1998/05/06 by S. A. Drake, Stephen A. Drake, Drake, Stephen A.
Engineering · Physics and Astronomy · #Astronomical Observations and Instrumentation #Astrophysics (astro-ph) #FOS: Physical sciences #Pulsars and Gravitational Waves Research #Solar and Space Plasma Dynamics #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9805049
8 pages, no figure, to appear in: Proc. of the 26th workshop of the European Working Group on CP stars, eds. P. North, A. Schnell and J. Ziznovsky, Contrib. Astr. Obs. Skalnate Pleso Vol. 27, No 3
arxiv created 1998/05/06 · openalex publication_date 1998/05/06 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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 ~35 MCP stars of the Helium-peculiar and Silicon-strong subclasses, with a functional dependence of radio luminosity LR ∝ Teff7 Hs1.2 Prot-0.6, where Teff is the effective temperature, Hs is the surface magnetic field strength, and Prot 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 (~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.