CAOSP abstracts, Volume: 27, No.: 3, year: 1998

Abstract: Before 1985, attempts to detect radio or X-ray emission from Magnetic CP (MCP) stars were either fruitless or ambiguous. However, more successful results have been obtained in the last dozen years: (i) Radio emission has now been detected from appr. 35 MCP stars of the Helium-peculiar and Silicon-strong subclasses, with a functional dependence of radio luminosity L(R) proportional to T_(eff)^(7) H_(s)^(1.2) P_(rot)^(-0.6), where T(eff) is the effective temperature, H_(s) is the surface magnetic field strength, and P_(rot) is the rotational period; rotational modulation of the radio emission has also been observed for several MCP stars. All of this evidence suggests that it is the MCP stars themselves, not close companions, that are responsible for the radio emission; (ii) The X-ray emission properties of MCP stars are however still poorly characterized: although a moderate number (appr. 18) have by now been associated with X-ray sources, the lack of a clear correlation of this X-ray emission with other stellar parameters has made it difficult to rule out the close companion hypothesis.

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