The Circumstellar Matter of the Magnetic Helium-Strong Star HD37017

Details The Circumstellar Matter of the Magnetic Helium-Strong Star HD37017 The Circumstellar Matter of the Magnetic Helium-Strong Star HD37017

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...273..509l&link_type=abstract

Astronomy and Astrophysics, Vol.273, NO. 2/JUNII, P. 509, 1993

Astronomy and Astrophysics

Astrophysics

3

Line: Profile, Stars: Chemically Peculiar, Stars: Circumstellar Matter, Stars: Individual: Hd 37017, Stars: Mass Loss

Scientific paper

Magnetic helium strong stars are characterized by a dipolar magnetic field; in principle, a stellar wind flows freely along the open field lines and stores matter between the closed lines (Shore t987). Since the dipole axis is tilted with respect to the rotational axis, an expanding wind above magnetic poles should give origin to a P-Cygni-like line profile when the dipole axis is oriented toward the observer.
Because of the reduced involved volume, with respect a spherical wind, the low mass-loss rate and the low expanding wind velocity for helium peculiar stars (Baker 1986), only small core profile variations are expected for the Hα line. To test such hypothesis, high resolution spectroscopy of Hα line for the helium strong star HD 37O17 has been performed when the dipole axis was oriented toward the earth.
The observed presence of a red-shifted small emission feature characterizing the Hα line core can thus be interpreted as due to a jet-like outflow above magnetic poles. Such outflow should be considered in interpreting the complex phenomenology characterizing magnetic helium peculiar stars.

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