Comparative performances of an objective grating concept in UV spectroscopic observations of solar system objects. III - Observations of diffuse emission lines

Details Comparative performances of an objective grating concept in UV spectroscopic observations of solar system objects. III - Observations of diffuse emission lines Comparative performances of an objective grating concept in UV spectroscopic observations of solar system objects. III - Observations of diffuse emission lines

Apr 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986a%26a...159..101b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 159, no. 1-2, April 1986, p. 101-107.

Astronomy and Astrophysics

Astrophysics

1

Astronomical Spectroscopy, Emission Spectra, Interplanetary Medium, Line Spectra, Solar System, Ultraviolet Spectroscopy, Diffuse Radiation, Helium, Hydrogen, Interstellar Gas, Lunar Occultation, Optical Filters, Spectral Resolution, Ultraviolet Filters, Velocity Distribution

Scientific paper

The observational capabilities of an objective grating instrument (Bruston et al., 1984) are fully described - as extended to the particular case of observations of diffuse emission lines - and compared with the usual techniques. It is shown that higher spectral resolutions can be obtained in particular conditions, using lunar occultations for example. It is suggested that the method be applied to measure both the H Lyman alpha (1216 angstrom) and the He I (584 angstrom) line profiles emitted through resonance scattering of solar photons, by the local interstellar medium (LISM). Such high resolution profile measurements do not presently exist in the case of the He component. For H, the more accurate spectral data so far obtained were provided by absorption cell techniques and concern only the total line width but not the complete emission profile. The method should permit a more precise description of the gas velocity distributions and new insights into the thermodynamical state of the LISM outside the solar interaction region and the interaction processes occurring within the solar cavity. Finally, the method is shown to be well suited for observations of other diffuse emissions such as the galactic one.

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