Results 231 to 240 of about 24,585 (264)

Lithium 6104 A in Population II stars

, 2002
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Populations of rotating stars. II. Rapid rotators and their link to Be-type stars

Astronomy & Astrophysics, 2013
Granada, A., Ekstrxf6m, S., Georgy, C., Krtička, J., Owocki, S., Meynet, G., Maeder, A., Granada, A.; Ekstrxf6m, S.; Georgy, C.; Krtička, J.; Owocki, S.; Meynet, G.; Maeder, A.   +14 more
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Thionation-enhanced through-space electronic coupling and excited-state dynamics in helicene diimides.

Chem Commun (Camb)
D'Orazio-Colman A, T A, Saji S, Hariharan M, Ravat P.   +4 more
europepmc   +1 more source

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Formation of Population II Stars

Publications of the Astronomical Society of Japan, 1975
Abstract Thermal and dynamical properties of gas clouds of mass between 1 M◉ and 106  M◉ with a fractional mass of heavy elements Z=10−3 to Z=10−5 are investigated by comparing the time scales of cooling, heating, expansion, and contraction for two cases with and without grains.
Satoshi Miki, Takenori Nakano
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Evolution of Population II stars

Astronomy and Astrophysics Review, 1998
The current knowledge of the evolution of Population II stars, as observed in galactic halos and globular clusters, is outlined. The recent theoretical results provided by an improved physical understanding of the stars are reported, with a particular emphasis upon those stellar evolutionary phases which are the keystones of the interpretation of ...
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Lithium in Population II Stars

1992
NEW data about dwarfs : a few more metal-poor dwarfs have been observed for lithium at the CAT + CES at La Silla (ESO). These new results, together with a few new measurements in the literature show again a constant lithium abundance, confirming the trend previously found (the plateau).
F. Spite, M. Spite, R. Cayrel, S. Huille
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Accretion of Heavy Elements on Population II Stars

Publications of the Astronomical Society of Japan, 1957
Abstract The effect of accretion of heavy elements on spectral appearance of population II stars, especially of globular cluster stars, are investigated in detail. It is shown to be implausible to explain the existence of these heavy elements by the accretion from outside.
Hisao Takebe, Naoyuki Matsunami
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The Cepheids of Population II and Related Stars

Publications of the Astronomical Society of the Pacific, 2002
The Type II Cepheids include most intrinsic variables with periods between 1 and about 50 days, except for the classical Cepheids and the shortest semiregular variables of type M. The Type II Cepheids may be divided in groups by period, such that the stars with periods beween 1 and 5 days (BL Her class), 10-20 days (W Vir class), and greater than 20 ...
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Spectra of Population II Cepheid Variable Stars

1958
The physical properties of the population II cepheids have been studied using the following material: photoelectric observations of Arp, low dispersion spectra of Joy, high dispersion spectra taken by Sanford and Abt, and numerous moderate dispersion spectra obtained by the author. Radial velocity curves for ten cepheids are shown.
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Very regular high-frequency pulsation modes in young intermediate-mass stars

Nature, 2020
Tim Bedding, Jj Hermes, Tanda Li
exaly