On the accretion mode of the intermediate polar V1025 Centauri

Details On the accretion mode of the intermediate polar V1025 Centauri On the accretion mode of the intermediate polar V1025 Centauri

2002-01-29

arxiv.org/abs/astro-ph/0201474v1

Mon.Not.Roy.Astron.Soc. 333 (2002) 84

Astronomy and Astrophysics

Astrophysics

9 pages, 8 figures, To appear in MNRAS, includes low-res figures to reduce size

Scientific paper

10.1046/j.1365-8711.2002.05381.x

The long white-dwarf spin periods in the magnetic cataclysmic variables EX Hya and V1025 Cen imply that if the systems possess accretion discs then they cannot be in equilibrium. It has been suggested that instead they are discless accretors in which the spin-up torques resulting from accretion are balanced by the ejection of part of the accretion flow back towards the secondary. We present phase-resolved spectroscopy of V1025 Cen aimed at deducing the nature of the accretion flow, and compare this with simulations of a discless accretor. We find that both the conventional disc-fed model and the discless-accretor model have strengths and weaknesses, and that further work is needed before we can decide which applies to V1025 Cen.

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