Multicast Mobility in Mobile IP Version 6 (MIPv6) : Problem Statement and Brief Survey

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Istorija kartografirovanija Fobosa

This paper briefly describes the main stages of Phobos mapping, from first topographic schemes to modern digital maps of the Phobos surface created using GIS (Geographic Information Systems) and Internet technologies like Geoportal

A terrain model transect across the Mare Orientale region from Clementine data

We derived a Digital Terrain Model (DTM) using stereo images obtained by the Clementine UVVIS camera along a narrow (60 km x 900 km) strip crosscutting the northern Mare Orientale basin (longitude 88 to 90 deg West; latitude -20 to +10 deg North). Photogrammetric block adjustment and automatic digital image matching were applied to improve the nominal camera pointing data and to determine disparity data (stereo effects) in the images. The resulting DTM has a grid spacing of 250 m and a height resolution of 50 m. Good agreement was found between our topographic data and that from Clementine laser altimeter tracks in the region. The terrain model extends from the Cordillera and outer Rook rings towards the center of Orientale dropping in elevation from +4000 to -3000 m. The Lacus Veris depression and several impact craters, such as Kopff, Kopff D and E are clearly visible. Local slopes in the area appear to be much steeper than was thought previously. The Orientale terrain datawill allow us to study the structure of this prototype multiringed impact basin in unprecedented detail and may be critical also for understanding other large impact basins of the Moon

Grooves of Phobos as seen on the MEX HRSC Rectified Images and Comparisons with Planetary Analogs

Here we analyze the HRSC images of Phobos revisiting a problem of origin of grooves, numerous linear features, often turning to chains of small craters. They were originally assumed to be fractures resulted of the large impacts or from tidal stresses. Also were suggested other hypotheses, the most discussed of which are a suggestion that the grooves were formed by rolling blocks of Phobos crater ejecta or they are chains of coalescing secondary craters formed by ejecta from large craters of Mars

Grooves of Phobos as Seen on Rectified Images Taken by the Mars Express High Resolution Stereo Camera

In this work, we analyze images taken by the HRSC camera onboard Mars Express to revisit the problem of the origin of Phobos’ grooves, numerous linear features, often turning to chains of small craters, which criss-cross its surface