Radiocontinuum and recombination lines toward CRL618 - Evidence for an ionized stellar wind?

Details Radiocontinuum and recombination lines toward CRL618 - Evidence for an ionized stellar wind? Radiocontinuum and recombination lines toward CRL618 - Evidence for an ionized stellar wind?

May 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988a%26a...197l..15m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 197, no. 1-2, May 1988, p. L15-L18.

Astronomy and Astrophysics

Astrophysics

38

Electron Energy, H Alpha Line, Ion Recombination, Ionized Gases, Planetary Nebulae, Radio Emission, Stellar Winds, Emission Spectra, Flux Density, Line Spectra, Stellar Mass Ejection

Scientific paper

The authors report the first detection of radio recombination lines towards CRL 618. They have detected the H41 α, H35 α and H30 α at the wavelengths of 3.5, 2 and 1.3 mm respectively. The continuum emission has been also measured at these wavelengths and at 1.3 cm. The averaged LTE electron temperature of the ionized gas is 13000K. The continuum and recombination line intensities are consistent with their emission arising in an isothermal stellar wind with a terminal velocity of ≡20 kms-1. The mass loss rate obtained from the continuum and the recombination lines is 2.7×10-5M_sun; yr-1. The large variation of the flux density at 3.4 mm over the past 10 years (a factor of 3.5) suggests that we are not only observing the ionized gas ejected in the red giant phase, but an ionized stellar wind generated by the central star whose mass loss rate has increased in the last decade.

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