Earth-prints repository, logo   DSpace

About DSpace Software
|earth-prints home page | roma library | bologna library | catania library | milano library | napoli library | palermo library
Please use this identifier to cite or link to this item: http://hdl.handle.net/2122/9656

Authors: Pozzobon, R.*
Mazzarini, F.*
Massironi, M.*
Marinangeli, L.*
Title: Self-similar clustering distribution of structural features on Ascraeus Mons (Mars): implications for magma chamber depth
Other Titles: ASCRAEUS MONS: PIT FRACTAL CLUSTERING
Publisher: Geological Society, London, Special Publications
Issue Date: 2015
URL: http://sp.lyellcollection.org/content/401/1/203
Keywords: Mars, Ascraeus Mons Volcano, plumbing system, fractal distribution
Abstract: The occurrence and distribution of monogenic eruptive features in volcanic areas testify to the presence of deep-crustal or subcrustal magma reservoirs hydraulically connected to the surface via a fracture network. The spatial distribution of vents can be studied in terms of self-similar (fractal) clustering, described by a fractal exponent D and defined over a range of lengths (l) between a lower and upper cutoff, Lco and Uco, respectively. The computed Uco values for several volcanic fields on Earth match the thickness of the crust between vents and magma reservoirs at depth. This analysis can thus be extended to other volcanic fields and volcanoes on rocky planets in the solar system where features such as vents and dykes occur, and for where complementary geophysical data are currently lacking. We applied this method to the Ascraeus Mons volcano on Mars, which presents hundreds of collapse pits similar to those observed on Earth volcanoes that are most likely related to feeder dykes. Based on structural mapping with High Resolution Stereo Camera data at 12 m/px and Context Camera data at 6 m/px mosaics, more than 2300 collapse pits and dyke traces were analysed, revealing two distinct fractal clustered populations. The obtained Uco values reveal the presence and likely depth of both a deep magma reservoir (c. 60 km deep) and a small shallower chamber (c. 11 km deep). This analysis can help to better constrain the depth and time evolution of volcanic processes on Tharsis, and on terrestrial planets’ volcanoes in general.
Appears in Collections:Book chapters
Book chapters
05.09.99. General or miscellaneous

Files in This Item:

File Description SizeFormatVisibility
Geological Society, London, Special Publications-2015-Pozzobon-203-18.pdfMain Article5.98 MBAdobe PDFonly authorized users View/Open


Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.


Share this record
Del.icio.us

Citeulike

Connotea

Facebook

Stumble it!

reddit


 

Valid XHTML 1.0! ICT Support, development & maintenance are provided by CINECA. Powered on DSpace Software. CINECA