Rotation, convection, and magnetic activity in lower main-sequence stars
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...If correct, the v sin i distributions would imply that most stars in our sample have equatorial velocities of at least 3 km s 1, which is inconsistent with measured rotation periods for inactive field stars (Noyes et al. 1984)....
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...…(20) Stauffer et al. (1989), (21) Soderblom et al. (1993), (22) Stauffer & Hartmann (1987), (23) Duncan et al. (1991), converted to to logR′ HK following Noyes et al. (1984), (24) Taylor (2006), (25) Paulson et al. (2002), (26) Upgren et al. (1985), (27) Reid (1992), (28) Weis & Upgren (1982),…...
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...We refer the reader to papers by Noyes et al. (1984); Baliunas et al. (1996, 1995); Henry et al. (1996); Wright et al. (2004, and references therein) for in-depth discussion of how to measure SMW and R′HK, as well as the history of studies using this index....
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...Chro- mospheric activity is generated through the stellar magnetic dynamo, the strength of which 1http://feps.as.arizona.edu appears to scale with rotation velocity (Kraft 1967; Noyes et al. 1984; Montesinos et al. 2001)....
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...The S-values from Duncan et al. (1991) were converted to R′HK following Noyes et al. (1984) using B−V colors from Perryman & ESA (1997)....
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...By “solar-type”, we mean ∼F7-K2 or 0.5 < (B − V )0 < 0.9 mag, which is approximately the color range over which the Noyes et al. (1984) relation for the photospheric contribution to the S-index is applicable, as well as the color range blanketed by recent activity surveys....
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...The value measured from our H′RHK and K lines is 24.93 as calibrated by Noyes et al. (1984)....
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"Rotation, convection, and magnetic ..." refers background or methods in this paper
...Finally, the period of the star HD 39587 is taken from the work of Stimets and Giles (1980), who extracted it from the long-term survey data of Wilson (1978)....
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...Such information may be obtainable from photometric and spectrophotometric (HK) rotational modulation light curves. Turning to the detailed dependence of tc on J3— V, we note that the empirical function tc (B—V) closely matches the theoretical convective overturn time for a ~ 2 (Fig. 5). As mentioned above, the scatter in plots of log (R'hk} versus P/t is slightly greater for a = 3 than for a = 2, and very much greater for a = 1. To the extent that the various assumptions made in the analysis are valid, this would suggest that a ~ 2 is a better description of convective envelopes of lower main sequence stars than a ~ 1 or (with somewhat less confidence) a ~ 3. A ratio of mixing length to scale height a ~ 2 implies a deeper convection zone than for the case a ~ 1 ; for the Sun, for example, the models of Gilman (1980) yield convection...
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...This would cause R'Hk to decrease correspondingly if it bears the same relation to period implied by Figure 8 for both fast and slow rotators, and therefore a gap would result in the distribution of chromospheric emission level. Hypothesis 3 is intriguing, but there is at present no independent evidence supporting such a period of rapid spindown. Soderblom (1983) concludes that the v sin i values...
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...Also, Hartmann et al (1984) have considered the statistical significance of the gap as outlined in the Vaughan and Preston (1980) neighborhood survey and find that it is not high, which favors hypothesis 1....
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...—The mean chromospheric H-K flux ratio as obtained from the mean Wilson (1978) survey data plotted in Fig....
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