Observational evidence on the early development of stars in Cepheus A

Details Observational evidence on the early development of stars in Cepheus A Observational evidence on the early development of stars in Cepheus A

Nov 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...298..830h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 298, Nov. 15, 1985, p. 830-837.

Astronomy and Astrophysics

Astronomy

34

Nebulae, Pre-Main Sequence Stars, Radio Astronomy, Stellar Evolution, Water Masers, Astronomical Maps, H Ii Regions, Optical Thickness, Protostars

Scientific paper

New observations of Cep A have been made at 6 cm and 20 cm with the VLA in the A configuration, providing angular resolution of 0.3 arcsec and 1 arcsec, respectively. Spectral indices show that optically thick regions are present in some of the 14 components previously detected, as would be expected if there were mass outflow. These components are the most compact ones, with radii of less than 100 AU, and have H2O masers associated with the edges of the H II regions and OH masers which are well outside. Even larger values of spectral index at shorter wavelengths and in the most compact components, as measured by others, lead to a model which shows that they are probably due to B3 stars at the end of their protostar stage, when accretion is ending, and the central star has become extended, presumably in a convective stage. Subsequently, the central star contracts, and the H II region grows as the result of a combination of radiation pressure and the pressure of the H II region. The radio continuum data shows no evidence for the central stars being the source of the bipolar outflow.

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