close binary evolutionmassive starsHR diagramstatistical studymass transferA statistical study is presented on the distribution of different kinds of massive star classes in the HR diagram using recent calculations of massive single star and massive close binary evolution. The influence of the mass ...
it was demonstrated that a strong correlation exists between the morphology of observed SLF variability and the location of a star in the Hertzsprung–Russell (HR) diagram (Bowman et al.2020)
They affect the tracks in the HR diagram, the lifetimes, the surface abundances, the hardness of the radiation field, the chemical yields, the presupernova status, the nature of the remnant, the mechanical energy released in the interstellar medium, etc. . . In this paper, after recalling ...
Our novel evolution models exhibit vertical evolution in the HR-diagram from the zero-age main sequence due to a self-regulatory effect driven by their wind-dominated nature, and we discuss what wind physics sets the stellar upper-mass limit. Our estimate for the Sunburst Arc in Vink (2023)...
The effects of rotation on the tracks in the HR diagram, the lifetimes, the isochrones, the blue-to-red supergiant ratios, the formation of Wolf-... Maeder,Andre,Meynet,... - 《Annual Review of Astronomy & Astrophysics》 被引量: 146发表: 2000年 POPULATION PARAMETERS OF INTERMEDIATE-AGE ...
(Meynet & Maeder 1997). Structural effects due to the centrifugal force are in general small in the interior. However, the distorsion of stellar surface may be large enough to produce significant shifts in the HR diagram (Maeder & Peytremann 1970). 2.2. Internal transport For the ...
Our mass limit to stars detected in all three bands is 0.1M ⊙ for a pre-main sequence star of age 0.7 Myr. The overall age of the pre-main sequence stars in the core region of NGC 3603 has been derived from isochrone fitting in the colour-magnitude diagram, leading to 0.3–1.0 Myr...
The key properties of a (single) massive star are defined by its initial mass and metallicity, but its path in the Hertzsprung–Russell diagram and ultimate fate depend critically on both mass loss and rotation [22, 23]. Studies have shown that the effects of rotation are enhanced at low ...
(blue-shifted)direction.Such a characteristic structure can arise from masers from an edge-on rotating disk or accelerating out,ow. In a case of an edge-on rotating Keplerian disk we can estimate the lower limit of the mass of a central star (e.g.Phillips et al. 1998).Assuming the ...
The adopted mass loss rate parameterization is fitted on observations, yielding mass loss rate expressions which differ according to star location in the HR diagram. Emphasis is put on the location of the He-burning stars on the diagram, and attention is given to the observational results of ...