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The Hot End of Evolutionary Horizontal Branches
The Astrophysical Journal, 1995 postscript file of 10 pages plus 1 tables,rep.1 5 figures will be added later as postscript file The tex file and the other two not postscript figures are available upon request at scilla@vaxfe.fe.infn.it, rep ...
CASTELLANI V +2 more
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Non-variable horizontal-branch stars [PDF]
Symposium - International Astronomical Union, 1997 For 25 years our ignorance of the physical basis of this mass loss process has been the barrier to progress in understanding horizontal branch morphology. I review some recent observational and theoretical results which may be giving us clues about the nature of the mass loss process.
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Bimodal Distributions on the Horizontal Branch [PDF]
Symposium - International Astronomical Union, 1988 We present preliminary versions of log g - log Teff diagrams for a number of clusters with gaps in their blue horizontal branches and for two normal clusters.
Robert T. Rood, Deborah A. Crocker
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Revista Brasileira de Ortopedia, 2014 Objective:To describe the path of the infrapatellar branch of the saphenous nerve (IBSN) using the medial joint line, anterior tibial tuberosity (ATT), tibial collateral ligament and a horizontal line parallel to the medial joint line that passes over ...
Julio Cesar Gali +6 more
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Multi-objective design and optimization of squeezed branch pile based on orthogonal test
Scientific Reports, 2023 In recent years, the emergence of the squeezed branch pile has presented a new avenue for civil engineering, offering a distinctive structure and favorable mechanical characteristics.
Ziqi Wang, Cunbao Zhao, Wenyue Zhang
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Planets around Extreme Horizontal Branch Stars [PDF]
AIP Conference Proceedings, 2011 We review three main results of our recent study: We show that a proper treatment of the tidal interaction prior to the onset of the common envelope (CE) leads to an enhance mass loss. This might increase the survivability of planets and brown dwarfs that enter a CE phase.
Ealeal Bear +4 more
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Pulsational instabilities in hot pre-horizontal branch stars
EPJ Web of Conferences, 2017 The ϵ mechanism is a self-excitation mechanism of pulsations which acts on the regions where nuclear burning takes place. It has been shown that the ϵ mechanism can excite pulsations in models of hot helium-core flash, and that the pulsations of LS IV-14·
Battich Tiara +3 more
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Gaps in the blue horizontal branch.
The Astrophysical Journal, 1976 Data leads to the conclusion that several distinct groups of stars exist on the field stars horizontal branch sequence. Consideration of current understanding of the advanced evolution of Population II stars indicates that, if Greenstein's (1971) ''extended horizontal-branch'' hypothesis is correct, these discrete horizontal-branch groups correspond to
B. Newell, J. A. Graham
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The structure of horizontal-branch models. I - The zero-age horizontal branch
The Astrophysical Journal Supplement Series, 1992 A detailed study of the structure of zero-age horizontal-branch (ZAHB) models is studied in order to show how the hydrostatic structure of these models changes with the input parameters and determines the H-R diagram location of a given model. The properties of composite polytropes on the homology-invariant (U,V)-plane are demonstrated.
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Diffusion in the Atmospheres of Blue Horizontal-Branch Stars [PDF]
The Astrophysical Journal, 2000 We investigate the effects of diffusion in the atmospheres of hot horizontal-branch stars using a model atmosphere code including diffusion self-consistently. Equilibrium stratifications (i.e., for which the diffusion velocity equals zero in each layer) are computed for models of effective temperatures between 10,000 and 25,000 K. The stratified models
, Hui-Bon-Hoa, , LeBlanc, , Hauschildt
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