2022A&A...657A..60S


Query : 2022A&A...657A..60S

2022A&A...657A..60S - Astronomy and Astrophysics, volume 657A, 60-60 (2022/1-1)

News from Gaia on σ Ori E: A case study for the wind magnetic braking process.

SONG H.F., MEYNET G., MAEDER A., MOWLAVI N., STROUD S.R., KESZTHELYI Z., EKSTROM S., EGGENBERGER P., GEORGY C., WADE G.A. and QIN Y.

Abstract (from CDS):


Context.σ Ori E, a massive helium B-type star, shows high surface rotation and a strong surface magnetic field, potentially challenging the process of wind magnetic braking.
Aims. The Gaia satellite provides an accurate distance to σ Ori E and confirms its membership to the σ Ori cluster. We account for these two key pieces of information in order to investigate whether single star models can reproduce the observed properties of σ Ori E and provide new estimates for its metallicity, mass, and age.
Methods. We computed rotating stellar models accounting for wind magnetic braking and magnetic quenching of the mass loss. We considered two metallicities (Z = 0.014, with a helium mass fraction Y = 0.273 and Z = 0.020 with Y = 0.266), four initial masses between 8 and 9 M, three initial rotations between 250 and 450 km/s, and three initial surface equatorial magnetic field between 3 and 7 kG. Differential rotation is assumed for the internal rotation in all models. We looked for models simultaneously accounting for the observed radius, position in the HR diagram, surface velocity, and braking timescale.
Results. We obtain that σ Ori E is a very young star (age less than 1 Myr) with an initial mass of around 9 M, a surface equatorial magnetic field of around 7 kG, and a metallicity Z (mass fraction of heavy elements) of around 0.020. No solution is obtained with the present models for a metallicity of Z = 0.014. The initial rotation of the models fitting σ Ori E is not highly constrained and could be anywhere in the range studied here. Because of its very young age, models predict no observable changes of the surface abundances due to rotational mixing.
Conclusions. The simultaneous high surface rotation and high surface magnetic field of σ Ori E may simply be a consequence of its young age. This young age implies that the processes responsible for producing the chemical inhomogeneities that are observed at its surface should be rapid. Therefore, for explaining the properties of σ Ori E, there is no necessity to invoke a merging event, although such a scenario cannot be discarded. Other stars (HR 5907, HR 7355, HR 345439, HD 2347, CPD -50°3509) showing similar properties to σ Ori E (fast rotation and strong surface magnetic field) may also be very young stars, although determination of the braking timescales is needed to confirm such a conclusion.

Abstract Copyright: © ESO 2022

Journal keyword(s): stars: chemically peculiar - stars: evolution - stars: magnetic field - stars: rotation

Simbad objects: 21

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Number of rows : 21
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 HD 2347 PM* 00 27 07.2052166352 -29 17 55.136759280   9.91 9.34     F7/8V 12 0
2 IC 348 OpC 03 44 32 +32 09.5           ~ 1334 1
3 HD 23478 Be* 03 46 40.8712236312 +32 17 24.675566784 6.17 6.708 6.671     B3IV 141 0
4 Ass Ori OB 1b As* 05 34.0 -01 30           ~ 257 0
5 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2207 1
6 Ass Ori OB 1c As* 05 35 21 -05 20.5           ~ 133 1
7 * sig Ori C Y*? 05 38 44.1189397296 -02 36 06.310060884   8.77 8.79   9.63 A2Vn 28 0
8 * sig Ori Y*O 05 38 44.7653828520 -02 36 00.283179888 2.54 3.58 3.79 3.87 4.11 O9.5V+B0.2V(n) 779 0
9 * sig Ori E Y*O 05 38 47.2050040320 -02 35 40.521424812 5.66 6.38 6.46 6.84 7.08 B2IV-Vp_He 441 0
10 HD 294297 * 05 40 27.5432293608 -02 25 43.161205152   10.7 10.117 10.01 9.77 G2: 29 0
11 V* V901 Ori Ro* 05 40 56.3704617744 -01 30 25.856677224 5.96 6.82 6.96     B2V 326 2
12 HD 91266 * 10 31 08.3187949992 -51 08 38.144365836   10.30 10.05     A2 5 0
13 CPD-57 3509 * 10 35 48.9972741480 -58 14 54.297364704 10.16 10.82 10.70 10.59 10.49 B2III 37 0
14 NGC 3293 OpC 10 35 53 -58 13.9           ~ 304 0
15 V* CU Vir a2* 14 12 15.8054758 +02 24 33.953395 4.46 4.90 5.02 5.10 5.23 ApSi 380 0
16 HD 142184 Be* 15 53 55.8637866220 -23 58 41.143370530 4.77 5.352 5.402     B2V 223 0
17 V* V913 Sco Ro* 15 58 34.8665694960 -24 49 53.361727284 4.70 5.34 5.43     B5V 198 0
18 NAME Upper Sco Association As* 16 12 -23.4           ~ 1252 1
19 * tau Sco * 16 35 52.9528530 -28 12 57.661515 1.55 2.56 2.81 2.93 3.18 B0.2V 901 0
20 HD 182180 * 19 24 30.1801035096 -27 51 57.389455476 5.22 5.889 6.011     B2Vnn 111 0
21 HD 345439 Be* 19 58 48.4896519480 +23 05 21.559730172   11.61 11.11 11.37   B1V-B2V 29 0

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2023.01.31-01:03:01

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