Variable radial velocities of two stars in the Taurus stream.

Barrett, Storrs B.

doi:10.1086/141795

Cited by 2 publications

(4 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A faint companion was detected interferometrically by Marion et al (2014) at a separation of 11 mas, contributing only about 3% in H band. 90 Tau was reported early on as a spectroscopic binary (Barrett 1910), but is labeled as a "constant:" velocity star in Abt (1965). Based on the evidence, we expect the interferometric companion to have little effect on the system photometry in the optical, but it is unclear whether there is a closer companion affecting the velocities.…”

Section: A2 Hyades Membersmentioning

confidence: 92%

“…HD 28527 / vB 82: This star is labelled as a δ Sct variable in SIMBAD, but it appears to be a constant star (Kovacs & Paparo 1989). It was identified as a possible binary by Barrett (1910), but later labeled as velocity constant in Abt (1965). Multiple lunar occultation observations (White 1979;Radick & Lien 1980;Fekel et al 1980;Evans & Edwards 1981;Radick et al 1982;Richichi et al 1999) have been negative for a companion, while Peterson et al (1981) provide "strong, but not definitive" evidence of a companion with fairly large magnitude difference (∼ 3 mag) at very small separation.…”

mentioning

confidence: 99%

See 1 more Smart Citation

The Interferometric Binary Epsilon Cancri in Praesepe: Precise Masses and Age

Morales,

Sandquist,

Schaefer

et al. 2022

Preprint

View full text Add to dashboard Cite

We observe the brightest member of the Praesepe cluster, Cnc, to precisely measure the characteristics of the stars in this binary system, en route to a new measurement of the cluster's age. We present spectroscopic radial velocity measurements and interferometric observations of the sky-projected orbit to derive the masses, which we find to be M 1 /M = 2.420 ± 0.008 and M 2 /M = 2.226 ± 0.004. We place limits on the color-magnitude positions of the stars by using spectroscopic and interferometric luminosity ratios while trying to reproduce the spectral energy distribution of Cnc. We re-examine the cluster membership of stars at the bright end of the color-magnitude diagram using Gaia data and literature radial velocity information. The binary star data are consistent with an age of 637 ± 19 Myr, as determined from MIST model isochrones. The masses and luminosities of the stars appear to select models with the most commonly used amount of convective core overshooting.

show abstract

Section: A2 Hyades Membersmentioning

confidence: 92%

mentioning

confidence: 99%

The Interferometric Binary Epsilon Cancri in Praesepe: Precise Masses and Age

Morales,

Sandquist,

Schaefer

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…A faint companion was detected interferometrically by Marion et al (2014) at a separation of 11 mas, contributing only about 3% in H band. 90 Tau was reported early on as a spectroscopic binary (Barrett 1910) but is labeled as a "constant:" velocity star in Abt (1965). Based on the evidence, we expect the interferometric companion to have little effect on the system photometry in the optical, but it is unclear whether there is a closer companion affecting the velocities.…”

Section: A2 Hyades Membersmentioning

confidence: 99%

“…HD 28527/vB 82: This star is labeled as a δ Sct variable in SIMBAD, but it appears to be a constant star (Kovacs & Paparo 1989). It was identified as a possible binary by Barrett (1910) but later labeled as velocity constant in Abt (1965). Multiple lunar occultation observations (White 1979;Fekel et al 1980;Radick & Lien 1980;Evans & Edwards 1981;Radick et al 1982;Richichi et al 1999) have been negative for a companion, while Peterson et al (1981) provide "strong, but not definitive" evidence of a companion with fairly large magnitude difference (∼3 mag) at very small separation.…”

Section: A2 Hyades Membersmentioning

confidence: 99%

The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age

Morales¹,

Sandquist²,

Schaefer³

et al. 2022

View full text Add to dashboard Cite

We observe the brightest member of the Praesepe cluster, ϵ Cnc, to precisely measure the characteristics of the stars in this binary system, en route to a new measurement of the cluster’s age. We present spectroscopic radial velocity measurements and interferometric observations of the sky-projected orbit to derive the masses, which we find to be M 1/M ⊙ = 2.420 ± 0.008 and M 2/M ⊙ = 2.226 ± 0.004. We place limits on the color–magnitude positions of the stars by using spectroscopic and interferometric luminosity ratios while trying to reproduce the spectral energy distribution of ϵ Cnc. We reexamine the cluster membership of stars at the bright end of the color–magnitude diagram using Gaia data and literature radial velocity information. The binary star data are consistent with an age of 637 ± 19 Myr, as determined from MIST model isochrones. The masses and luminosities of the stars appear to select models with the most commonly used amount of convective core overshooting.

show abstract

Variable radial velocities of two stars in the Taurus stream.

Cited by 2 publications

References 0 publications

The Interferometric Binary Epsilon Cancri in Praesepe: Precise Masses and Age

The Interferometric Binary Epsilon Cancri in Praesepe: Precise Masses and Age

The Interferometric Binary ϵ Cnc in Praesepe: Precise Masses and Age

Contact Info

Product

Resources

About