Evolution of a transfer-related basin: the Ardea basin (Latium, central Italy)   总被引：1，自引：0，他引：1  

CLAUDIO Faccenna  RENATO Funiciello† ‡  ALESSANDRO Bruni  MASSIMO Mattei†  LEONARDO Sagnotti‡ 《Basin Research》1994,6(1):35-46

During the Messinian—Pleistocene, the Peninsular Tyrrhenian margin underwent a NE—SW orientated stretching regime, with the formation of a NW—SE normal fault system and basins which are linked by NE—SW transfer fault zones. These fault zones border narrow and deep asymmetric basins. This paper uses geological and geophysical analysis (structural and stratigraphical data, seismic lines and anisotropy of magnetic susceptibility (AMS) data) to look at the evolution of one of these transfer-related basins, located south of Rome (Ardea basin). Comparison with other similar features indicates that the common characteristics of these transfer structures are: (i) the slip vector along the transfer fault is mostly dip-slip, which means that the local extensional direction is orthogonal to the regional extensional direction; (ii) development of a narrow and deep half-graben basin.  相似文献   

Supporting evidence from the EPICA Dronning Maud Land ice core for atmospheric CO₂ changes during the past millennium     

URS SIEGENTHALER  ERIC MONNIN  KENJI KAWAMURA  RENATO SPAHNI  JAKOB SCHWANDER  BERNHARD STAUFFER  THOMAS F. STOCKER  JEAN-MARC BARNOLA  HUBERTUS FISCHER 《Tellus. Series B, Chemical and physical meteorology》2005,57(1):51-57

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STUDY OF CORONAL TRANSIENTS IN UV LINE EMISSION     

MARTIN  RENATO  MACCARI  LISA  NOCI  GIANCARLO 《Solar physics》1997,172(1-2):215-223

We investigate the expected emission from coronal transients in the following spectral lines observable with the Ultraviolet Coronagraph Spectrometer (UVCS) on board SOHO: Hi L 1216 Å, Ovi 1032–1037 Å, Nv 1239–1243 Å, Mgx 610–625 Å, Sixii 499–521 Å, and Fexii 1242 Å. We calculate line intensities and profiles for typical CME conditions, and we analyse their relation with the properties of the perturbed coronal region. We find that significant changes in UV line intensities are produced during a coronal transient. An overall decrease of the Hi L intensity is found, which is mainly due to the Doppler dimming produced by the increase in plasma outflow velocity. The emission from heavy ions is instead mainly affected by variations in plasma density and temperature. We expect to compare these results with the future UVCS observations of coronal transients.  相似文献