Rotational mixing in Magellanic clouds B stars : theory versus observation

I. Brott; I. Hunter; A. de Koter; N. Langer; D.J. Lennon; P.L. Dufton

Rotational mixing in Magellanic clouds B stars : theory versus observation

I. Brott, I. Hunter, A. de Koter, N. Langer, D.J. Lennon, P.L. Dufton

extern

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › Academic

Abstract

We have used VLT FLAMES data to constrain the physics of rotational mixing in stellar evolution models. We have simulated a population of single stars and found two groups of observed stars that cannot be explained: (1) a group of fast rotating stars which do not show evidence for rotational mixing and (2) a group of slow rotators with strong N enrichment. Binary effects and fossil magnetic fields may be considered to explain those two groups. We suggest that the element boron could be used to distinguish between rotational mixing and the binary scenario. Our single star population simulations quantify the expected amount of boron in fast and slow rotators and allow a comparison with measured nitrogen and boron abundances in B-stars.

Original language	Undefined/Unknown
Title of host publication	Evolution and pulsation of massive stars on the main sequence and close to it
Editors	A. Noels
Place of Publication	Vienna
Publisher	Austrian Academy of Sciences Press
Pages	55-60
Number of pages	6
Publication status	Published - 7 Jul 2008

Cite this

@inproceedings{ce8867e5ac7343fca4c674a12fce150f,

title = "Rotational mixing in Magellanic clouds B stars : theory versus observation",

abstract = "We have used VLT FLAMES data to constrain the physics of rotational mixing in stellar evolution models. We have simulated a population of single stars and found two groups of observed stars that cannot be explained: (1) a group of fast rotating stars which do not show evidence for rotational mixing and (2) a group of slow rotators with strong N enrichment. Binary effects and fossil magnetic fields may be considered to explain those two groups. We suggest that the element boron could be used to distinguish between rotational mixing and the binary scenario. Our single star population simulations quantify the expected amount of boron in fast and slow rotators and allow a comparison with measured nitrogen and boron abundances in B-stars.",

author = "I. Brott and I. Hunter and {de Koter}, A. and N. Langer and D.J. Lennon and P.L. Dufton",

note = "Communications in Asteroseismology, vol. 158 [Niet in lijst!!!] AAMAS",

year = "2008",

month = jul,

day = "7",

language = "Undefined/Unknown",

pages = "55--60",

editor = "A. Noels",

booktitle = "Evolution and pulsation of massive stars on the main sequence and close to it",

publisher = "Austrian Academy of Sciences Press",

}

Rotational mixing in Magellanic clouds B stars : theory versus observation. / Brott, I.; Hunter, I.; de Koter, A. et al.
Evolution and pulsation of massive stars on the main sequence and close to it. ed. / A. Noels. Vienna: Austrian Academy of Sciences Press, 2008. p. 55-60.

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution › Academic

TY - GEN

T1 - Rotational mixing in Magellanic clouds B stars : theory versus observation

AU - Brott, I.

AU - Hunter, I.

AU - de Koter, A.

AU - Langer, N.

AU - Lennon, D.J.

AU - Dufton, P.L.

N1 - Communications in Asteroseismology, vol. 158 [Niet in lijst!!!] AAMAS

PY - 2008/7/7

Y1 - 2008/7/7

N2 - We have used VLT FLAMES data to constrain the physics of rotational mixing in stellar evolution models. We have simulated a population of single stars and found two groups of observed stars that cannot be explained: (1) a group of fast rotating stars which do not show evidence for rotational mixing and (2) a group of slow rotators with strong N enrichment. Binary effects and fossil magnetic fields may be considered to explain those two groups. We suggest that the element boron could be used to distinguish between rotational mixing and the binary scenario. Our single star population simulations quantify the expected amount of boron in fast and slow rotators and allow a comparison with measured nitrogen and boron abundances in B-stars.

AB - We have used VLT FLAMES data to constrain the physics of rotational mixing in stellar evolution models. We have simulated a population of single stars and found two groups of observed stars that cannot be explained: (1) a group of fast rotating stars which do not show evidence for rotational mixing and (2) a group of slow rotators with strong N enrichment. Binary effects and fossil magnetic fields may be considered to explain those two groups. We suggest that the element boron could be used to distinguish between rotational mixing and the binary scenario. Our single star population simulations quantify the expected amount of boron in fast and slow rotators and allow a comparison with measured nitrogen and boron abundances in B-stars.

M3 - Conference contribution

SP - 55

EP - 60

BT - Evolution and pulsation of massive stars on the main sequence and close to it

A2 - Noels, A.

PB - Austrian Academy of Sciences Press

CY - Vienna

ER -