Results 11 to 20 of about 1,202 (206)
Studying Asymptotic Giant Branch Stars in the JWST Era [PDF]
Universe, 2020 We explore the potential offered by the incoming launch of the James Webb Space Telescope, to study the stars evolving through the asymptotic giant branch (AGB) phase. To this aim we compare data of AGB stars in the Large Magellanic Cloud, taken with the
Paolo Ventura +3 more
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Turbulent dynamo in asymptotic giant branch stars [PDF]
Monthly Notices of the Royal Astronomical Society, 2002 Using recent results on the operation of turbulent dynamos, we show that a turbulent dynamo can amplify a large scale magnetic field in the envelopes of asymptotic giant branch (AGB) stars. We propose that a slow rotation of the AGB envelope can fix the symmetry axis, leading to the formation of an axisymmetric magnetic field structure.
Noam Soker, Essam Zoabi
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Magnetic Flares on Asymptotic Giant Branch Stars [PDF]
The Astrophysical Journal, 2003 We investigate the consequences of magnetic flares on the surface of asymptotic giant branch (AGB) and similar stars. In contrast to the solar wind, in the winds of AGB stars the gas cooling time is much shorter than the outflow time. As a result, we predict that energetic flaring will not inhibit, and may even enhance, dust formation around AGB stars.
Noam Soker, Joel H. Kastner
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A Solar‐like Cycle in Asymptotic Giant Branch Stars [PDF]
The Astrophysical Journal, 2000 I propose that the mechanism behind the formation of concentric semi-periodic shells found in several planetary nebulae (PNs) and proto-PNs, and around one asymptotic giant branch (AGB) star, is a solar-like magnetic activity cycle in the progenitor AGB stars.
Noam Soker
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Dynamical Models of Asymptotic-Giant-Branch Stars [PDF]
Symposium - International Astronomical Union, 1974 The dynamical behaviour of the envelopes of four asymptotic-giant-branch stars of composition (X, Z)=(0.68, 0.02) and luminosity log L/L⊙ = 3.41, 3.60, 3.85 and 4.14 has been studied. At log L/L⊙ = 3.41, the envelope pulsates in the first-overtone mode and exhibits properties similar to those of the Mira variables.
P. R. Wood
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Fluorine Production in Asymptotic Giant Branch Stars [PDF]
Symposium - International Astronomical Union, 2000 The present status of our understanding of fluorine production in asymptotic giant branch stars is reviewed, and future perspectives are presented.
N. Mowlavï, A. Jorissen, M. Arnould
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Magnetic Mixing in Red Giant and Asymptotic Giant Branch Stars [PDF]
The Astrophysical Journal, 2008 The available information on isotopic abundances in the atmospheres of low-mass Red Giant Branch (RGB) and Asymptotic Giant Branch (AGB) stars requires that episodes of extensive mixing occur below the convective envelope, reaching down to layers close to the hydrogen burning shell (Cool Bottom Processing).
Jason Nordhaus +4 more
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Thes‐Process in Rotating Asymptotic Giant Branch Stars
The Astrophysical Journal, 2003 50 pages, 13 figures, ApJ in press, tentatively scheduled for v593 n2 August 20 ...
Falk Herwig, N. Langer, Maria Lugaro
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s process in low-mass asymptotic giant branch stars [PDF]
Nuclear Physics A, 2005 pages ...
O. Straniero, R. Gallino, S. Cristallo
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Asymptotic giant branch stars in the Phoenix dwarf galaxy [PDF]
Monthly Notices of the Royal Astronomical Society, 2008 JHKs near-infrared photometry of stars in the Phoenix dwarf galaxy is presented and discussed. Combining these data with the optical photometry of Massey et al. allows a rather clean separation of field stars from Phoenix members. The discovery of a Mira variable (P = 425 days), which is almost certainly a carbon star, leads to an estimate of the ...
J. W. Menzies +5 more
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