Superhumps and their Amplitudes

• Autorzy: Smak J.
• Języki publikacji: EN

Abstrakty

EN

Superhump amplitudes observed in dwarf novae during their superoutbursts depend on orbital inclination: the maximum amplitudes in systems with low inclinations are A₀≈0.25 mag, while at higher inclinations they increase from A₀≈0.3 mag to A₀≈0.6 mag. The mean maximum superhump amplitudes normalized to the average luminosity of the disk are: <A_n>=0.34±0.02 mag in low inclination systems and only <A_n>=0.17±0.01 mag in high inclination systems. This shows that at high inclinations the superhump light source is partly obscured by the disk edge and implies that it is located close to the disk surface but extends sufficiently high above that surface to avoid full obscuration. Superhump amplitudes in high inclination systems show modulation with beat phase (φ_b), interpreted as being due to azimuth-dependent obscuration effects in a non-axisymmetric disk. In addition they show modulation with 2φ_b which implies that the orientation of the superhump light source is correlated with the direction of the stream. The dependence of superhump amplitudes on orbital inclination and their modulation with beat phase eliminate the tidal-resonance model for superhumps. Instead they support an alternative interpretation of superhumps as being due to periodically modulated dissipation of the kinetic energy of the stream. Superhump amplitudes in permanent superhumpers are <A>=0.12 mag, i.e., much smaller than the maximum amplitudes observed during superoutbursts.

Słowa kluczowe

EN

accretion; accretion disks; novae; cataclysmic variables; stars: dwarf novae

• Wydawca: Copernicus Foundation for Polish Astronomy
• Czasopismo: Acta Astronomica
• Rocznik: 2010
• Tom: Vol. 60, No. 4
• Strony: 357--371
• Opis fizyczny: Bibliogr. 60 poz., tab., wykr.

Twórcy

autor

Smak J.

• N. Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716 Warsaw, Poland

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