منابع مشابه
Fine mesh calculations of dwarf nova outbursts
We present new results from fine mesh calculations of dwarf nova outbursts. The vertical thermal and the radial vis-cous evolution of the accretion disk is followed simultaneously. This is essential for determining formation, structure, and propagation of transition fronts which are a fundamental constituent of the dwarf nova cycle. In addition to the equation of continuity of mass flow and the...
متن کاملConstraining Jet Theories Using Nova Outbursts
It is commonly accepted that jets have not been observed in cataclysmic variables (CVs) so far. This absence was recently explained by their low mass transfer rates compared with objects with jets. A mass accretion limit for jets in CVs was proposed to be Ṁ ∼ 10−7 − 10−6 M⊙/yr. There was, however, a report of evidence for jets in V1494 Aql, the second nova that erupted in Aquila in 1999. In thi...
متن کاملThe Nature of Dwarf Nova Outbursts
We show that if the dwarf-nova disc instability model includes the effects of heating by stream impact and tidal torque dissipation in the outer disc, the calculated properties of dwarf-nova outbursts change considerably, and several notorious deficiencies of this model are repaired. In particular: (1) outside-in outbursts occur for mass transfer rates lower than in the standard model as requir...
متن کاملWhite Dwarf Heating and Subsequent Cooling in Dwarf Nova Outbursts
We follow the time dependent thermal evolution of a white dwarf (WD) undergoing sudden accretion in a dwarf nova outburst, using both simulations and analytic estimates. The post-outburst lightcurve clearly separates into early times when the WD flux is high, and late times when the flux is near the quiescent level. The break between these two regimes, occurring at a time of order the outburst ...
متن کاملOn the occurrence of dwarf nova outbursts in post novae
We show that irradiation of the accretion disc by the white dwarf limits the occurrence of dwarf nova outbursts in post nova accretion discs. After the nova explosion, the white dwarf has to cool for up to ∼ 100 yr – depending on the orbital period (i.e., disc size) and the temperature of the white dwarf after the nova-eruption – before the disc can begin producing dwarf nova outbursts. During ...
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 2007
ISSN: 0035-8711,1365-2966
DOI: 10.1111/j.1365-2966.2006.11254.x