The spectrum of H1-36 /= 3U 1746-37/ at radio wavelengths

Details The spectrum of H1-36 /= 3U 1746-37/ at radio wavelengths The spectrum of H1-36 /= 3U 1746-37/ at radio wavelengths

Sep 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977mnras.180p..97p&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 180, Sept. 1977, p. 97p-100p.

Astronomy and Astrophysics

Astronomy

5

Emission Spectra, Radio Sources (Astronomy), Radio Spectra, X Ray Sources, Astronomical Models, Ion Temperature, Nebulae, Plasma Density, Radiant Flux Density, Stellar Mass Ejection, Stellar Models, Stellar Structure, Thermal Radiation

Scientific paper

Flux-density measurements at frequencies of 2.7 to 90 GHz, three-element interferometric observations, and some optical data are reported for the high-excitation emission-line object H1-36, which has been suggested as the optical counterpart of the X-ray source 3U 1746-37. The radio spectrum of this object is found to suggest thermal emission from an extensive expanding circumstellar shell, which was probably produced by prolonged mass outflow from the central stellar system. It is argued that if the identification of H1-36 with 3U 1746-37 is correct and if the distance to the object is relatively small (e.g., a few hundred parsecs), the central stellar system is probably a mass-transfer binary with a compact object as one component. However, if the distance to H1-36 is 2 kpc or more, mass outflow would be the basic mechanism, and both mass transfer and X-ray emission would be side effects. The symbiotic nature of the radio spectrum is mentioned in passing.

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