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Hobbs, L. M.

Publications and source records attributed to Hobbs, L. M..

65 records · Page 4
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NASA NTRS1973

The doublet-ratio method and interstellar abundances.

The method of doublet ratios, used in obtaining interstellar Na I and Ca II abundances, is generalized to include realistic multiple-cloud cases. Entirely apart from any errors of observation, the simplified velocity distribution used in the method leads to errors in the inferred column densities which are systematic and which can be as large as a factor of ten or more in some practical cases. The D lines of Na I toward zeta Oph illustrate such order-of-magnitude underestimates.

Nachman, P.↗
NASA NTRS1973

On the interstellar CO/+//CO abundance ratio.

A search at high sensitivity for interstellar absorption in the 4250-A line of CO(+) yields negative results toward 14 stars, despite the pervasive presence of large amounts of CO in the interstellar gas. This result is in accord with theory, but still lacks by a large factor sufficient sensitivity to test any details of the theory.

Hobbs, L. M.↗
NASA NTRS1973

Interferometric studies of interstellar CH/+/ molecules.

The work reported consists of interferometric, photoelectric scans in the region of the line at 4232 A in the spectra of 28 stars. An instrumental passband of about 0.014 A was selected for the observations. In comparison with the capabilities of the older methods utilized in particular by Adams, the present method yields a fivefold improvement in spectral resolution, as well as the higher accuracy inherent in photoelectric detection. As a result, the detailed line profiles of individual line components can be recorded rather than only the composite equivalent widths.

Hobbs, L. M.↗
NASA NTRS1973

Interstellar Na I, K I, Ca II, and CH/+/ line profiles toward zeta Ophiuchi.

Comparison of interferometric, photoelectric scans of interstellar absorption-line profiles of Na I, K I, Ca II, and CH(+) toward zeta Ophiuchi. Near a heliocentric velocity of -15 km/sec, there is a strong composite feature showing four components. The atomic and molecular absorption lines do not arise in a common volume of gas but rather in essentially different clouds whose atomic abundances and/or ionization balances vary substantially.

Hobbs, L. M.↗
NASA NTRS1973

Stellar and interstellar K lines - Gamma Pegasi and iota Herculis.

High-resolution scans show that the relatively strong (about 90 mA) K lines of Ca II in the early B stars gamma-Peg and iota-Her are almost entirely stellar in origin, although the latter case includes a small interstellar contribution. Such stellar lines can be of great importance in augmenting the interstellar absorption, up through the earliest of the B stars.

Hobbs, L. M.↗
NASA NTRS1972

On circumstellar molecules in the Pleiades.

Consideration of both old and new observations of the interstellar 4232-A line of CH(+) for the brightest members of the Pleiades. These observations suggest that the molecules are circumstellar in some sense, perhaps resembling in this respect the micron-sized grains inferred to be present in this region.

Hobbs, L. M.↗
NASA NTRS1972

Interstellar C-12/C-13 ratios toward six stars.

N(C-12)/N(C-13) ratios were measured for interstellar CH(+) molecules toward six stars, using the 4232 A line. The measurements were performed with a spectrometer at the coude focus of a 107-inch telescope with an instrument passband of roughly 0.014 A. The lower bounds of these ratios are 77 for 20 Tau, 20 for 23 Tau, 58 for Xi Per, 52 for Zeta Oph, 20 for P Cyg, and 26 for 55 Cyg.

Hobbs, L. M.↗
NASA NTRS1972

Interferometric studies of interstellar calcium lines.

Review of interferometric, photoelectric scans of the interstellar calcium K-lines in the spectra of 65 stars. The scans were obtained with a PEPSIOS spectrometer having a passband with a full half-intensity width of 1.0 km/sec or 0.013 A. The fivefold improvement in resolution over that used by Adams reveals numerous line components which correspond very well to those of the interstellar sodium lines, apart from frequent differences in relative intensities.

Marschall, L. A.↗
NASA NTRS1972

Interstellar sodium lines and the two-component model of galactic H I regions.

The intensities and widths of the interstellar sodium lines are considered as possible discriminants between two different two-component models recently proposed for galactic H I regions. Depending on the model, the observed sodium lines are either formed entirely in the clouds or, alternatively, in both the clouds and the intercloud medium. Present observational evidence is insufficient to distinguish between these two possibilities.

Hobbs, L. M.↗
NASA NTRS1971

Observations of interstellar Ca I lines.

Evaluation of interferometric, photoelectric scans of the interstellar Ca I line at 4226 A for four stars having strong interstellar Ca II K-lines. The Ca I line is detected in three, and possibly all four, cases, of which one was kn*wn previously. Negative Ca I results are also obtained for six stars with weaker K-lines. The significance of the resulting electron densities deduced from the Ca I and Ca II lines is discussed.

Hobbs, L. M.↗