An upper limit to coronal X-rays from single, magnetic white dwarfs
نویسندگان
چکیده
منابع مشابه
Accretion on to Magnetic White Dwarfs
The Magnetic Cataclysmic Variables (MCVs) are close interacting binaries where mass is transferred from a late type secondary star to a magnetic white dwarf. Two modes of accretion can be identified depending on the strength of the magnetic field, the mass transfer rate and orbital parameters. (a) Disced Accretion: In the Intermediate polars (IPs), the mass transfer stream circularises and form...
متن کاملMagnetic Accretion Onto White Dwarfs
The influence of the magnetic field on process of the accretion onto White Dwarfs in Cataclysmic Variables (CVs) is discussed. Except for the Polars or AM Her objects, the strength of magnetic field can not be measured directly in CVs by modern techniques. But there is growing evidence that most of the types of Cataclysmic Variables classified on the basis of their observational characteristics...
متن کاملAccretion onto Magnetic White Dwarfs
Recent developments in the accretion onto magnetic white dwarfs are reviewed. Accreting magnetic white dwarfs display many of the characteristics of accreting systems of a galactic scale, with the advantage that in these systems the accreting material is collimated into a relatively well-determined 1-dimensional ow.
متن کاملLarge-scale Solar Coronal Structures in Soft X-rays and Their Relationship to the Magnetic Flux
We have investigated the relationship between magnetic activity and coronal structures using soft X-ray data from the Yohkoh soft X-ray telescope and magnetic field data from the Kitt Peak Solar Observatory for the period of 1991–2001 and EUV data from the Solar and Heliospheric Observatory EUV Imaging Telescope for 1996–2001. The data are reduced to Carrington synoptic maps, which reveal two t...
متن کاملX-rays from magnetic massive OB stars
The magnetic activity of solar-type and low-mass stars is a well known source of coronal X-ray emission. At the other end of the main sequence, X-rays emission is instead associated with the powerful, radiatively driven winds of massive stars. Indeed, the intrinsically unstable line-driving mechanism of OB star winds gives rise to shock-heated, soft emission (∼0.5 keV) distributed throughout th...
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ژورنال
عنوان ژورنال: Journal of Astrophysics and Astronomy
سال: 1993
ISSN: 0250-6335,0973-7758
DOI: 10.1007/bf02702364