CRP 463: Active Transportation Plan for the City of Paso Robles

As a part of CRP 463 led by Dr. William Riggs, this report provided an analysis of the bicycle, pedestrian and transit travel in the City of Paso Robles and produced a draft Active Transportation Plan for the City

Bicycle Friendly Community Assessment Spring 2015

Completed by Cal Poly, San Luis Obispo City & Regional Planning students enrolled in a bicycle and pedestrian planning course (CRP 425), under the direction of Dr. William Riggs this report was designed to gather data in advance of the City of San Luis Obispo\u27s application to be a Bicycle Friendly Community. The report focuses on the key certification areas of Engineering, Education, Encouragement, Evaluation/Planning and Enforcement providing documentation for the City\u27s eventual application

ATOMIUM: The astounding complexity of the near circumstellar environment of the M-type AGB star R Hydrae: I. Morpho-kinematical interpretation of CO and SiO emission

Evolved low- to intermediate-mass stars are known to shed their gaseous envelope into a large, dusty, molecule-rich circumstellar nebula which typically develops a high degree of structural complexity. Most of the large-scale, spatially correlated structures in the nebula are thought to originate from the interaction of the stellar wind with a companion. As part of the ATOMIUM large programme, we observed the M-type asymptotic giant branch (AGB) star R Hydrae with the Atacama Large Millimeter/submillimeter Array. The morphology of the inner wind of R Hya, which has a known companion at similar to 3500 au, was determined from maps of CO and SiO obtained at high angular resolution. A map of the CO emission reveals a multi-layered structure consisting of a large elliptical feature at an angular scale of similar to 10 '' that is oriented along the north-south axis. The wind morphology within the elliptical feature is dominated by two hollow bubbles. The bubbles are on opposite sides of the AGB star and lie along an axis with a position angle of similar to 115 degrees. Both bubbles are offset from the central star, and their appearance in the SiO channel maps indicates that they might be shock waves travelling through the AGB wind. An estimate of the dynamical age of the bubbles yields an age of the order of 100 yr, which is in agreement with the previously proposed elapsed time since the star last underwent a thermal pulse. When the CO and SiO emission is examined on subarcsecond angular scales, there is evidence for an inclined, differentially rotating equatorial density enhancement, strongly suggesting the presence of a second nearby companion. The position angle of the major axis of this disc is similar to 70 degrees in the plane of the sky. We tentatively estimate that a lower limit on the mass of the nearby companion is similar to 0.65 M-circle dot on the basis of the highest measured speeds in the disc and the location of its inner rim at similar to 6 au from the AGB star