Systematics of Dwarf Novae
نویسندگان
چکیده
منابع مشابه
Dwarf Novae at Low Mass Transfer Rates
We show that if the inner regions of accretion discs in quiescent dwarf nova systems are removed by magnetic disruption or evaporated by siphon ows, the remaining disc is globally stable for mass transfer rates < 10 15 g s 1. This implies that (super)outbursts in these systems have to be triggered by an enhanced mass transfer form the companion. We suggest that the lack of normal outbursts in W...
متن کاملVery-high-energy γ-ray observations of novae and dwarf novae with the MAGIC telescopes
Context. In the last five years the Fermi Large Area Telescope (LAT) instrument detected GeV γ-ray emission from five novae. The GeV emission can be interpreted in terms of an inverse Compton process of electrons accelerated in a shock. In this case it is expected that protons in the same conditions can be accelerated to much higher energies. Consequently they may produce a second component in ...
متن کاملHydrodynamic simulations of irradiated secondaries in dwarf novae
Context. Secondary stars in dwarf novae are strongly irradiated during outbursts. It has been argued that this could result in an enhancement of the mass transfer rate even though the L1 region is shadowed from the primary irradiation by the accretion disc. Previous investigations of the possibility of a circulation flow transporting heat from hot regions to L1 gave opposite answers. Aims. We i...
متن کاملOn the Origin of Episodic Accretion in Dwarf Novae
We show that dwarf nova disks in quiescence have rather low magnetic Reynolds number, of order 10. Numerical simulations of magnetized accretion disks suggest that under these conditions magnetohydrodynamic turbulence and the associated angular momentum transport is sharply reduced. This could be the physical origin of episodic accretion in dwarf nova disks. If so, the standard disk instability...
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: International Astronomical Union Colloquium
سال: 1987
ISSN: 0252-9211
DOI: 10.1017/s0252921100104580