The eclipsing double-lined binaries V883 Cen and   Mus

Hensberge, H.; Nitschelm, Christian; Olsen, E. H.; Sterken, C.; David, M.; Freyhammer, L. M.; Landin, N. R.; Bouzid, Maroua; Papadaki, C.; Pritchard, J. D.; Clausen, J. V.; Vaz, L. P. R.

doi:10.1111/j.1365-2966.2007.11955.x

Cited by 7 publications

(11 citation statements)

References 18 publications

(26 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…they were all within their probable errors), also with the Hipparcos light curve. We also found a small shift to the zero point of the phases (0.0040) calculated from the ephemeris of Hensberge et al (2007). Bakış et al (2007) noted, from the high dispersion spectroscopy, a greater apparent rotation speed of the secondary than the primary (see also Section 3.1).…”

Section: Photometric Analysissupporting

confidence: 68%

“…Starting from such preliminaries, ILOT type analysis was applied to the more extensive uvby photometry, kindly supplied by Dr H. Hensberge (Hensberge et al 2007; Figure 2). The essentially unity value of the spectroscopic mass ratio found below was used.…”

Section: Light Curves Of Hensberge Et Almentioning

confidence: 99%

“…The relatively small proximity effects are evaluated as described in the curvefit manual of Rhodes (2008) corresponding to the assigned effective temperatures and uvby filter wavelengths. Hensberge et al (2007) also referred to photometry during the interval [1983][1984][1985][1986][1987][1988][1989][1990], their analysis of which resulted in a refined period of 2.396320 d. We will discuss this in Section 5.…”

Section: Light Curves Of Hensberge Et Almentioning

confidence: 99%

“…Bakış et al (2007) noted, from the high dispersion spectroscopy, a greater apparent rotation speed of the secondary than the primary (see also Section 3.1).

Figure 2. Light-curve fittings applied to the uvby photometry of η Mus, as presented by Hensberge et al (2007). The relative fluxes are shown against phase with each curve vertically displaced by a linear displacement of 0.2.…”

Section: Photometric Analysismentioning

confidence: 99%

See 3 more Smart Citations

The Multiple Star η Muscae

Budding

Butland

Blackford³

2013

Publ. Astron. Soc. Aust.

View full text Add to dashboard Cite

High-resolution spectroscopy of η Mus is combined with literature and new photometry to provide a comprehensive analysis of its components. Our main absolute parameters for the close binary system are M 1 and M 2 3.34 ± 0.04 M ࣻ , R 1 2.13 ± 0.07 R ࣻ , R 2 2.34 ± 0.10 R ࣻ ; T 1 13 000 ± 300, T 2 12 600 ± 300, K; and distance 125 ± 10 pc. Our findings update earlier results in a number of respects. We thus confirm that η Mus B is a gravitationally bound companion of the close binary. This relates to the variable γ velocity of the radial velocities of η Mus A. We connect this to the recently discovered member η Mus D, whose orbit we link to new data. We also provide a spectroscopic examination of the Ap star η Mus B, listing over 450 identified lines. We argue that the system is still young, and the apparently anomalous rotation of the close binary's secondary can be reconciled with its being a physically larger star, still condensing to the zero-age main sequence. Models of young condensing stars permit such expanded states, particularly during the deuterium-burning stage, and our results are in agreement with appropriate low-age models. This possible configuration may make η Mus an important example for testing young star models, formation, and evolution scenarios. This multiple star can be compared with V831 Cen and the general properties related to its membership of the Sco-Cen OB2 association.

show abstract

Section: Photometric Analysissupporting

confidence: 68%

Section: Light Curves Of Hensberge Et Almentioning

confidence: 99%

Section: Light Curves Of Hensberge Et Almentioning

confidence: 99%

“…Bakış et al (2007) noted, from the high dispersion spectroscopy, a greater apparent rotation speed of the secondary than the primary (see also Section 3.1).

Section: Photometric Analysismentioning

confidence: 99%

See 2 more Smart Citations

The Multiple Star η Muscae

Budding

Butland

Blackford³

2013

Publ. Astron. Soc. Aust.

View full text Add to dashboard Cite

show abstract

“…7, the normalized flux level around the Mg ii line is below the continuum level, which suggests an extra absorption line of a fast‐rotating additional star. This was also noted by Hensberge et al (2007) in their spectra; however, a detailed analysis is deferred to a future publication. It is desirable to analyse all available sets of spectra together, using spectral disentangling techniques, in order to confirm or exclude the presence of an additional component.…”

Section: Model Atmosphere Applicationssupporting

confidence: 54%

Muscae: a young detached binary with two identical components

Bakış

Bakıș

Eker

et al. 2007

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

High-resolution (λ/dλ ∼ 41 000) echelle spectra of the multiple system η Muscae were analysed. Precise spectroscopic orbital elements of the close pair η Muscae-A were obtained by means of two techniques; cross-correlation and spectral disentangling. The updated light elements of the close pair were derived using new photometric and spectroscopic data together with Hipparcos ephemerides. According to simultaneous studies of radial velocities with Hipparcos light curve and recent and historic light curves in Strömgren bands, η Mus-A consists of two quasi-identical components: M 1 = 3.30 M , M 2 = 3.29 M , R 1 = 2.14 R , R 2 = 2.13 R , T 1 = 12 700 K and T 2 = 12 550 K separated from each other by a = 14.11 R in an orbit inclined 77. • 4. The membership of η Mus-A to the Lower Centaurus-Crux OB association is discussed. The rotational velocity of the primary component was found to be smaller than that of the secondary component. The asynchronous slow rotation of the primary and the synchronous rotation of the secondary imply a recent decrease in the orbital period, either due to orbital angular momentum being transferred to the visual companion η Mus-C or due to relatively frequent stellar encounters in this crowded region. The visual companion η Mus-B is found to be gravitationally unbound to the close pair η Mus-A. The radial velocity measurements of the visual companion η Mus-B, when combined with its positional information, support its membership to the Lower Centaurus-Crux OB association, but the evidence for membership of η Mus-A is weaker.

show abstract

Ap stars with resolved magnetically split lines: Magnetic field determinations from StokesIandVspectra

Mathys

2017

A&A

115

232

View full text Add to dashboard Cite

Aims. We present the results of a systematic study of the magnetic fields and other properties of the Ap stars with resolved magnetically split lines. Methods. This study is based on new measurements of the mean magnetic field modulus, the mean longitudinal magnetic field, the crossover, the mean quadratic magnetic field, and the radial velocity of 43 stars, complemented by magnetic data from the literature for 41 additional stars. Results. Stars with resolved magnetically split lines represent a significant fraction, of the order of several percent, of the whole population of Ap stars. Most of them are genuine slow rotators, whose consideration provides new insight into the long-period tail of the distribution of the periods of the Ap stars. Emerging correlations between rotation periods and magnetic properties provide important clues for the understanding of the braking mechanisms that have been at play in the early stages of stellar evolution. The geometrical structures of the magnetic fields of Ap stars with magnetically resolved lines appear in general to depart slightly, but not extremely, from centred dipoles. However, there are a few remarkable exceptions, which deserve further consideration. We suggest that pulsational crossover can be observed in some stars; if confirmed, this would open the door to the study of non-radial pulsation modes of degree ℓ too high for photometric or spectroscopic observations. How the lack of short orbital periods among binaries containing an Ap component with magnetically resolved lines is related with their (extremely) slow rotation remains to be fully understood, but the very existence of a correlation between the two periods lends support to the merger scenario for the origin of Ap stars.

show abstract

The eclipsing double-lined binaries V883 Cen and Mus

Cited by 7 publications

References 18 publications

The Multiple Star η Muscae

The Multiple Star η Muscae

Muscae: a young detached binary with two identical components

Ap stars with resolved magnetically split lines: Magnetic field determinations from StokesIandVspectra

Contact Info

Product

Resources

About