![]() © Dana Berry (STScI) |
![]() © 1998 M. A. Garlick: "Cataclysm II" |
![]() © 2002 M. A. Garlick: "Cataclysm IV" |
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| There are two important structures in a non-magnetic CV: | |
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1) The accretion disk, where about half of the gravitational potential energy of the accreting material is released, and |
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2) The boundary layer between the accretion disk and the surface of the white dwarf, where the kinetic energy of the flow is thermalized and radiated. |
| Because the effective temperature of the accretion disk ranges from ~ 5000 K at its outer edge to ~ few x 104 K at its inner edge, it radiates over a broad energy range from the optical through the far ultraviolet. | |
| Because of the small size and high luminosity of the boundary layer, its temperature is significantly higher than that of the accretion disk. When the mass-accretion rate is high (Mdot ~ 10-8 Msun/yr; e.g., novalike variables and dwarf novae in outburst), the boundary layer is optically thick and its temperature ~ 105 K (10 eV), so it radiates primarily in the extreme ultraviolet and soft X-ray bandpasses. When the mass-accretion rate is low (Mdot ~ 10-11 Msun/yr; e.g., dwarf novae in quiescence), the boundary layer is optically thin and its temperature ~ 108 K (10 keV), so it radiates primarily in the X-ray bandpass. | |
| As evidenced by the P Cygni profiles of their ultraviolet resonance lines, high mass-accretion rate non-magnetic CVs are known to have strong (Mdot ~ 10-11 Msun/yr), high-velocity (v ~ 3000 km/s) outflows ("winds") which are thought to be driven from the surface of the accretion disk by radiation pressure and possibly magnetic forces. | |
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| Novae | CV Subtypes | Non-Magnetic CVs | Intermediate Polars | Polars | |
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| Last modified December 13, 2004 | |||||
| UCRL-MI-135159 | |||||