stellar rotation/ mass intermediate starsHertzsprung-Russell diagramthermohaline mixingrotation-induced effectAims. Weak G-band (WGB) stars are a rare class of cool luminous stars that present a strong depletion in carbon, but also lithium abundance anomalies that have been little explored in the ...
The H-R diagram was developed in 1910 by the astronomers Ejnar Hertzsprung and Henry Norris Russell. Both men were working with spectra of stars — that is, they were studying the light from stars by usingspectrographs. Those instruments break down the light into its component wavelengths. The...
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Stars.- Population of Dynamically Formed Triples in Dense Stellar Systems.- Interferometric studies of multiple stars.- Interferometric orbits of new Hipparcos binaries.- New facts about Velorum: fewer but larger components.- Speckle Interferometry of Two Low-mass Triple Systems in the Solar ...
The HR diagram in the infrared (K, V-K) for the RR Lyrae stars of the globular cluster M3 is derived using published photometric data. Also shown is the relation - versus log PF for the RR Lyrae stars in the same cluster. Those stars which are the most evolved from ZAHB are well ...
Stars Classifying stars: H-R diagram Vogt-Russell theorem Mass-luminosity relation Evolution on the HR diagram. THE BIG BANG This model suggests that somewhere around 13.7 billion years ago all matter in the Universe was contained in a hot, dense particle. The temperature. ...
With the aid of these stellar models we analyze the HR diagram (HRD) of supergiant stars in the LMC by Fitzpatrick & Garmany (1990) and that of supergiant stars in the Milky Way by Blaha & Humphreys (1989). Particular attention is paid to the star counts across the HRD, the stars in...
Finally, the chapter notes that an extension of the SPB instability strip toward the supergiant regime ("SPBsg stars") has been suggested by Saio et al. 展开 关键词: β Cephei Be stars H‐R diagram pulsating stars slowly pulsating blue variables SPB stars SPBsg stars ...
At the zero age main sequence (ZAMS), the position in the HR diagram depends on the mass and metallicity of the stars. Massive stars have higher luminosities and temperatures than low-mass stars. Stars on the ZAMS are in hydrostatic and thermal equilibrium. Metal-poor stars are hotter and ...
Dwarf galaxies are by far the most numerous galaxies in the Universe, showing properties that are quite different from those of their larger and more luminous cousins. This review focuses on the physical and chemical properties of the interstellar medium