Open AccessThe optical interstellar spectrum of Vel (HD 81188) and a measurement of interstellar cloud turbulence
Author(s) -
Dunkin S. K.,
Crawford I. A.
Publication year - 1999
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.1999.02117.x
Subject(s) - physics , astrophysics , turbulence , mean kinetic temperature , interstellar medium , line (geometry) , kinetic energy , line of sight , spectral resolution , spectral line , radial velocity , interstellar cloud , velocity dispersion , astronomy , galaxy , stars , mechanics , geometry , mathematics , quantum mechanics
We present ultra‐high resolution (R≈10 6 >) observations of lines due to interstellar Na i D, Ca ii K, K i and Ti ii towards κ Vel (HD 81188). Five velocity components are identified in both Na i and Ca ii, and two in K i; an upper limit is recorded for Ti ii. The very high spectral resolution has enabled us to resolve fully the intrinsic interstellar line profiles, and thereby obtain reliable measurements of the velocity dispersion parameters ( b ‐values) for all identified velocity components. By comparing the observed b ‐values for Na i and K i, which differ in mass by almost a factor of 2, it has been possible to derive the kinetic temperature ( T k ) and line‐of‐sight rms turbulent velocity ( v t ) simultaneously for the two clouds identified in both elements. We obtain rigorous upper limits of 0.46 and 0.33 km s ‐1 for v t in these two clouds, which are definitely subsonic at the measured temperatures. The three‐dimensional turbulent velocity (≡√ 3 × v t ) is also almost certainly subsonic for both components, although it might just exceed the isothermal sound speed if the kinetic temperatures were close to the lower limits permitted by the line‐profile analysis.