Results 291 to 300 of about 41,072 (339)

Stellar Rotation in the Scorpio-Centaurus Association

The Astrophysical Journal, 1968
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Blood Pressure in Adolescence and Atherosclerosis in Middle Age.

JAMA Cardiol
Herraiz-Adillo Á, Eriksson H, Ahlqvist VH, Ballin M, Wennberg P, Daka B, Lenander C, Berglind D, Östgren CJ, Lundgren O, Rådholm K, Henriksson P.   +11 more
europepmc   +1 more source

Primordial Rotating Disk Composed of ≥15 Star Forming Clumps at Cosmic Dawn

Fujimoto S, Ouchi M, Kohno K, Valentino F, Giménez-Arteaga C, Brammer G, Furtak L, Kohandel M, Oguri M, Pallottini A, Richard J, Zitrin A, Bauer F, Boylan-Kolchin M, Dessauges-Zavadsky M, Egami E, Finkelstein S, Ma Z, Smail I, Watson D, Hutchison T, Rigby J, Welch B, Ao Y, Bradley L, Caminha G, Caputi K, Espada D, Endsley R, Fudamoto Y, González-López J, Hatsukade B, Koekemoer A, Kokorev V, Laporte N, Lee M, Magdis G, Ono Y, Rizzo F, Shibuya T, Shimasaku K, Sun F, Toft S, Umehata H, Wang T, Yajima H.   +45 more
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The Orion OB1 association. 1: Stellar content

, 1994
Brown, A.G.A., Geus, E.J. de, Zeeuw, P.T. de   +2 more
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Polarimetric Investigations of Stellar Associations

Astrophysics, 2002
The degree of polarization of light from stars in 44 O B associations as a function of interstellar absorption is investigated. It is shown that the character of the dependence of P on AV for stars in associations and stars not in associations depends on the value of AV: for AV ≤ 2m.5 it has a linear character and is the same for both groups of stars ...
E. Ye. Khachikian, M. A. Eritsian, R. Kh. Hovhannessian   +2 more
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Dynamical models of stellar associations

Astronomical & Astrophysical Transactions, 1998
Abstract Numerical N-body investigations of the dynamical evolution of a young stellar aggregate embedded in a massive interstellar cloud are presented. We discuss some mechanisms of the formation of OB-associations – traditional as well as new ones.
E. V. Moskal, V. G. Surdin
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Formation of stellar associations

Astrophysics and Space Science, 1970
The Rayleigh-Taylor instability forms massive complexes. When 1021 atoms cm−2 are gathered, X-rays which heat the gas and UV-rays which ionize carbon are absorbed. A layer should appear with temperatures as low as 6 K and density to 4×103 cm−3. Finally the layer is fragmented into stars whose masses may even be less than one solar mass. The temperature
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New stellar associations in M33 galaxy

Astrophysics and Space Science, 1984
Extending the numeration of Humphreys and Sandage (1980) 54 new associations are identified in the galaxy M33 by comparing the plates in theU andB system. The larger part of the associations are located in the spiral arms. The young associations are prevailing in proximity to the nucleus.
P. Z. Kunchev, G. R. Ivanov
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Stellar associations and complexes in M33

Astrophysics and Space Science, 1987
About 460 OB associations were selected by a comparison of theUBV plates. TheUBV photographic photometry of 1944 blue stars in the associations was made. The new associations appear like cores within Humphreys and Sandage's associations. Their star content, size distribution, and mean size ≈80 pc confirm their identity with the OB associations in the ...
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