Universität zu Köln

Shultz, M., Le Bouquin, J. -B., Rivinius, Th., Wade, G. A., Kochukhov, O., Alecian, E., Petit, V., Pfuhl, O., Karl, M., Gao, F., Grellmann, R., Lin, C. -C., Garcia, P. and Lacour, S. (2019). NU Ori: a hierarchical triple system with a strongly magnetic B-type star. Mon. Not. Roy. Astron. Soc., 482 (3). S. 3950 - 3966. OXFORD: OXFORD UNIV PRESS. ISSN 1365-2966

Full text not available from this repository.

Abstract

NU Ori is a massive spectroscopic and visual binary in the Orion Nebula Cluster, with four components: Aa, Ab, B, and C. The B0.5 primary (Aa) is one of the most massive B-type stars reported to host a magnetic field. We report the detection of a spectroscopic contribution from the C component in high-resolution ESPaDOnS spectra, which is also detected in a Very Large Telescope Interferometer data set. Radial velocity (RV) measurements of the inner binary (designated Aab) yield an orbital period of 14.3027(7) d. The orbit of the third component (designated C) was constrained using both RVs and interferometry. We find C to be on a mildly eccentric 476(1) d orbit. Thanks to spectral disentangling of mean line profiles obtained via least-squares deconvolution, we show that the Zeeman Stokes V signature is clearly associated with C, rather than Aa as previously assumed. The physical parameters of the stars were constrained using both orbital and evolutionary models, yielding M-Aa = 14.9 +/- 0.5 M-circle dot, M-Ab = 3.9 +/- 0.7 M-circle dot, and M-C = 7.8 +/- 0.7 M-circle dot. The rotational period obtained from longitudinal magnetic field (B-z) measurements is P-rot = 1.09468(7)d, consistent with previous results. Modelling of (B-z) indicates a surface dipole magnetic field strength of similar to 8 kG. NU Ori C has a magnetic field strength, rotational velocity, and luminosity similar to many other stars exhibiting magnetospheric Ha emission, and we find marginal evidence of emission at the expected level (similar to 1 per cent of the continuum).

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Shultz, M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Le Bouquin, J. -B. UNSPECIFIED UNSPECIFIED UNSPECIFIED Rivinius, Th. UNSPECIFIED UNSPECIFIED UNSPECIFIED Wade, G. A. UNSPECIFIED UNSPECIFIED UNSPECIFIED Kochukhov, O. UNSPECIFIED UNSPECIFIED UNSPECIFIED Alecian, E. UNSPECIFIED UNSPECIFIED UNSPECIFIED Petit, V. UNSPECIFIED UNSPECIFIED UNSPECIFIED Pfuhl, O. UNSPECIFIED UNSPECIFIED UNSPECIFIED Karl, M. UNSPECIFIED UNSPECIFIED UNSPECIFIED Gao, F. UNSPECIFIED UNSPECIFIED UNSPECIFIED Grellmann, R. UNSPECIFIED UNSPECIFIED UNSPECIFIED Lin, C. -C. UNSPECIFIED UNSPECIFIED UNSPECIFIED Garcia, P. UNSPECIFIED UNSPECIFIED UNSPECIFIED Lacour, S. UNSPECIFIED UNSPECIFIED UNSPECIFIED
URN:	urn:nbn:de:hbz:38-139328
DOI:	10.1093/mnras/sty2985
Journal or Publication Title:	Mon. Not. Roy. Astron. Soc.
Volume:	482
Number:	3
Page Range:	S. 3950 - 3966
Date:	2019
Publisher:	OXFORD UNIV PRESS
Place of Publication:	OXFORD
ISSN:	1365-2966
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language ROTATING MAGNETOSPHERE MODEL; DRIVEN STELLAR WINDS; X-RAY-EMISSION; MASSIVE STARS; SPECTROSCOPIC BINARIES; DYNAMICAL SIMULATIONS; NEBULA CLUSTER; MIMES SURVEY; FIELD; AXES Multiple languages Astronomy & Astrophysics Multiple languages
Refereed:	Yes
URI:	http://kups.ub.uni-koeln.de/id/eprint/13932