Computer Science
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt........17g&link_type=abstract
Thesis (PH.D.)--THE PENNSYLVANIA STATE UNIVERSITY, 1995.Source: Dissertation Abstracts International, Volume: 56-09, Section: B,
Computer Science
Scientific paper
A multiwavelength study of the Orion-Eridanus superbubble has been carried out based on the ROSAT PSPC pointed observation data, IRAS 100 μm data, the 21 cm data obtained with NRAO 140-foot telescope at Green Bank and the inter-stellar Na D data obtained with NOAO Coude Feed telescope. The temperature and the N_{rm H} distribution across the superbubble have been obtained from the X-ray data analysis. It is found that the temperature and N _{rm H} distribution obtained from the best fit are consistent with the morphology difference between the 1over 4 keV and the 3over 4 keV X-ray emission results from the absorption by the intervening gas. Distance limits to the boundary of the Local Bubble and to the near and far sides of the shell associated with the Orion-Eridanus bubble have been estimated based on our 21 cm mapping of the X-ray absorbing clouds and our interstellar Na D absorption line observations toward stars in the 21 cm fields. It is found that the distance to the near side of the Orion -Eridanus bubble is 155 +/- 22 pc in the direction (1,b) ~ (203 ^circ, -40^circ ) and the upper distance limit to the far side of the bubble is 586 pc in the same direction. The observed geometry and kinematics of the Orion-Eridanus feature have been compared with the standard wind-blown bubble theory. It is found that the Orion-Eridanus feature can be explained as a stellar wind superbubble associated with the Orion OB1 association. The evolution and dynamics of the Orion -Eridanus superbubble have also been discussed and it is found that the interstellar pressures from cosmic rays and interstellar magnetic fields play important roles in determining whether the Orion-Eridanus superbubble will blow out the entire galactic H scI disk.
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