Tertiary companions to close spectroscopic binaries

Tokovinin, Andreï; Thomas, S.; Sterzik, M.; Udry, S.

doi:10.1051/0004-6361:20054427

Cited by 444 publications

(551 citation statements)

References 51 publications

Supporting

Mentioning

492

Contrasting

Order By: Relevance

“…We know now that W UMa binaries almost certainly have companions ; and citations therein), in full confirmation of the work of Tokovinin et al (2006) of the increasing multiplicity at short binary periods.…”

Section: W Uma-type Binaries (S M Rucinski)supporting

confidence: 75%

Commission 42: Close Binary Stars

Ruciński¹,

Ribas²,

Giménez³

et al. 2008

Proc. IAU

View full text Add to dashboard Cite

Two meetings of interest to close binaries took place during the reporting period: A full day session on short-period binary stars – mostly CV's – (Milone et al. 2008) during the 2006 AAS Spring meeting in Calgary and the very broadly designed IAU Symposium No. 240 on Binary Stars as Critical Tools and Tests in Contemporary Astrophysics in Prague, 2006, with many papers on close binaries [Hartkopf et al. 2007]. In addition, the book by Eggleton (2006), which is a comprehensive summary of evolutionary processes in binary and multiple stars, was published.

show abstract

Section: W Uma-type Binaries (S M Rucinski)supporting

confidence: 75%

Commission 42: Close Binary Stars

Ruciński¹,

Ribas²,

Giménez³

et al. 2008

Proc. IAU

View full text Add to dashboard Cite

show abstract

“…The star was listed as an uncertain spectroscopic binary in Tokovinin et al (2006), who did not have sufficient radial-velocity measurements to constrain the orbit. -HD 4747 (HIP 3850) has a potential brown-dwarf companion discovered with radial velocities by Nidever et al (2002).…”

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

214

314

View full text Add to dashboard Cite

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.

show abstract

“…This is the reason why we discuss it in a separate chapter. This common proper motion pair is comprised of a DA white dwarf (WD0433+270) and a K type star (BD +26 730) (Holberg et al 2002), which is a well studied variable star (V833 Tau) and also a single-lined spectroscopic binary with a very low-mass companion (Tokovinin et al 2006). As in the case of the rest of common proper motion pairs of our sample we can assume that they were born simultaneously and with the same chemical composition (Wegner 1973;Oswalt et al 1988).…”

Section: Introductionmentioning

confidence: 99%

Testing the Initial–Final Mass Relationship of White Dwarfs

Catalán

Isern

Garcı́a–Berro

et al. 2010

Astrophysics and Space Science Proceedings

113

184

View full text Add to dashboard Cite

A mis padres y hermana AgraïmentsEn primer lloc vull agrair als meus directors de tesi, Jordi Isern i Enrique García-Berro, que em donessin l'oportunitat de realitzar el doctorat a l'IEEC (al CSIC i a la UPC), així com que em proporcionessin tot el suport necessari. Crec que he après moltes coses importants en aquestsúltims anys, no només en la part científica, i això en partés una conseqüència d'haver treballat amb ells. Els vull donar les gràcies també pel suport i la confiança dipositada en mi, especialment durant aquestúltim any de feina.Durant tota aquestaèpoca he tingut la sort de tenir uns companys fantàstics que m'han fet molt més fàcil la feina. Primer vaig conèixer l'Alina, la meva companya de "fatigas" i després el Jose, el Pep i el Miquel. Més tard s'hi van afegir l'Ignasi, la Violeta, l'Anna C., l'Anna A., el Carlo, el Moi, el Nil, l'Anaïs. . . Tots els moments que hem compartit dins i fora de l'IEEC han estat molt importants per a mi i m'emporto un gran record de tota aquestaèpoca, primer al Nexus, després a la UAB i finalment a l'ETSE. Ara que tinc la oportunitat, els hi vull agrair als meus companys, o més ben dit, amics, tots elsànims i suport que m'han donat. També els hi vull donar les gràcies al personal d'administració i a la resta de companys que he tingut durant aquests anys.En especial, l'Ignasi es mereix un gran gràcies. . . Primer de tot, per venir a l'IEEC en un moment en que la meva feina necessitava d'un observador amb experiència. Per tenir la generositat de compartir els seus coneixements amb mi durant aquests anys, per acompanyar-me en les observacions, per tenir sempre tanta confiança en mi, molta més que jo mateixa i per ajudar-me sempre que se li presentés la oportunitat. Els seusànims i el seu suport han estat essencials per a que arribés aquest moment i per tant, només em queda donar-li el meu agraïment més sincer.También le debo un agradecimiento especial a Carlos Allende Prieto, que sin ni siquiera conocerme en persona aceptó acompañarme a observar al McDonald Observatory durante 10 días. Su ayuda y dedicación en la distancia, especialmente en el análisis de las compañeras de las enanas blancas, han sido también vitales para el desarrollo de esta tesis.Durante mi doctorado he tenido la oportunidad de disfrutar de estancias en otros centros. Le quiero dar las gracias a Inma Domínguez, Carlos Abia y Olga Zamora de la Universidad de Granada por la atención que me dispensaron cuando estuve allí. También quisiera dar las gracias a Roberto Silvotti y Juan Alcalá por la ayuda y el buen trato que me dieron durante el tiempo que pasé en el Osservatorio Astronomico di Capodimonte. Gracias también al resto de personas que trabajan en el Osservatorio y que hicieron mi estancia muy agradable.A mi profesor Manolo Segura le quiero agredecer que en su día me hiciera creer en mis posibilidades y despertara mi afán por intentar superarme poco a poco. Muchas gracias también por la "contingencia" y por la confianza dipositada en mí.En un momento para mí tan importante comoéste no me puedo olvi...

show abstract

Tertiary companions to close spectroscopic binaries

Cited by 444 publications

References 51 publications

Commission 42: Close Binary Stars

Commission 42: Close Binary Stars

Search for brown-dwarf companions of stars

Testing the Initial–Final Mass Relationship of White Dwarfs

Contact Info

Product

Resources

About