnically, another implication is that the wide presence of fine and cohesive ash, not only on top of the coarse fallout sequences but also on the ground, prevented water infiltration, favoring surficial runoff and creating sliding surfaces (Baumann et al., 2020). The results show that for both eruptions the distribution of the primary deposits is wider than previously known. A consequence of these results is that a wider areal impact should be expected in terms of civil protection, as the sub-Plinian scenario is the reference one for a future large eruption of Vesuvius. Such a distribution of the pyroclastic deposits directly affects the one of the lahar deposits, also because a significant remobilization took place during and after the studied eruptions, which involved distal phreatomagmatic ash.
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A massive deposit follows upward; it is progressively humified and contains abundant reworked and rounded pumice clasts from the Avellino eruption. The top humified surface is almost always eroded by anthropogenic activity and is generally plowed (p1 in Fig. C2). It is few centimeters thick and is composed of a basal layer of dark coarse ash (small pumice fragments), overlain by a massive ash bed, containing abundant accretionary lapilli.
In particular, hf refers to lahar deposits relatively close to the obstacles but which were not affected by them during emplacement, i.e., close but not so much. We assessed that correlation taking into account the stratigraphic and sedimentological characteristics of the lahar deposits and the fact that Eq. (7) performs better with layers emplaced after remobilization of primary pyroclastic fallout or dominantly ash flow deposits. The lithological and sedimentological analyses carried out in the field allowed the macroscopic definition of the primary pyroclastic deposits affected by the remobilization and of the lahar deposits. In many cases, the archeological findings permitted us to define the local paleoenvironment and related land use, then permitted us to constrain the age and timing of the deposition. The absence of information in the Lauro and Avella–Baiano valleys is likely due to the absence of detailed descriptions of alluvial events or more likely to the position of the inhabited areas generally located on the hills and thus far from the lower part of the valleys.
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Figure C8Avella–Baiano Valley; the Pollena primary deposit (a,b) lies on plowed soil (p) and is covered by at least three flow units of lahars (c). Finally, routine magnetic measurements were done on the lahar matrix to determine the characteristic remanent magnetization (ChRM) by thermal and alternating field demagnetizations. The direction of the Earth’s magnetic field during the Pollena eruption is well-known (Zanella et al., 2008). If the sampled lahars were emplaced shortly after the eruption, both the secondary TRMs and the matrix of the lahars should show a remanent magnetization direction similar to the Pollena ones. ChRMs can also test if the two lahars (Acerra at 12 km from Somma–Vesuvius and Nola at 10–15 km from Apennine source valleys) are coeval.
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The Nola and Cimitile areas are covered by thick sequences of fallout and lahar deposits. This effect is clearly visible in the Amphitheater Laterizio, which was completely filled by the primary and secondary deposits. The same is true in Cimitile, where at the archeological site of the early Christian basilicas the present ground level is about 2 m higher than the one before the eruption.
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The studied sequences start from the paleosol developed on top of the ash deposits of the 79 CE eruption. The paleosol is mature and contains pottery fragments until the second century CE. Representative sequences of the area include a basal ash layer with a thickness ranging from 1 to 4 cm (b in Fig. C7), thickening in the depressions, that is cohesive and locally vesiculated. It is interpreted here as co-ignimbritic ash emplaced by fallout during the phreatomagmatic final immediatemax-air.com phases of the Pollena eruption. Upwardly, the sequence includes several lahar units from massive to slightly stratified, composed of fine and very cohesive ash, and containing scattered greenish pumice fragments (lithofacies mM) (b1 in Fig. C7). Locally, this deposit, also in the case of multiple units, is cut by vertical drying cracks.
Besides, the modulus of the susceptibility axes provides some magnetic parameters useful to express the intensity of the anisotropy (Pj) and the oblate–prolate fabric occurrence (T). Generally, sedimentary vs. pyroclastic deposit fabric, here considered to be a proxy for the lahar fabric, is oblate with a horizontal to gently imbricated (less than 20°) magnetic foliation. In this case, both the F imbrication and the L direction can provide the local flow direction. Other times, L is orthogonal to the F plunge or F is statistically horizontal, and it is not possible to infer the flow direction. The distribution of the syn- and post-eruptive 1631 lahar deposits mainly reflects the major dispersal axis affecting the fallout deposit distribution, while the pyroclastic current deposits were minorly remobilized as exposed on the gentler slopes of southwestern Vesuvius (Fig. 6).