2003/09/03 by Gavin Ramsay, M. Cropper, Mark Cropper +4 · 1 citation
Earth and Planetary Sciences · Physics and Astronomy · #Accretion (finance) #Accretion disc #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Cataclysmic variable star #High-pressure geophysics and materials #Light curve #Mass ratio #Orbital period #Physics #Pulsars and Gravitational Waves Research #Stars #White dwarf #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2004.07242.x
published as Mon.Not.Roy.Astron.Soc.347:95,2004 · accepted MNRAS
arxiv created 2003/09/03 · openalex publication_date 2003/12/15 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We present phase-resolved XMM–Newton data of three short-period polars: V347 Pav, GG Leo and EU UMa. All three systems show one dominant accretion region, which is seen for approximately half the orbital cycle. GG Leo shows a strong dip feature in its X-ray and ultraviolet (UV) light curves, which is due to absorption of X-rays from the accretion site by the accretion stream. The emission in the case of EU UMa is dominated by soft X-rays: its soft/hard X-ray ratio is amongst the highest seen in these objects. In contrast, GG Leo and V347 Pav shows a ratio consistent with that predicted by the standard shock model. We infer the mass of the white dwarf and explore the effect of restricting the energy range on the derived parameters.