Results 181 to 190 of about 18,777 (215)
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1990
Cool stars on the asymptotic giant branch (AGB) form a late stage of stellar evolution shortly before loosing their outer layers and moving into the state where a planetary nebula is excited. These stars show severe mass-loss rates between 10−8 M ⊙yr−1 at the lower AGB, increasing to some l0−4 M ⊙yr−1 as the star evolves to the top of the AGB while ...
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Cool stars on the asymptotic giant branch (AGB) form a late stage of stellar evolution shortly before loosing their outer layers and moving into the state where a planetary nebula is excited. These stars show severe mass-loss rates between 10−8 M ⊙yr−1 at the lower AGB, increasing to some l0−4 M ⊙yr−1 as the star evolves to the top of the AGB while ...
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Late-Type Stars and Close Binaries
2007Late-type stars are generally characterized by the chromospheric structure showing active phenomena observable by the formation of emission lines and emission of X-ray and UV radiations. In the optical region, most ubiquitous emission lines are CaII H, K lines, while Hα line appears in fully developed chromospheres.
Tomokazu Kogure, Kam-Ching Leung
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Infrared Spectra of Late-Type Stars
1971Spectra have been obtained in the 2μ atmospheric window with a resolution of 32 and 65Å of late-type dwarfs, giants, supergiants, and long period variables. In the non-variable stars, the first overtone band of C0 at 2.29μ shows a systematic increase with both increasing luminosity and decreasing temperature. This increasing strength is interpreted as
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Spectroscopic study of late type stars
Vistas in Astronomy, 1966Abstract Spectroscopic investigation of late type stars from both observation and theory is discussed. Starting from the identification problem of elements in these stars, some preliminary studies of chemical abundance are made by the curve of growth method.
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Prominences on Late Type Active Stars
1996There is increasing evidence of prominence-like neutral hydrogen clouds suspended in the otherwise hot coronae of active late-type stars. We review this evidence here and discuss the nature of these clouds. In particular we discuss their possible role in rotational braking.
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Rotational Velocities of Late-Type Stars
Publications of the Astronomical Society of the Pacific, 1997A calibration based on the results of Gray has been used to determine projected rotational velocities for 133 bright stars with spectral types of F, G, or K, most of which appear in {The Bright Star Catalogue}. The vast majority have {v} sin {i} ≤q 10 km s-1 and, thus, are slow rotators.
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Outer Atmospheres of Late-Type Stars
1981I will attempt to summarize our limited understanding of the outer atmospheres of red giants by describing recent important observational results concerning chromospheres and coronae in late-type stars and how red giants fit into the emerging picture.
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Health insurance status and cancer stage at diagnosis and survival in the United States
Ca-A Cancer Journal for Clinicians, 2022Jingxuan Zhao +2 more
exaly
ROSAT Observations of Late-Type Stars
1993I will review results from X-ray observations of late-type stars in the ROSAT all-sky survey as well as in the ROSAT pointing program. The various background components and the resulting sensitivity of the all-sky survey will be discussed. Among the scientific issues covered are coronal dividing lines, hybrid stars and X-ray microflares.
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Ages of Spotted Late-Type Stars
1991It is shown that 87% of spotted single late-type field stars belong to the young disc and Local Association population with ages from 107 to 109 year. A comparison of photometric periods of T Tau-type, cluster, and single field stars confirms that the period difference is largest in the stars with ages of 107 – 108 year.
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