Figure 9: Mass-loss rate vs. orbital period for “typical” AM CVn-stars: an interacting double
degenerate system with initial masses of donor and accretor and (red line) and
a “semidegenerate” low-mass helium star donor plus white dwarf accretor of the same initial masses
(blue line). Black dots on the red curve mark positions of the system at
from Roche-lobe overflow; on the blue curve they mark . Green lines mark
lower and upper limits of the disk instability region according to Tsugawa and Osaki [406]. Below
the magenta circles and conventional evolutionary computations may be not adequate for
description of mass-transfer process (see the text).
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