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A Stellar Rotation Census of B Stars: from ZAMS to TAMS

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Title: A Stellar Rotation Census of B Stars: from ZAMS to TAMS
Authors: Huang, Wenjin, Gies, Douglas R., McSwain, M. Virginia
Publication Year: 2010
Collection: Astrophysics
Subject Terms: Astrophysics - Solar and Stellar Astrophysics
More Details: Two recent observing campaigns provide us with moderate dispersion spectra of more than 230 cluster and 370 field B stars. Combining them and the spectra of the B stars from our previous investigations ($\sim$430 cluster and $\sim$100 field B stars) yields a large, homogeneous sample for studying the rotational properties of B stars. We derive the projected rotational velocity $V\sin i$, effective temperature, gravity, mass, and critical rotation speed $V_{\rm crit}$ for each star. We find that the average $V\sin i$ is significantly lower among field stars because they are systematically more evolved and spun down than their cluster counterparts. The rotational distribution functions of $V_{\rm eq}/V_{\rm crit}$ for the least evolved B stars show that lower mass B stars are born with a larger proportion of rapid rotators than higher mass B stars. However, the upper limit of $V_{\rm eq}/V_{\rm crit}$ that may separate normal B stars from emission line Be stars (where rotation promotes mass loss into a circumstellar disk) is smaller among the higher mass B stars. We compare the evolutionary trends of rotation (measured according to the polar gravity of the star) with recent models that treat internal mixing. The spin-down rates observed in the high mass subset ($\sim 9 M_\odot$) agree with predictions, but the rates are larger for the low mass group ($\sim 3 M_\odot$). The faster spin down in the low mass B stars matches well with the predictions based on conservation of angular momentum in individual spherical shells. Our results suggest the fastest rotators (that probably correspond to the emission line Be stars) are probably formed by evolutionary spin up (for the more massive stars) and by mass transfer in binaries (for the full range of B star masses).
Comment: 44 pages, 10 figures, accepted for publication in ApJ
Document Type: Working Paper
DOI: 10.1088/0004-637X/722/1/605
Access URL: http://arxiv.org/abs/1008.1761
Accession Number: edsarx.1008.1761
Database: arXiv
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  Data: A Stellar Rotation Census of B Stars: from ZAMS to TAMS
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  Data: <searchLink fieldCode="AR" term="%22Huang%2C+Wenjin%22">Huang, Wenjin</searchLink><br /><searchLink fieldCode="AR" term="%22Gies%2C+Douglas+R%2E%22">Gies, Douglas R.</searchLink><br /><searchLink fieldCode="AR" term="%22McSwain%2C+M%2E+Virginia%22">McSwain, M. Virginia</searchLink>
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  Data: 2010
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  Data: Two recent observing campaigns provide us with moderate dispersion spectra of more than 230 cluster and 370 field B stars. Combining them and the spectra of the B stars from our previous investigations ($\sim$430 cluster and $\sim$100 field B stars) yields a large, homogeneous sample for studying the rotational properties of B stars. We derive the projected rotational velocity $V\sin i$, effective temperature, gravity, mass, and critical rotation speed $V_{\rm crit}$ for each star. We find that the average $V\sin i$ is significantly lower among field stars because they are systematically more evolved and spun down than their cluster counterparts. The rotational distribution functions of $V_{\rm eq}/V_{\rm crit}$ for the least evolved B stars show that lower mass B stars are born with a larger proportion of rapid rotators than higher mass B stars. However, the upper limit of $V_{\rm eq}/V_{\rm crit}$ that may separate normal B stars from emission line Be stars (where rotation promotes mass loss into a circumstellar disk) is smaller among the higher mass B stars. We compare the evolutionary trends of rotation (measured according to the polar gravity of the star) with recent models that treat internal mixing. The spin-down rates observed in the high mass subset ($\sim 9 M_\odot$) agree with predictions, but the rates are larger for the low mass group ($\sim 3 M_\odot$). The faster spin down in the low mass B stars matches well with the predictions based on conservation of angular momentum in individual spherical shells. Our results suggest the fastest rotators (that probably correspond to the emission line Be stars) are probably formed by evolutionary spin up (for the more massive stars) and by mass transfer in binaries (for the full range of B star masses).<br />Comment: 44 pages, 10 figures, accepted for publication in ApJ
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        Value: 10.1088/0004-637X/722/1/605
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      – SubjectFull: Astrophysics - Solar and Stellar Astrophysics
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      – TitleFull: A Stellar Rotation Census of B Stars: from ZAMS to TAMS
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