Spectroscopy of four early-type eclipsing binaries

Mayer, P.; Lorenz, R.; Drechsel, H.

doi:10.1051/0004-6361:20020486

Cited by 15 publications

(30 citation statements)

References 24 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Column 3 of Table 2 lists the period values obtained. Their weighted mean is P = 5.816032 ± 0.000058 days, which is very close to the He i λ4471 value and contains both ST96 and Mayer et al (1992) values within a ±1σ interval. The very small uncertainty of the ST96 period determination results from the large time base of their IUE data set (∼5860 days) which is almost exactly four times ours.…”

Section: The Periodsupporting

confidence: 52%

“…The study of the light curve of HD 152248 by Mayer et al (1992) revealed that the system displays two eclipses of unequal depth and that both minima are not separated by a 0.5 cycle, suggesting a non-zero eccentricity. Based on IUE observations and using a cross-correlation technique, Stickland et al (1996, ST96 hereafter) derived a period of 5.816083 days, an eccentricity of 0.124 and a mass ratio of 0.941.…”

Section: Overviewmentioning

confidence: 99%

“…Based on the same set of IUE data and using a tomographic reconstruction algorithm to separate primary and secondary spectra, Penny et al (1999, PGB hereafter) derived a spectral type of O7I+O7I. They also re-analysed the light curve of the system, complementing the Mayer et al (1992) data set with Hipparcos observations. PGB showed that the system displays ellipsoidal light variations due to tidal deformations.…”

Section: Overviewmentioning

confidence: 99%

See 2 more Smart Citations

HD 152248: Evidence for a colliding wind interaction

Sana

Rauw

Gosset

2001

A&A

View full text Add to dashboard Cite

Abstract. We present the results of a four year spectroscopic campaign on the early-type binary system HD 152248. Our analysis yields a new classification as O7.5III(f) + O7III(f), in contradiction with previous classifications of the components as supergiants. We derive improved orbital elements and the corresponding masses (M1 = 29.6 M and M2 = 29.9 M ) are somewhat larger than previously reported in the literature, although they are still significantly lower than the ones expected from evolutionary tracks. Both components of the system are close to filling their Roche lobe at periastron passage. We also investigate the equivalent width variations of the lines of the two components and we discuss their relation to the Struve-Sahade effect. Finally, we show that the line profile variability of the He ii λ4686 and H α lines is consistent with a strong wind interaction between the two stars, quite as predicted by current colliding wind models.

show abstract

Section: The Periodsupporting

confidence: 52%

Section: Overviewmentioning

confidence: 99%

Section: Overviewmentioning

confidence: 99%

See 1 more Smart Citation

HD 152248: Evidence for a colliding wind interaction

Sana

Rauw

Gosset

2001

A&A

View full text Add to dashboard Cite

show abstract

“…The spectra are listed in Table 1. They were reduced with the MIDAS package; details of the reduction procedure were described by Mayer et al (1997). The S/N ratio of the ECHELEC spectra is about 150, in case of CAT/CES spectra about 250.…”

Section: Spectroscopymentioning

confidence: 99%

The early-type multiple system QZ Carinae

Mayer

Lorenz²,

Drechsel³

et al. 2001

A&A

Self Cite

View full text Add to dashboard Cite

Abstract.We present an analysis of the early-type quadruple system QZ Car, consisting of an eclipsing and a non-eclipsing binary. The spectroscopic investigation is based on new high dispersion echelle and CAT/CES spectra of H and He lines. The elements for the orbit of the non-eclipsing pair could be refined. Lines of the brighter component of the eclipsing binary were detected in near-quadrature spectra, while signatures of the fainter component could be identified in only few spectra. Lines of the primary component of the non-eclipsing pair and of both components of the eclipsing pair were found to be variable in position and strength; in particular, the He ii 4686 emission line of the brighter eclipsing component is strongly variable. An ephemeris for the eclipsing binary QZ Car valid at present was derived Prim. Min. = hel. JD 2448687.16 + 5.d 9991 · E. The relative orbit of the two binary constituents of the multiple system is discussed. In contrast to earlier investigations we found radial velocity changes of the systemic velocities of both binaries, which were used -together with an O-C analysis of the expected light-time effect -to derive approximate parameters of the mutual orbit of the two pairs. It is shown that this orbit and the distance to QZ Car can be further refined by minima timing and interferometry.

show abstract

“…HD 75821 (#4) : this eclipsing binary has a period of about 26.3 days and a radial velocity semi-amplitude of 92 km s −1 (Mayer et al 1997).…”

Section: Spectroscopic Binariesmentioning

confidence: 99%

A new method for an objective,χ²-based spectroscopic analysis of early-type stars

Irrgang¹,

Przybilla²,

Heber³

et al. 2014

A&A

View full text Add to dashboard Cite

Astrophysics ABSTRACTContext. A precise quantitative spectral analysis, encompassing atmospheric parameter and chemical elemental abundance determination, is time-consuming due to its iterative nature and the multi-parameter space to be explored, especially when done by the naked eye. Aims. A robust automated fitting technique that is as trustworthy as traditional methods would allow for large samples of stars to be analyzed in a consistent manner in reasonable time.Methods. We present a semi-automated quantitative spectral analysis technique for early-type stars based on the concept of χ 2 minimization. The method's main features are as follows: far less subjectivity than the naked eye, correction for inaccurate continuum normalization, consideration of the whole useful spectral range, and simultaneous sampling of the entire multi-parameter space (effective temperature, surface gravity, microturbulence, macroturbulence, projected rotational velocity, radial velocity, and elemental abundances) to find the global best solution, which is also applicable to composite spectra. Results. The method is fast, robust, and reliable as seen from formal tests and from a comparison with previous analyses. Conclusions. Consistent quantitative spectral analyses of large samples of early-type stars can be performed quickly with very high accuracy.

show abstract

Spectroscopy of four early-type eclipsing binaries

Cited by 15 publications

References 24 publications

HD 152248: Evidence for a colliding wind interaction

HD 152248: Evidence for a colliding wind interaction

The early-type multiple system QZ Carinae

A new method for an objective,χ²-based spectroscopic analysis of early-type stars

Contact Info

Product

Resources

About

Spectroscopy of four early-type eclipsing binaries

Cited by 15 publications

References 24 publications

HD 152248: Evidence for a colliding wind interaction

HD 152248: Evidence for a colliding wind interaction

The early-type multiple system QZ Carinae

A new method for an objective,χ2-based spectroscopic analysis of early-type stars

Contact Info

Product

Resources

About

A new method for an objective,χ²-based spectroscopic analysis of early-type stars