The magnetic field and wind confinement of θ1 Orionis C

By J. Donati, J. Babel, Tim Harries, I. Howarth, P. Petit, M. Semel. 2002

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View Paper: https://www.semanticscholar.org/paper/1ed22924715e44697a0d9d32b74c0049f0f767e7

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In Astronomy and Astrophysics

Citations in the corpus

Chandra HETGS Multiphase Spectroscopy of the Young Magnetic O Star θ1 Orionis C (2005, methodology): “Donati et al. (2002) estimate its orbital period to be 8–16 yr and Schertl et al. (2003) estimate its spectral type as B0-A0.”
Toward Understanding Massive Star Formation (2007, background): “…there are by now at least two cases where strong kilo-Gauss stellar magnetic fields have been inferred from Zeeman spectro-polarimetry, including the oblique magnetic rotator θ1 Ori C (Stahl et al. 1996, Donati et al. 2002) and the Of?p star HD 191612 (Walborn et al. 2003, Donati et al. 2006).”
The MiMeS survey of Magnetism in Massive Stars : magnetic analysis of the O-type stars (2016, background): “Within the context of the MiMeS project, HD191612 was re-observed and found to show Bℓ variations from about −600 to 100G. Similarly to θ1 OriC, the field is welldescribed by a dipole, with a polar field strength of about 2.5 kG, with a magnetic axis oblique to the rotation axis by about 70◦.”
The Magnetar Model for Type I Superluminous Supernovae. I. Bayesian Analysis of the Full Multicolor Light-curve Sample with MOSFiT (2017, background): “Such fields have been measured for a small number of Galactic O stars (Donati et al. 2002, 2006).”
A rigidly rotating magnetosphere model for circumstellar emission from magnetic OB stars (2004, background): “More recently, more moderate magnetic fields have been detected in Be emission-line stars (e.g., β Cep – Henrichs et al. 2000), slowly-pulsating B stars (e.g., ζ Cas – Neiner et al. 2003), and O-type stars (e.g., θ1 Ori C – Donati et al. 2002).”
Dynamical Simulations of Magnetically Channeled Line-driven Stellar Winds. I. Isothermal, Nonrotating, Radially Driven Flow (2002, background): “This is a typical value for known magnetic massive stars, as inferred from Stokes V measurement of photospheric lines with circular polarization by the Zeeman effect (see, e.g., Donati et al. 2002).”
X-ray spectroscopy of stars (2009, background): “References: (1) Rauw et al (2002a), (2) Hubrig et al (2008), (3 Nazé et al (2008b,c), (4) Donati et al (2002), Gagné et al(2005b), (5) Donati et al (2006a), Nazé et al (2007b, 2008b), Howarth et al (2007), (6) Hubrig et al (2008), Prinja et al (1990), Vilkoviskii and Tambovtseva (1992), (7)…”
The surprising magnetic topology of τ Sco: fossil remnant or dynamo output? (2006, unknown): “5). are detected in a star like τ Sco, known for its peculiar spectroscopic morphology (e.g., through its abnormally strong UV P-Cygni lines and its unusually hard X-ray emission), after having been detected in other peculiar hot stars (like θ 1 Ori C, HD 191612 and β Cep), represents further eviden”
Magnetic Fields of Nondegenerate Stars (2009, methodology): “…detections have been obtained sofar, 6 in early B stars (namelyβ Cep,ζ Cas,τ Sco,ξ1 CMa, Par 1772ν Ori, e.g., Henrichs et al. 2000; Neiner et al. 2003; Donati et al. 2006c; Petit et al. 2008b) and 3 in O stars (namelyθ1 Ori C, HD 191612 and ζ Ori A, Donati et al. 2002, 2006b; Bouret et al. 2008).”
O stars with weak winds: the Galactic case (2005, background): “Indeed, the only O stars with a detected magnetic field - Theta1 Ori C (Donati et al. 2002) - shows unusual features which may be related to the geometry of magnetically confined wind (Walborn et al. 1985, Gagné et al., 2005).”
Presupernova Evolution of Differentially Rotating Massive Stars Including Magnetic Fields (2004, background): “To the extent that such magnetic fields also exist in massive MS stars (where they are much harder to detect, see however Donati et al. 2002), they are likely to have led to a stronger magnetic coupling between core and envelope, and hence to more slowly rotating pre-SN cores.”