High precision spectropolarimetry of stars and planets. III - The wavelength dependence of interstellar polarization

Details High precision spectropolarimetry of stars and planets. III - The wavelength dependence of interstellar polarization High precision spectropolarimetry of stars and planets. III - The wavelength dependence of interstellar polarization

May 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984mnras.208..461w&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 208, May 15, 1984, p. 461-480.

Astronomy and Astrophysics

Astronomy

3

Astronomical Spectroscopy, Interstellar Matter, Planetology, Polarization Characteristics, Stellar Spectra, Cosmic Dust, Interstellar Extinction, Ophiuchi Clouds, Ultraviolet Astronomy, Wavelengths

Scientific paper

The interstellar polarization curve has been measured for three stars at a resolution of 50 Å. Low amplitude structure is present in each case. For Zeta Ophiuchi, the star studied in greatest detail (3100 - 7600 Å), the structure includes an oscillation in the degree of polarization at λ ⪆ λmax and a feature about 200 Å wide near 4100 Å. 55 Cygni shows a feature of similar width and amplitude but at 4400 Å. The rotation of position angle across the spectrum seen in all three stars may be interpreted in terms of two or more dust clouds along the line-of-sight. These clouds must differ in grain size and grain size distribution as well as in the direction of grain alignment. The authors argue that the structure in Zeta Ophiuchi beyond λmax may be due to magnetite impurities in silicate grains.

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