Mesures de vitesses radiales

Fehrenbach, Charles; Duflot, M.; Mannone, C.; Burnage, R.; Genty, V.

doi:10.1051/aas:1997360

Cited by 46 publications

(50 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The radial-velocity variability was confirmed by Petrie (1958), who mentioned an amplitude of 71 km s −1 from measurements at 12 epochs, and later by Fehrenbach et al (1997). However, radial velocities were measured as if it was a single-lined binary, while our high-resolution spectroscopy presented here reveals three components (Fig.…”

Section: Camelopardalissupporting

confidence: 79%

Northern Binaries in the Evrena Project

et al. 2011

View full text Add to dashboard Cite

show abstract

Section: Camelopardalissupporting

confidence: 79%

Northern Binaries in the Evrena Project

et al. 2011

View full text Add to dashboard Cite

show abstract

“…It is still not clear if CP stars are X-ray emitters at such levels, or if, alternatively, the observed X-ray flux is due to a late-type unseen companion. Three radial velocity measurements for XX Ari have been obtained by Fehrenbach et al (1997). The first and the second values, obtained about 654 days apart, differ by 24 km s −1 , while the second and the third values, obtained about 25 days apart, give the same result.…”

Section: Hd 20629 = XX Ari (D H = 238mentioning

confidence: 94%

Long-term monitoring of active stars

Cutispoto¹,

Messina²,

Rodonò³

2001

A&A

View full text Add to dashboard Cite

Abstract. As a part of an extensive program focused on the global properties and evolution of active stars, high-precision UBV (RI)c and UBV photometry of 31 selected stars is presented. The UBV (RI)c observations were collected at the European Southern Observatory over the 31 December 1992-18 January 1993 and the 20 November-3 December 1993 intervals. Additional UBV photometry obtained by the "Phoenix" and by the Catania Astrophysical Observatory Automatic Photoelectric Telescopes from 1990 to 1993 is also presented for some of the program stars. Significant evolution of the light curves, period variations and evidence for longterm variability of the global degree of spottedness are found. Some spectral classifications are revised and the inferred photometric parallaxes are compared, whenever possible, with the values measured by the Hipparcos satellite. These observations are finalized to the construction of an extended photometric database, which can give important clues on topics such as the stability of spotted areas, differential rotation, solar-like cycles and the correlation between inhomogeneities at different atmospheric levels.

show abstract

“…It was classified as B8V in an objective prism survey by Duflot et al (1957) and its only measured RV = +21 km s −1 also comes from such a survey (Fehrenbach et al 1996). It has a rather accurate parallax of 0.…”

Section: The B Star Hd 32328mentioning

confidence: 99%

Large distance ofε Aurigae inferred from interstellar absorption and reddening

Guinan

Mayer

Harmanec

et al. 2012

A&A

View full text Add to dashboard Cite

The long-period (P = 27.1 years) peculiar eclipsing binary ε Aur, which has recently completed its two year-long primary eclipse, has perplexed astronomers for over a century. The eclipse arises from the transit of a huge, cool and opaque, disk across the face of the F0 Iab star. One of the principal problems with understanding this binary is that the very small parallax of p = (1.53 ± 1.29) mas, implying a distance range of d ∼ (0.4−4.0) kpc, returned by a revised reduction of the Hipparcos satellite observations, is so uncertain that it precludes a trustworthy estimate of the luminosities and masses of the binary components. A reliable distance determination would help solve the nature of this binary and distinguish between competing models. A new approach is discussed here: we estimate the distance to ε Aur from the calibration of reddening and interstellar-medium gas absorption in the direction of the system. The distance to ε Aur is estimated from its measured E(B − V) and the strength of the diffuse interstellar band 6613.56 Å. Spectroscopy and UBV photometry of several B-and A-type stars (<1 • of ε Aur) were carried out. The distances of the reference stars were estimated from either measured or spectroscopic parallaxes. The range in distances of the reference stars is from 0.2 to 3.0 kpc. We find reasonably tight relations among E(B − V), EW, and I c (6613 Å feature) with distance. From these calibrations, a distance of d = (1.5 ± 0.5) kpc is indicated for ε Aur. If ε Aur is indeed at (or near) this distance, its inferred absolute visual magnitude of M V (−9.1 ± 1.1) mag for the F-supergiant indicates that it is a very young, luminous and massive star. Noteworthy, the high luminosity inferred here is well above the maximum value of M V −6. m 2 expected for (less-massive) post asymptotic giant branch supergiant stars. Thus, based on the circumstantial evidence, the higher-mass model appears to best explain the properties of this mysterious binary system. As a by-product of this study, our spectroscopy led to the finding that two of the stars used in the distance calibrations, HD 31617 and HD 31894, are newly discovered spectroscopic binaries, and HD 32328 is a new radial-velocity variable.

show abstract

Mesures de vitesses radiales

Abstract: Abstract. We publish 1879 radial velocities of stars distributed in 105 fields of 4• × 4• . We continue the PPO series (Fehrenbach et al. 1987;Duflot et al. 1990Duflot et al. , 1992Duflot et al. and 1995, using the Fehrenbach objective prism method.

Cited by 46 publications

References 0 publications

Northern Binaries in the Evrena Project

Northern Binaries in the Evrena Project

Long-term monitoring of active stars

Large distance ofε Aurigae inferred from interstellar absorption and reddening

Contact Info

Product

Resources

About