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Components in the interstellar medium toward epsilon persei and delta persei

Journal Article · · Astrophys. J.; (United States)
DOI:https://doi.org/10.1086/159971· OSTI ID:6865045
We analyze the lines of sight toward epsilon Persei and delta Persei with a procedure that gives velocity components for various interstellar ions. The column densities found for ions expected to be relatively undepleted are used to estimate the column density of neutral hydrogen in each component. The velocities found correspond well with those determined from previous optical studies when the optical components can be resolved. Whenever possible we calculate electron density, calcium and titanium depletion, molecular hydrogen excitation temperature, and hydrogen volume density for each component. Toward each star there is one dominent component with high column density, low LSR velocity, a large depletion in Ca and Ti, and low H/sub 2/ excitation temperature. The H/sub 2/ results also indicate that the dominant component has a high hydrogen volume density. The components at higher velocities are characterized by lower column densities and less Ca and Ti depletion, relative to the dominant component. There is also evidence that there is one component toward each star which contains mostly ionized gas. While the electron densities found seem consistent with previous results, questions are raised concerning the formation rate of H/sub 2/ and the abundance variations of certain species from cloud to cloud.
Research Organization:
Princeton University Observatory
OSTI ID:
6865045
Journal Information:
Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 257:1; ISSN ASJOA
Country of Publication:
United States
Language:
English

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