S$\mathsf{_{B^9}}$: The ninth catalogue of spectroscopic binary orbits

Pourbaix, D.; Tokovinin, Andreï; Batten, A. H.; Fekel, Francis C.; Hartkopf, William I.; Levato, H.; Morrell, N.; Torres, Guillermo; Udry, S.

doi:10.1051/0004-6361:20041213

Cited by 616 publications

(628 citation statements)

References 10 publications

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“…Some of them are eclipsing binaries with a pulsating component, and some semi-regular variables with unknown short-term variations or some pulsating ellipsoidal variables (Derekas et al 2006;Nie, Zhang, & Jiang 2010;Faigler & Mazeh 2011;Faigler et al 2012). In several studies, V1464 Aql was classified as a spectroscopic binary system, RR Lyr (RRc), an eclipsing binary, possibly contact (EC) or semi-detached system (ESD) (Duerbeck 1997;Pourbaix et al 2004;Pribulla & Rucinski 2006; PASA, 30, e016 (2013) doi:10.1017/pasa.2012.016 Aerts et al (2002). c Henry et al (2004).…”

Section: Resultsmentioning

confidence: 99%

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

Dal

Sipahi

2013

Publ. Astron. Soc. Aust.

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Taking into account the results obtained from the models and analyses of the BVRI light curves, we discuss the nature of V1464 Aql. The analyses indicated that the mass ratio of the system is q = 0.71 ± 0.02, while the inclination of the system (i) is 38°.45 ± 0°.22. Taking the primary component's temperature as 7 420 ± 192 K, we found that the temperature of the secondary is 6 232 ± 161 K. The mass of the primary component was found to be 1.74 ± 0.05 M ࣻ , while it is 1.23 ± 0.01 M ࣻ for the secondary. The primary component's radius was found to be 2.10 ± 0.05 R ࣻ , while it was found as 1.80 ± 0.01 R ࣻ for the secondary. Revealing that the system should not exhibit any eclipses, we demonstrated that the main variation with large amplitude should be caused due to the ellipsoidal effect. Indeed, the Fourier analysis also supported the result. For the first time in the literature, we revealed that the primary component is a δ Scuti star. The period of pulsation was found to be 58.482 ± 0.002, 58.482 ± 0.001, 60.966 ± 0.002, and 60.964 ± 0.003 min in BVRI bands, respectively. We plotted V1464 Aql in the log(P orb )-log (P pulse ) plane. Using more than 160 binaries, whose one or both components are pulsating, we derived a new linear fit in the log (P orb )-log (P pulse ) plane for each type of binary. Using the linear fit of each group, we obtained new calibrations between log (P orb ) and log (P pulse ) for different types of pulsating stars. In addition, a calibration has been obtained for the first time for the pulsating stars with spectral types O and B. V1464 Aql seems to be located near the other ellipsoidal and close binaries. Thus, we listed V1464 Aql as a new candidate for the ellipsoidal variables with a δ Scuti component.

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Section: Resultsmentioning

confidence: 99%

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

Dal

Sipahi

2013

Publ. Astron. Soc. Aust.

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“…-HD 4747 (HIP 3850) has a potential brown-dwarf companion discovered with radial velocities by Nidever et al (2002). We combine CORALIE observations with the KECK HIRES radial velocities of Nidever et al (2002) retrieved from the SB9-catalogue (Pourbaix et al 2004). However, the orbital period is very long and not covered by the measurements (see Fig.…”

Section: Details Of the Surveyed Starsmentioning

confidence: 99%

Search for brown-dwarf companions of stars

Sahlmann

Ségransan

Queloz

et al. 2010

A&A

Self Cite

213

314

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Context. The frequency of brown-dwarf companions in close orbit around Sun-like stars is low compared to the frequency of planetary and stellar companions. There is presently no comprehensive explanation of this lack of brown-dwarf companions. Aims. By combining the orbital solutions obtained from stellar radial-velocity curves and Hipparcos astrometric measurements, we attempt to determine the orbit inclinations and therefore the masses of the orbiting companions. By determining the masses of potential brown-dwarf companions, we improve our knowledge of the companion mass-function. Methods. The radial-velocity solutions revealing potential brown-dwarf companions are obtained for stars from the CORALIE and HARPS planet-search surveys or from the literature. The best Keplerian fit to our radial-velocity measurements is found using the Levenberg-Marquardt method. The spectroscopic elements of the radial-velocity solution constrain the fit to the intermediate astrometric data of the new Hipparcos reduction. The astrometric solution and the orbit inclination are found using non-linear χ 2 -minimisation on a two-parameter search grid. The statistical confidence of the adopted orbital solution is evaluated based on the distribution-free permutation test. Results. The discovery of nine new brown-dwarf candidates orbiting stars in the CORALIE and HARPS radial-velocity surveys is reported. New CORALIE radial velocities yielding accurate orbits of six previously-known hosts of potential brown-dwarf companions are presented. Including the literature targets, 33 hosts of potential brown-dwarf companions are examined. Employing innovative methods, we use the new reduction of the Hipparcos data to fully characterise the astrometric orbits of six objects, revealing M-dwarf companions of masses between 90 M J and 0.52 M . In addition, the masses of two companions can be restricted to the stellar domain. The companion to HD 137510 is found to be a brown dwarf. At 95% confidence, the companion of HD 190228 is also a brown dwarf. Twenty-three companions remain brown-dwarf candidates. On the basis of the CORALIE planet-search sample, we obtain an upper limit of 0.6% for the frequency of brown-dwarf companions around Sun-like stars. We find that the companion-mass distribution function increases toward the lower end of the brown-dwarf mass range, suggesting that we detect the high-mass tail of the planetary distribution. Conclusions. Our findings agree with the results of previous similar studies and confirm the pronounced paucity of brown-dwarf companions around Sun-like stars. They are affected by the Hipparcos astrometric precision and mission duration, which limits the minimum detectable companion mass, and some of the remaining candidates are probably brown-dwarf companions.

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“…Finally, stars in multiple systems were removed from the sample. We used the CCDM (Dommanget & Nys 1994 and SB9 (Pourbaix et al 2004) catalogues to identify astrometric and spectroscopic binaries, respectively. These stars are potential targets for present and future projects that aim to detect Earth-like planets or exo-solar analogues to the Edgeworth-Kuiper Belt.…”

Section: The Stellar Samplementioning

confidence: 99%

Chromospheric activity and rotation of FGK stars in the solar vicinity

Martínez-Arnáiz¹,

Maldonado

Montes³

et al. 2010

A&A

116

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Context. Chromospheric activity produces both photometric and spectroscopic variations that can be mistaken as planets. Large spots crossing the stellar disc can produce planet-like periodic variations in the light curve of a star. These spots clearly affect the spectral line profiles, and their perturbations alter the line centroids creating a radial velocity jitter that might "contaminate" the variations induced by a planet. Precise chromospheric activity measurements are needed to estimate the activity-induced noise that should be expected for a given star. Aims. We obtain precise chromospheric activity measurements and projected rotational velocities for nearby (d ≤ 25 pc) cool (spectral types F to K) stars, to estimate their expected activity-related jitter. As a complementary objective, we attempt to obtain relationships between fluxes in different activity indicator lines, that permit a transformation of traditional activity indicators, i.e., Ca ii H & K lines, to others that hold noteworthy advantages.Methods. We used high resolution (∼50 000) echelle optical spectra. Standard data reduction was performed using the IRAF echelle package. To determine the chromospheric emission of the stars in the sample, we used the spectral subtraction technique. We measured the equivalent widths of the chromospheric emission lines in the subtracted spectrum and transformed them into fluxes by applying empirical equivalent width and flux relationships. Rotational velocities were determined using the cross-correlation technique. To infer activity-related radial velocity (RV) jitter, we used empirical relationships between this jitter and the R HK index. Results. We measured chromospheric activity, as given by different indicators throughout the optical spectra, and projected rotational velocities for 371 nearby cool stars. We have built empirical relationships among the most important chromospheric emission lines. Finally, we used the measured chromospheric activity to estimate the expected RV jitter for the active stars in the sample.

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S$\mathsf{_{B^9}}$: The ninth catalogue of spectroscopic binary orbits

Cited by 616 publications

References 10 publications

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

Search for brown-dwarf companions of stars

Chromospheric activity and rotation of FGK stars in the solar vicinity

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