The Metabolism of Iproniazid

Koechlin, Bernard A.; Iliev, Venelin

doi:10.1111/j.1749-6632.1959.tb49263.x

Cited by 26 publications

(3 citation statements)

References 5 publications

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“…Except for two more recorded attempts by Wilson (1939Wilson ( , 1941 to resolve the pair visually, almost 50 years elapsed until the next astrometric observations were made at Pulkovo Observatory by , with a similar interferometer also using a 6-m baseline. Additional long-baseline interferometric observations have been reported by Blazit et al (1977a) (baseline 12-20 m), Koechlin et al (1979) (baseline 13.8 m), Koechlin et al (1983) (baseline 5.5-35 m), (three-element Cambridge Optical Aperture Synthesis Telescope, COAST, using baselines up to 6.1 m), and more recently by (three-element Infrared Optical Telescope Array, IOTA, using baselines up to 38 m). By far the most precise interferometric observations of Capella are those of Hummel et al (1994) with the Mark III interferometer on Mount Wilson, using baselines of 3.0 to 23.6 m. These observations improved the uncertainties in both the position angle and the angular separation by about an order of magnitude compared to previous measures.…”

Section: Astrometric Observationsmentioning

confidence: 83%

“…The date assigned to this observation (not precisely given by either author) is JD 2,444,637.6, which corresponds to a reasonable hour angle at the Kitt Peak Observatory during twilight on UT 1981 February 2. Koechlin et al (1983): The first three interferometric measurements are apparently repeated from an earlier report by Koechlin et al (1979), although they are slightly different in two cases. We consider them to supersede the original measurements.…”

Section: Notes On the Astrometric Observationsmentioning

confidence: 88%

“…All other measurements obtained by long-baseline interferometry are given in Figure 8, including both those originally made in polar coordinates and those made in rectangular coordinates. Among the latter, the much larger residuals in ∆x (right ascension) than in ∆y (declination) are due to the north-south orientation of the baseline of the interferometer used by Koechlin et al (1979) and Koechlin et al (1983), which is the source of most of those measurements.…”

Section: Orbital Solutionmentioning

confidence: 99%

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Binary Orbit, Physical Properties, and Evolutionary State of Capella (Α Aurigae)

Torres

Claret

Young

2009

ApJ

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We report extensive radial-velocity measurements of the two giant components of the detached, 104day period binary system of Capella. Our highly accurate three-dimensional orbital solution based on all existing spectroscopic and astrometric observations including our own yields much improved masses for the primary and secondary of 2.466 ± 0.018 M ⊙ and 2.443 ± 0.013 M ⊙ , with relative errors of only 0.7% and 0.5%, respectively. The mass ratio is considerably closer to unity than previously believed, which has an impact on assessing the evolutionary state of the system. Improved values are presented also for the radii (11.87 ± 0.56 R ⊙ and 8.75 ± 0.32 R ⊙ ), effective temperatures (4920 ± 70 K and 5680 ± 70 K), and luminosities (79.5 ± 4.8 L ⊙ and 72.1 ± 3.6 L ⊙ ). The distance is determined to be 13.042 ± 0.028 pc, based on the accurate orbital parallax. The projected rotational velocities and individual rotation periods are also known. Capella is unique among evolved stars in that, in addition to all of the above, the chemical composition is known as well. This includes the overall metallicity [m/H], the carbon isotope ratio 12 C/ 13 C for the primary, and the lithium abundance and C/N ratios for both components. We present new or revised values for some of these. The latter three quantities are sensitive diagnostics of evolution, and change drastically for giants as a result of the deepening of the convective envelope during the first dredge-up. The secondary is crossing the Hertzprung gap, while the primary is believed to be in the longer-lived core-helium burning phase. Previous studies using only the masses, temperatures, and luminosities have found good agreement with stellar evolution models placing the primary in the clump. Here we compare all of the constraints simultaneously against three sets of current models. We find that they are unable to match all of the observations for both components at the same time, and at a single age, for any evolutionary state of the primary. This shows the great importance of chemical information for assessing the evolutionary state of giant stars. A comparison with models of tidal evolution yields similarly disappointing results, when tested against the fact that the orbit is circular, the primary is rotating synchronously, the secondary ∼12 times faster than synchronous, and the spin axes are apparently aligned with the axis of the orbit. When confronted in detail, our understanding of the advanced stages of stellar evolution is thus still very incomplete.