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Stellar structure and mass loss on the upper asymptotic giant branch
ABSTRA C T We examine the envelope properties of asymptotic giant branch (AGB) stars as they evolve on the upper AGB and during the early post-AGB phase. Because of the high mass-loss rate, theExpand
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Rotation, planets, and the second parameter of the horizontal branch
ABSTRA C T We analyse the angular momentum evolution from the red giant branch (RGB) to the horizontal branch (HB) and along the HB. Using rotation velocities for stars in the globular cluster M13,Expand
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PREVENTION OF NITRATE LEAKAGE FROM THE HULA BASIN, ISRAEL: A CASE STUDY IN WATERSHED MANAGEMENT
Drainage of the Hula basin led to the exposure of about 2000 ha of organic soils. Corollary to a high subsidence rate, extensive nitrification and leaching of nitrates became evident, endangering theExpand
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POSSIBLE IMPLICATIONS OF THE PLANET ORBITING THE RED HORIZONTAL BRANCH STAR HIP 13044
We propose a scenario to account for the surprising orbital properties of the planet orbiting the metal-poor red horizontal branch star HIP 13044. The orbital period of 16.2 days implies that theExpand
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Overluminous Blue Horizontal-Branch Stars Formed by Low-Mass Companions
We construct a speculative scenario for rotation-induced extra helium mixing to the envelope of horizontal-branch (HB) stars. This scenario differs from previous ones in that the mixing occurs afterExpand
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CAN A SINGLE AGB STAR FORM AN AXIALLY SYMMETRIC PLANETARY NEBULA
We apply a method, which is traditionally used for the solar magnetic field, to estimate the magnetic activity of AGB stars. We find that any magnetic field model which tries to explainExpand
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Eccentric Binary Model for Off-Center Planetary Nebula Nuclei
We examine the influence of eccentric binary progenitors on the morphologies of their descendant planetary nebulae. In particular, we consider how mass loss via a stellar wind by an asymptotic giantExpand
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Criticism of recent calculations of common envelope ejection
We re-examine a recent claim made by Han et al. that the ionization energy in the envelope has to be included in the ejection criterion of common envelopes. In particular, we argue that: (i) theyExpand
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