Download Angular Momentum Evolution of Young Stars by Peter Bodenheimer (auth.), S. Catalano, J. R. Stauffer PDF

By Peter Bodenheimer (auth.), S. Catalano, J. R. Stauffer (eds.)

This ebook stories the lawsuits of the NATO complicated learn Workshop on "An­ gular Momentum Evolution of younger Stars" held from 17 to 21 September 1990 at Noto, Italy. The workshop had its instant beginning in a dialogue concerning the availability of stel­ lar rotation information, that happened in 1987 at Viana do Castelo Portugal in the course of the NATO assembly, Formation and Evolution of Low Mass Stars. We famous that just about two decades had handed because the final assembly on stellar rotation and that major growth within the statement of rotation premiums in low mass stars were made. over the past twenty years, new effective instrumentation (CCD and photon counting de­ tectors and echelle spectrographs) and new research concepts (profile Fourier research) have allowed us to degree rotational velocities as little as 1-2 km/s and to arrive low mass stars in younger clusters. regardless of those advances, rotational velocities of low mass stars might have remained difficult to figure out if all unmarried, low mass stars later than pass had rotational velocities of order or under 10 km/sec. facts that this isn't continually the case was once first supplied by way of the photometric variability facts acquired by means of van Leeuwen and Alphenaar for ok dwarfs within the Pleiades and extra lately by means of the vsini measurements of low mass stars in different younger clusters.

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In The Sun in Time, ed. C. P. Sonett (Tucson: Univ. of Arizona Press), in press. Levy, E. , and Sonett, C. P. 1978. In Prot08tar8 and Planet8, ed. T. Gehrels (Tucson: Univ. of Arizona Press), p. 516. Lin, D. N. , and Papaloizou, J. 1980. Mon. Not. R. astr. , 191,37. Lin, D. N. , and Savonije, G. 1990. Ap. , 364,326. Lin, D. N. , and Pringle, J. E. 1987. Mon. Not. R. astr. , 225,607. , and Shu, F. H. 1989. Ap. , 342, 834. , and Schluter, A. 1955. Zeits. , 38, 190. Makalkin, A. B. 1987. Astr. ), 21, 324.

1 ne are displayed in Fig. 1. Each figure is labelled with the index I of the angular expansion in vector spherical harmonics. For I 2, ... , 12 the convergence of the series solution is better than 1%. A blown-out view of the subsurface region (ranging from l~ R* to R*) is shown in Figs. 2,3 and 4 for three different values of the coefficient of eddy viscosity. Note that the figures are not in scale and the velocity field is represented on a logarithmic scale. The relevant characteristics of the meridional circulation are summarized in Table 1 for different values of the coefficient of eddy viscosity lit.

And Papaloizou, J. 1980. Mon. Not. R. astr. , 191,37. Lin, D. N. , and Savonije, G. 1990. Ap. , 364,326. Lin, D. N. , and Pringle, J. E. 1987. Mon. Not. R. astr. , 225,607. , and Shu, F. H. 1989. Ap. , 342, 834. , and Schluter, A. 1955. Zeits. , 38, 190. Makalkin, A. B. 1987. Astr. ), 21, 324. Mathieu, R. , Benson, P. , Fuller, G. , Myers, P. , and Schild, R. E. 1988. Ap. , 330, 385. Mestel, L. 1968. Mon. Not. R. astr. , 138,359. Mestel, L. 1985. In Protostars and Planets II, eds. D. C. Black and M.

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