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J/PASP/109/759 Rotational Velocities of Intermediate-mass MS Stars (Wolff+ 1997)

Rotational Velocities of Intermediate-mass Main Sequence Stars Wolff S.C., Simon T. <Publ. Astron. Soc. Pac. 109, 759 (1997)> =1997PASP..109..759W
ADC_Keywords: Rotational velocities; Stars, normal; Spectroscopy Description: Rotational velocities are reported for intermediate-mass main-sequence stars selected from Gray (1986, Gray and Garrison 1987, 1989a, 1989b). Measured rotational velocities, with photometric data from SIMBAD, are given in table1.dat for 249 stars. The measurements are based on new, high-S/N CCD spectra from the Coude Feed Telescope of the Kitt Peak National Observatory. Published velocities for 294 stars are provided in table2.dat. Abstract: (from Publ. Astron. Soc. Pac. 109, 759 (1997)) We analyze these rotation rates for a dependence on both mass and age. We compare the average rotation speeds of the field stars with mean velocities for young stars in Orion, the Α Persei cluster, the Pleiades, and the Hyades. The average rotation speeds of stars more massive than ∼1.6 Msol experience little or no change during the evolutionary lifetimes of these stars on the zero age main sequence (ZAMS) or within the ZAMS band. Less massive stars in the range between 1.6 Msol and 1.3 Msol also show little decline in mean rotation rate while they are on the main sequence, and at most a factor of two decrease in velocity as they evolve off the main sequence. The e-folding time for the loss of angular momentum by the latter group of stars is at least 1-2 billion years. This inferred characteristic time scale for spindown is far longer than the established rotational braking time for solar-type stars with masses below ∼1.3 Msol. We conclude from a comparison of the trends in rotation with trends in chromospheric and coronal activity that the overall decline in mean rotation speed along the main sequence, from ∼2 Msol down to ∼1.3 Msol, is imposed during the pre-main-sequence phase of evolution, and that this pattern changes little thereafter while the star resides on the main sequence. The magnetic activity must therefore play only a minor role in determining the rotation rates of the intermediate-mass stars, either because a solar-like dynamo is weak or absent, or else the geometry of the magnetic field is appreciably less effective in removing angular momentum from these stars. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 45 249 Measured rotational velocities table2.dat 46 294 Published rotational velocities
See also: III/22 : Rotation of Evolving A and F Stars (Danziger+ 1972) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD number 8- 12 F5.2 mag B-V *B-V color index 14- 18 F5.3 mag beta *Hβ index 19- 24 F6.3 mag b-y *b-y color index 26- 30 F5.3 mag c1 *c1 index 32- 36 F5.2 mag mag Absolute magnitude MV 38 A1 --- l_vsini [<]? Limit flag on V*Sin(i) 40- 42 I3 km/s vsini Measured V*Sin(i) 44- 45 I2 --- bin *? Bin in Fig. 3(a), color-magnitude
Note on B-V, beta, b-y, c1: Photometric data from SIMBAD. Note on bin: A blank indicates that the star lies beyond the terminal age main sequence (TAMS).
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD number 8- 11 F4.2 mag B-V B-V color index 13- 17 F5.3 mag beta Hβ index 19- 23 F5.3 mag b-y b-y color index 25- 29 F5.3 mag c1 c1 index 31- 35 F5.2 mag mag Absolute magnitude MV 37 A1 --- l_vsini [<]? Limit flag on V*Sin(i) 39- 41 I3 km/s vsini Published V*Sin(i) 43- 44 I2 --- bin *? Bin in Fig. 3(a), color-magnitude 46 I1 --- ref *[1-5] Reference code
Note on bin: A blank indicates that the star lies beyond the terminal age main sequence (TAMS). Note on ref: 1 = Slettebak et al. 1975ApJS...29..137S 2 = Kraft 1967ApJ...150..551K 3 = Danziger and Faber 1972A&A....18..428D 4 = Soderblom 1983ApJS...53....1S 5 = Benz and Mayor 1984A&A...138..183B
Acknowledgment: The ADC thanks Dr. Simon for providing the data tables as LaTeX files. J.A. Watko [SSDOO/ADC] converted the tables to ASCII. References: Benz W., Mayor M. 1984. Astron. Astrophys. 138, 183. (1984A&A...138..183B) Danziger I.J., Faber S.M. 1972. Astron. Astrophys. 18, 428. (1972A&A....18..428D, CDS Cat. III/22) Gray R.O. 1986. Thesis, U. Toronto. Gray R.O., Garrison R.F. 1987. Astrophys. J. Suppl. 65, 581. (1987ApJS...65..581G) Gray R.O., Garrison R.F. 1989a. Astrophys. J. Suppl. 69, 301. (1989ApJS...69..301G) Gray R.O., Garrison R.F. 1989b. Astrophys. J. Suppl. 70, 623. (1989ApJS...70..623G) Kraft R.P. 1967b. Astrophys. J. 150, 551. (1967ApJ...150..551K) Slettebak A., Collins G.W., Boyce P.B., White N.M., Parkinson T.D. 1975. Astrophys. J. Suppl. 29, 137. (1975ApJS...29..137S) Soderblom D.R. 1983 Astrophys. J., Suppl. 53, 1 (1983ApJS...53....1S) Wolff S.C., Simon T. 1997. Publ. Astron. Soc. Pac. 109,759. (1997PASP..109..759W)
(End) Julie Anne Watko [SSDOO/ADC] 08-Jan-1998
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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