Results 21 to 30 of about 20,031 (219)
OH Masers in Envelopes of Late Type Stars [PDF]
Symposium - International Astronomical Union, 1987 Two studies of OH maser emission in envelopes of late type stars -miras (3) and OH/IR objects- have been performed with the Nancay radio-telescope. Mainly, the OH miras are found with thicker dust envelopes than the non OH ones. A sample of unidentified IRAS point sources selected on their colors has been observed.
A.M. Le Squeren +4 more
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Isochrones for late-type stars [PDF]
Proceedings of the International Astronomical Union, 2008 AbstractA brief summary of the history of stellar evolution theory and the use of isochrones is given. The present state of the subject is summarized. The major uncertainties in isochrone construction are considered: chemical abundances and color calibrations, and the treatment of turbulent convection in stellar interior and atmosphere models.
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Gravity darkening in late-type stars [PDF]
Astronomy & Astrophysics, 2018 Context.Recent interferometric data have been used to constrain the brightness distribution at the surface of nearby stars, in particular the so-called gravity darkening that makes fast rotating stars brighter at their poles than at their equator. However, good models of gravity darkening are missing for stars that posses a convective envelope.Aim.In ...
Raynaud, Raphaël +4 more
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[Cii] emission and star formation in late-type galaxies [PDF]
Monthly Notices of the Royal Astronomical Society, 1999 A linear correlation between the ratio of the[CII( $$^{\text{2}}$$ P $$_{3/2}$$ →
Pierini, D. +3 more
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Differential Line Shifts in Late Type Stars [PDF]
International Astronomical Union Colloquium, 1980 AbstractThe differential line shifts method for studying convective type motions has been described in the review of Glebocki and Stawikowski at this colloquium. Here the results of differential line shifts for twenty late type stars are presented. Line shifts were determined either from published wavelength measurements (α CMi, β Peg, α Boo, α Ser, α ...
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A Spectroscopic Orbit for the Late-type Be Star β CMi [PDF]
The Astrophysical Journal, 2017 Abstract The late-type Be star β CMi is remarkably stable compared to other Be stars that have been studied. This has led to a realistic model of the outflowing Be disk by Klement et al. These results showed that the disk is likely truncated at a finite radius from the star, which Klement et al.
Nicholas A. Dulaney +14 more
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Flares in late-type stars: X-ray [PDF]
International Astronomical Union Colloquium, 1995 Flare-like brightenings, similar to those observed on the Sun but on a larger energy scale, are observed in a variety of late-type stars, including classical M dwarf flare stars, RS CVn-type binaries and pre-main sequence (PMS) objects. These events, which are observable over the whole electromagnetic spectrum, are interpreted as due to rapid release ...
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Solid Pseudopapillary Neoplasm of the Pancreas in Children and Adolescents: Expert Recommendations
Pediatric Blood &Cancer, EarlyView.ABSTRACT Solid pseudopapillary neoplasm of the pancreas (SPN) is a rare low‐grade malignant exocrine pancreatic tumor, mostly discovered during the second decade of life in females, with a very good prognosis, provided microscopically complete surgical excision is achieved.
Sabine Irtan +18 more
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Pediatric Blood &Cancer, EarlyView.ABSTRACT As part of the European Cooperative Study Group for Paediatric Rare Tumours initiative, we developed standard clinical practice guidelines for ovarian sex cord stromal tumors, based on comprehensive national and international cohort analyses, literature review, and a final expert consensus conference.
Dominik T. Schneider +15 more
wiley +1 more source
SPECTROSCOPIC ORBITS FOR 15 LATE-TYPE STARS
The Astronomical Journal, 2016 ABSTRACT Spectroscopic orbital elements are determined for 15 stars with periods from 8 to 6528 days with six orbits computed for the first time. Improved astrometric orbits are computed for two stars and one new orbit is derived. Visual orbits were previously determined for four stars, four stars are members of multiple systems, and ...
Daryl W. Willmarth +3 more
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