Tomographic Separation of Composite Spectra. XI. The Physical Properties of the Massive Close Binary HD 100213 (TU Muscae)

Penny, Laura R.; Ouzts, C.; Gies, Douglas R.

doi:10.1086/587509

Cited by 18 publications

(22 citation statements)

References 38 publications

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“…Radiation from the hot component of a symbiotic binary could ionize the nearby interstellar medium, so producing interstellar absorption from highly ionized atoms, without such lines being seen in the spectra of other stars in similar lines of sight. The estimated distance of SY Mus is 850 pc according to Schmutz et al (1994), while TU Mus, a β Lyr type eclipsing variable with a O star component, has a distance of 2.1 kpc according to Penny et al (2008) and is only 0.3 • in the sky from SY Mus. The stronger N v 1238 Å doublet resonance line absorption of TU Mus is weak as is also the stronger Si iv 1393 Å doublet resonance line.…”

Section: Discussionmentioning

confidence: 99%

UV emission line shifts of symbiotic binaries

Friedjung¹,

Mikołajewska²,

Zajczyk³

et al. 2010

A&A

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Aims. Relative and absolute emission line shifts have been previously found for symbiotic binaries, but their cause was not clear. This work aims to better understand the emission line shifts. Methods. Positions of strong emission lines were measured on archival UV spectra of Z And, AG Dra, RW Hya, SY Mus and AX Per and relative shifts between the lines of different ions compared. Profiles of lines of RW Hya and Z And were also examined.Results. The reality of the relative shift between resonance and intercombination lines of several times ionised atoms was clearly shown except for AG Dra. This redshift shows a well defined variation with orbital phase for Z And and RW Hya. In addition the intercombination lines from more ionised atoms and especially O iv are redshifted with respect to those from less ionised atoms.Other effects are seen in the profiles. Conclusions. The resonance-intercombination line shift variation can be explained in quiescence by P Cygni shorter wavelength component absorption, due to the wind of the cool component, which is specially strong in inferior conjunction of this cool giant. The velocity stratification permits absorption of line emission. The relative intercombination line shifts may be connected with varying occultation of line emission near an accretion disk, which is optically thick in the continuum.

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Section: Discussionmentioning

confidence: 99%

UV emission line shifts of symbiotic binaries

Friedjung¹,

Mikołajewska²,

Zajczyk³

et al. 2010

A&A

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“…Mutual irradiation of the stars in this very short-period system leads to the observation of line strength variations along the orbit (Linder et al 2007;. The eclipses of the system indicate that the stars are in contact while the masses derived from the orbital solution are lower than expected from evolutionary models, suggesting a past episode of mass-transfer (Linder et al 2007;Qian et al 2007;Penny et al 2008, and references therein).…”

Section: The Samplementioning

confidence: 82%

“…Gies (2003) provided lists of well-studied double-lined spectroscopic (SB2) binary systems located in the Galaxy and the Magellanic Clouds, among which he separately listed unevolved cases (his Table 1) and evolved cases (his Table 2), the latter ones being subdivided between systems before contact, in contact, and after mass transfer. Penny et al (2008) also listed binaries in which one star fills its Roche lobe, complementing the list. Eliminating the complex high-multiplicity systems δ Ori and Cyg OB2 5, which could blur the picture, while adding HD 149404 and LSS 3074, two other post-Roche Lobe Overflow (RLOF) systems not listed in these references but whose interactions were recently analyzed (see details below), we ended up with 15 relatively bright targets:…”

Section: The Samplementioning

confidence: 99%

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How unique is Plaskett’s star? A search for organized magnetic fields in short period, interacting or post-interaction massive binary systems

Nazé

Neiner

Grunhut

et al. 2017

Mon. Not. R. Astron. Soc.

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Amongst O-type stars with detected magnetic fields, the fast rotator in the close binary called Plaskett's star shows a variety of unusual properties. Since strong binary interactions are believed to have occurred in this system, one may wonder about their potential role in generating magnetic fields. Stokes V spectra collected with the low-resolution FORS2 and high-resolution ESPaDOnS and Narval spectropolarimeters were therefore used to search for magnetic fields in 15 interacting or post-interaction massive binaries. No magnetic field was detected in any of them, with 0 G always being within 2σ of the derived values. For 17 out of 25 stars in the systems observed at high-resolution, the 90% upper limit on the individual dipolar fields is below the dipolar field strength of Plaskett's secondary; a similar result is found for five out of six systems observed at low resolution. If our sample is considered to form a group of stars sharing similar magnetic properties, a global statistical analysis results in a stringent upper limit of ∼ 200 G on the dipolar field strength. Moreover, the magnetic incidence rate in the full sample of interacting or post-interaction systems (our targets + Plaskett's star) is compatible with that measured from large surveys, showing that they are not significantly different from the general O-star population. These results suggest that binary interactions play no systematic role in the magnetism of such massive systems.

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“…Some semi-detached systems with short periods are believed to be post-contact binaries, whose orbital periods increase after a minimum is reached during fast case A mass transfer. Examples of this are TU Mus (P orb = 1.4 d, O7 V+O8 V; Penny et al 2008), or IU Aur 5 (P orb = 1.8 d, O9.5 V+B0.5 V; Özdemir et al 2003). In these cases, the contact phase should be short lived (Qian et al 2013, and references therein).…”

Section: Discussionmentioning

confidence: 99%

GU Monocerotis: A high-mass eclipsing overcontact binary in the young open cluster Dolidze 25

Lorenzo

Negueruela

Vilardell

et al. 2016

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Context. The eclipsing binary GU Mon is located in the star-forming cluster Dolidze 25, which has the lowest metallicity measured in a Milky Way young cluster. Aims. GU Mon has been identified as a short-period eclipsing binary with two early B-type components. We set out to derive its orbital and stellar parameters. Methods. We present a comprehensive analysis, including B and V light curves and 11 high-resolution spectra, to verify the orbital period and determine parameters. We used the stellar atmosphere code FASTWIND to obtain stellar parameters and create templates for cross-correlation. We obtained a model to fit the light and radial-velocity curves using the Wilson-Devinney code iteratively and simultaneously.Results. The two components of GU Mon are identical stars of spectral type B1 V with the same mass and temperature. The light curves are typical of an EW-type binary. The spectroscopic and photometric analyses agree on a period of 0.896640 ± 0.000007 d. We determine a mass of 9.0 ± 0.6 M for each component and for temperatures of 28 000 ± 2000 K. Both values are consistent with the spectral type. The two stars are overfilling their respective Roche lobes, sharing a common envelope and, therefore the orbit is synchronised and circularised. Conclusions. The GU Mon system has a fill-out factor above 0.8, containing two dwarf B-type stars on the main sequence. The two stars are in a very advanced stage of interaction, with their extreme physical similarity likely due to the common envelope. The expected evolution of such a system very probably leads to a merger while still on the main sequence.

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Tomographic Separation of Composite Spectra. XI. The Physical Properties of the Massive Close Binary HD 100213 (TU Muscae)

Cited by 18 publications

References 38 publications

UV emission line shifts of symbiotic binaries

UV emission line shifts of symbiotic binaries

How unique is Plaskett’s star? A search for organized magnetic fields in short period, interacting or post-interaction massive binary systems

GU Monocerotis: A high-mass eclipsing overcontact binary in the young open cluster Dolidze 25

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