Stellar Rotation and be Stars in the H and χ Persei Association

Slettebak, Arne

doi:10.1086/149814

Cited by 35 publications

(24 citation statements)

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“…These numbers show that our sample is biased toward earlier subtypes ( luminosity biased). The distribution of V sin i for cluster stars is basically flat over this range, and appears similar to the classical diagram for nearby B-type stars presented by Slettebak (1970). There is a slight indication that there are more fast rotators among the late-B subtypes (B5-B8), which is similar to what Brown & Verschueren (1997) found for stars in Sco OB2 and to what Abt et al (2002) found for nearby field stars.…”

Section: Resultssupporting

confidence: 84%

“…We found V sin i measurements in the WEBDA database on open clusters (Mermilliod & Paunzen 2003) for 69 stars in common with our sample (Slettebak 1965(Slettebak , 1968(Slettebak , 1985Hill 1967;Balona 1975a;Dworetsky 1975;Wolff 1981;Arnal et al 1988;Verschueren 1991;Penny 1996;Mathys et al 2002). Some 90% of these published V sin i values were obtained by simple visual estimates or by measuring line widths, but Mathys et al (2002) measured V sin i in six stellar spectra using line-profile fitting and a simple convolution scheme for rotational broadening.…”

Section: Measuring Projected Rotational Velocitiesmentioning

confidence: 89%

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Stellar Rotation in Young Clusters. I. Evolution of Projected Rotational Velocity Distributions

Huang

Gies

2006

ApJ

144

172

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Open clusters offer us the means to study stellar properties in samples with well-defined ages and initial chemical composition. Here we present a survey of projected rotational velocities for a large sample of mainly B-type stars in young clusters to study the time evolution of the rotational properties of massive stars. The survey is based on moderate-resolution spectra made with the WIYN 3.5 m and CTIO 4 m telescopes and Hydra multi-object spectrographs, and the target stars are members of 19 young open clusters with an age range of approximately 6-73 Myr. We made fits of the observed lines He i kk4026, 4387, 4471, and Mg ii k4481, using model theoretical profiles to find projected rotational velocities for a total of 496 OB stars. We find that there are fewer slow rotators among the cluster B-type stars relative to nearby B stars in the field. We present evidence consistent with the idea that the more massive B stars (M > 9 M ) spin down during their main-sequence phase. However, we also find that the rotational velocity distribution appears to show an increase in the numbers of rapid rotators among clusters with ages of 10 Myr and higher. These rapid rotators appear to be distributed between the zero age and terminal age main-sequence locations in the Hertzsprung-Russell diagram, and thus only a minority of them can be explained as the result of a spin-up at the terminal age main sequence due to core contraction. We suggest instead that some of these rapid rotators may have been spun up through mass transfer in close binary systems. Subject headingg s: line: profiles -open clusters and associations: individual

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Section: Resultssupporting

confidence: 84%

Section: Measuring Projected Rotational Velocitiesmentioning

confidence: 89%

Stellar Rotation in Young Clusters. I. Evolution of Projected Rotational Velocity Distributions

Huang

Gies

2006

ApJ

144

172

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“…The colourmagnitude diagram of the double cluster shows an important scatter (see Figure 1). It has long been known that h and χ Persei are extremely rich in Be stars (Slettebak 1968). Our previous contention (Waelkens et al 1990) that the large-amplitude variable stars we discovered are also Be stars, could be confirmed for a few objects.…”

Section: Introductionsupporting

confidence: 66%

“…This effect would imply blueward evolution. Rotation velocities for stars in h and χ Persei have been obtained by Slettebak (1968Slettebak ( , 1985. We have also determined υ sin i values for several cluster members, using the high-resolution spectrograph Aurélie of the Observatoire de Haute-Provence.…”

Section: Rotation and Main-sequence Broadeningmentioning

confidence: 99%

Main-sequence broadening, Be stars, and stellar rotation inhand χ Persei

Denoyelle

Aerts

Waelkens

1994

Symp. - Int. Astron. Union

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The double cluster h andxPersei is one of the richest clusters containing early-B stars, and therefore is important for observational and theoretical studies on the fundamental parameters of massive stars. The colour-magnitude diagram of the double cluster shows an important scatter (see Figure 1). It has long been known thathandxPersei are extremely rich in Be stars (Slettebak 1968). Our previous contention (Waelkens et al. 1990) that the large-amplitude variable stars we discovered are also Be stars, could be confirmed for a few objects. Rotation velocities for stars inhandxPersei are usually high, which is not surprising in view of the large fraction of Be stars.

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“…The list of standard stars used can be found in Table 2, along with their standard values used for the transformation, taken from and Johnson & Morgan (1955) for h and s Persei, Perry, Lee, & Barnes (1978) for NGC 2169, Crawford, Barnes, & Hill (1977) for NGC 6910, and Canterna, Perry, & Crawford (1979) for NGC 1039. Spectral types, when available, have been taken from Schild (1965) and Slettebak (1968) for h and s Persei, Perry et al (1978) for NGC 2169, Morgan & Harris (1956) and Applequist (1965) for NGC 6910, andCanterna et al (1979) for NGC 1039.…”

Section: èèèèèèèèèèèèèèèmentioning

confidence: 99%

Photometric and Spectroscopic Study of the Young Open Cluster NGC 1893

Marco

Bernabeu

Negueruela

2001

The Astronomical Journal

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We present uvbyb CCD photometry of the Ðeld of the open cluster NGC 1893. Our photometry is deep enough to cover the complete main-sequence B spectral type. We identify D50 very likely members of the cluster down to spectral type B9ÈA0, some of which have much higher reddenings than the average. We derive a color excess E(b[y) \ 0.33^0.03 and a dereddened distance modulus V 0 [M V \ 13.9^0.2. From the b index, we identify several candidates as emission-line stars, for which we have obtained spectroscopy. Three of them display spectra corresponding to spectral type F but showing Ha in emission. Photometric measurements in this and previous studies indicate strong variability. These characteristics show them to be preÈmain-sequence stars of spectral type F. We also identify two likely Herbig Be stars. These results hint at the existence of a sizable preÈmain-sequence population in NGC 1893.

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Stellar Rotation and be Stars in the H and χ Persei Association

Cited by 35 publications

References 0 publications

Stellar Rotation in Young Clusters. I. Evolution of Projected Rotational Velocity Distributions

Stellar Rotation in Young Clusters. I. Evolution of Projected Rotational Velocity Distributions

Main-sequence broadening, Be stars, and stellar rotation inhand χ Persei

Photometric and Spectroscopic Study of the Young Open Cluster NGC 1893

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