Erratum: An investigation of the magnetic properties of the classical Be star ω Ori by the MiMeS Collaboration

Neiner, C.; Grunhut, J.; Petit, Véronique; ud‐Doula, Asif; Wade, G. A.; Landstreet, J. D.; Batz, B. de; Cochard, Francois; Gutiérrez‐Soto, J.; Huat, Anne-Laure

doi:10.1093/mnras/stt1554

Cited by 8 publications

(22 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In Fig. 4, the phase of minimum rotational light variation coincides with the minimum magnetic field strength and minimum UV spectral line equivalent width, as determined by Neiner et al (2012a). In B1, v and B there is also a double maximum, as in the UV line strength.…”

Section: V2052 Ophsupporting

confidence: 58%

“…4) in phase with the magnetic field and UV wind variations. This could be due to spots at the surface of the star (such as those suggested by Neiner et al 2012a) or magnetically confined clouds in the circumstellar environment (e.g. Townsend & Owocki 2005).…”

Section: V2052 Ophmentioning

confidence: 99%

“…the sum of the angles of the inclination of the rotation axis and the magnetic obliquity i + β must exceed 90 • . Neiner et al (2012a) determined i to be 53 • < i < 77 • from modelling Stokes profiles. This is consistent with the inclination of the rotation axis we obtained with a stellar radius corresponding to radial fundamental mode pulsation, but not with the value assuming that the radial mode is the first overtone.…”

Section: V2052 Ophmentioning

confidence: 99%

“…We therefore rule out the latter possibility. Using r = B min /B max = cos (i − β)/cos (i + β), where r is the ratio of the minimum and maximum magnetic field strength of the rotation cycle and the r values are determined by Neiner et al (2012a), we obtain 58 • < β < 66 • .…”

Section: V2052 Ophmentioning

confidence: 99%

“…Besides the detection of a second, non-radial, pulsation mode, these authors could derive an accurate rotation period of 3.638 833 ± 0.000 003 d. V2052 Oph also possesses a dipole magnetic field. Based on new data of superior quality, Neiner et al (2012a) determined that B pol ≈ 400 G, that the magnetic field is likely off-centred and that He patches are present close to the magnetic poles. Because of the presence of a radial pulsation mode (that allows the determination of the mean stellar density), and of the known rotation period that makes it spin about twice as fast as the most 'rapidly' rotating seismically well-studied β Cep star (12 Lac; Desmet et al 2009), it was deemed worthwhile to devote a large observational effort to V2052 Oph.…”

mentioning

confidence: 99%

See 4 more Smart Citations

A multisite photometric study of two unusual β Cep stars: the magnetic V2052 Oph and the massive rapid rotator V986 Oph

Handler

Shobbrook

Uytterhoeven³

et al. 2012

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We report a multisite photometric campaign for the β Cep stars V2052 Oph and V986 Oph. 670 h of high‐quality differential photoelectric Strömgren, Johnson and Geneva time‐series photometry was obtained with eight telescopes on five continents during 182 nights. Frequency analyses of the V2052 Oph data enabled the detection of three pulsation frequencies, the first harmonic of the strongest signal, and the rotation frequency with its first harmonic. Pulsational mode identification from analysing the colour amplitude ratios confirms the dominant mode as being radial, whereas the other two oscillations are most likely l = 4. Combining seismic constraints on the inclination of the rotation axis with published magnetic field analyses we conclude that the radial mode must be the fundamental mode. The rotational light modulation is in phase with published spectroscopic variability, and consistent with an oblique rotator for which both magnetic poles pass through the line of sight. The inclination of the rotation axis is 54° < i < 58° and the magnetic obliquity 58° < β < 66°. The possibility that V2052 Oph has a magnetically confined wind is discussed. The photometric amplitudes of the single oscillation of V986 Oph are most consistent with an l = 3 mode, but this identification is uncertain. Additional intrinsic, apparently temporally incoherent light variations of V986 Oph are reported. Different interpretations thereof cannot be distinguished at this point, but this kind of variability appears to be present in many OB stars. The prospects of obtaining asteroseismic information for more rapidly rotating β Cep stars, which appear to prefer modes of higher l, are briefly discussed.

show abstract

Section: V2052 Ophsupporting

confidence: 58%

Section: V2052 Ophmentioning

confidence: 99%

Section: V2052 Ophmentioning

confidence: 99%

Section: V2052 Ophmentioning

confidence: 99%

mentioning

confidence: 99%

See 3 more Smart Citations

A multisite photometric study of two unusual β Cep stars: the magnetic V2052 Oph and the massive rapid rotator V986 Oph

Handler

Shobbrook

Uytterhoeven³

et al. 2012

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

Blue supergiants as descendants of magnetic main sequence stars

Petermann

Langer

Castro

et al. 2015

A&A

View full text Add to dashboard Cite

About 10% of the massive main sequence stars have recently been found to host a strong, large scale magnetic field. Both, the origin and the evolutionary consequences of these fields are largely unknown. We argue that these fields may be sufficiently strong in the deep interior of the stars to suppress convection near the outer edge of their convective core. We performed parametrised stellar evolution calculations and assumed a reduced size of the convective core for stars in the mass range 16 M to 28 M from the zero age main sequence until core carbon depletion. We find that such models avoid the coolest part of the main sequence band, which is usually filled by evolutionary models that include convective core overshooting. Furthermore, our "magnetic" models populate the blue supergiant region during core helium burning, i.e., the post-main sequence gap left by ordinary single star models, and some of them end their life in a position near that of the progenitor of Supernova 1987A in the Hertzsprung-Russell diagram. Further effects include a strongly reduced luminosity during the red supergiant stage, and downward shift of the limiting initial mass for white dwarf and neutron star formation.

show abstract

Improved model of the triple system V746 Cassiopeiae that has a bipolar magnetic field associated with the tertiary

Harmanec

Brož

Mayer

et al. 2017

A&A

View full text Add to dashboard Cite

V746Cas is known to be a triple system composed of a close binary with an alternatively reported period of either 25 d .4 or 27 d .8 and a distant third component in a 170 yr (62000 d) orbit. The object was also reported to exhibit multiperiodic light variations with periods from 0 d .83 to 2 d .50, on the basis of which it was classified as a slowly pulsating B star. Interest in further investigation of this system was raised by the recent detection of a variable magnetic field. Analysing spectra from four instruments, earlier published radial velocities, and several sets of photometric observations, we arrived at the following conclusions: (1) The optical spectrum is dominated by the lines of the B-type primary (T eff 1 ∼ 16500(100) K), contributing 70 % of the light in the optical region, and a slightly cooler B tertiary (T eff 3 ∼ 13620(150) K). The lines of the low-mass secondary are below our detection threshold; we estimate that it could be a normal A or F star. (2) We resolved the ambiguity in the value of the inner binary period and arrived at a linear ephemeris of T super. conj. = HJD 2443838.78(81) + 25 d .41569(42) × E. (3) The intensity of the magnetic field undergoes a sinusoidal variation in phase with one of the known photometric periods, namely 2 d .503867(19), which we identify with the rotational period of the tertiary. (4) The second dominant photometric 1 d .0649524(40) period is tentatively identified with the rotational period of the broad-lined Btype primary, but this interpretation is much less certain and needs further verification. (5) If our interpretation of photometric periods is confirmed, the classification of the object as a slowly pulsating B star should be revised. (6) Applying an N-body model to different types of available observational data, we can constrain the orbital inclination of the inner orbit to ∼ 60 • < i 1 < 85 • even in the absence of binary eclipses, and we estimate the probable properties of the triple system and its components.

show abstract

Erratum: An investigation of the magnetic properties of the classical Be star ω Ori by the MiMeS Collaboration

Cited by 8 publications

References 1 publication

A multisite photometric study of two unusual β Cep stars: the magnetic V2052 Oph and the massive rapid rotator V986 Oph

A multisite photometric study of two unusual β Cep stars: the magnetic V2052 Oph and the massive rapid rotator V986 Oph

Blue supergiants as descendants of magnetic main sequence stars

Improved model of the triple system V746 Cassiopeiae that has a bipolar magnetic field associated with the tertiary

Contact Info

Product

Resources

About