Voltammetric determination of pyridoxine by use of a carbon paste electrode

Söderhjelm, Petter; Lindquist, Jörgen

doi:10.1039/an9750000349

Cited by 90 publications

(91 citation statements)

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“…So for the first runs we used the parameters for the β Persei system which were given in Kiseleva et al (1998). However, we have to note that setting the mutual inclination of the orbits to 100 • , as was done in the above mentioned work, results in a too fast variation in the observable inclination of the close system, which is inconsistent with the observations (see, e.g., Söderhjelm 1980). For these first runs we used three different sets of the k 2 , k 3 apsidal motion constants (see Table 1).…”

Section: An Application For Algolcontrasting

confidence: 42%

Tidal and rotational effects in the perturbations of hierarchical triple stellar systems

Borkovits

Forgács‐Dajka

2008

EAS Publications Series

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Abstract.A new numerical integrator has been developed for studying the orbital and spin evolution of hierarchical triple stellar systems. The code includes equilibrium tide approximations with arbitrary direction of rotational axes. The variation of the orbital elements (e.g. the inclination of the close -eclipsing -binary) and its observational consequences according to the distorted models with different mass-distributions of the stars, as well as with and without dissipation are studied in the case of the well-known eclipsing triple system Algol. We found that, in the absence of the tidal dissipation, the presence of the third star may cause sudden fluctuations in the orbital elements and the stellar rotation of the binary members even in the previously synchronized case, too. The dissipation can eliminate these fluctuations, nevertheless some variations which would produce observable effects in the same order which have been measured in several eclipsing binaries are also present.

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Section: An Application For Algolcontrasting

confidence: 42%

Tidal and rotational effects in the perturbations of hierarchical triple stellar systems

Borkovits

Forgács‐Dajka

2008

EAS Publications Series

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“…The EA systems have obviously different depths between the primary and secondary minima, and have clearly defined times for the beginning and ending of the eclipses; EA systems are often but not always a detached eclipsing system (Catelan & Smith 2015), although the prototype of the class, Algol, is believed to be a semidetached system (Soderhjelm 1980;Kolbas et al 2015). The EB systems show a continuous change in brightness and have a deeper primary depth than that of the secondary.…”

Section: Searching For Variabilitymentioning

confidence: 99%

Variable Stars Observed in the Galactic Disk by AST3-1 from Dome A, Antarctica

Wang

et al. 2017

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AST3-1 is the second-generation wide-field optical photometric telescope dedicated to time domain astronomy at Dome A, Antarctica. Here we present the results of i band images survey from AST3-1 towards one Galactic disk field. Based on time-series photometry of 92,583 stars, 560 variable stars were detected with i magnitude ≤ 16.5 mag during eight days of observations; 339 of these are previously unknown variables. We tentatively classify the 560 variables as 285 eclipsing binaries (EW, EB, EA), 27 pulsating variable stars (δ Scuti, γ Doradus, δ Cephei variable and RR Lyrae stars) and 248 other types of variables (unclassified periodic, multi-periodic and aperiodic variable stars). Among the eclipsing binaries, 34 show O'Connell effects. One of the aperiodic variables shows a plateau light curve and another one shows a secondary maximum after peak brightness. We also detected a complex binary system with RS CVn-like light curve morphology; this object is being followed-up spectroscopically using the Gemini South telescope.

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“…(The masses are given in solar mass, the period in days, and the angular orbital elements in degrees.) The non-arbitrary parameters are taken from Söderhjelm (1980), Lestrade et al (1993) for Algol, and from Drechsel et al (1994) …”

Section: Comparison With Other Analytical and Numerical Calculationsmentioning

confidence: 99%

On the detectability of long period perturbations in close hierarchical triple stellar systems

Borkovits

Érdi

Forgács‐Dajka

et al. 2003

A&A

104

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Abstract.We study the possibility of the detection of the low amplitude long (P ) period perturbative effect of a distant third companion on the motion of a close binary. We give a new, more accurate analytical formula for this kind of perturbation affecting the moments of the times of minima in eclipsing binaries. The accuracy of this formula is tested by numerical integrations carried out for several initial configurations. We also describe a numerical method based on a non-linear Levenberg-Marquardt algorithm which makes it possible to separate this dynamical effect from the pure geometrical light-time effect in the eclipsing O−C diagram. The capabilities of this new method are demonstrated by the analysis of numerically simulated O−Cs for test systems having physical parameters very similar to Algol and IU Aur. The results show that the above mentioned effect would be detectable in these systems nowadays, observing almost each minima events in a 1-2 year-long interval.

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Voltammetric determination of pyridoxine by use of a carbon paste electrode

Cited by 90 publications

References 0 publications

Tidal and rotational effects in the perturbations of hierarchical triple stellar systems

Tidal and rotational effects in the perturbations of hierarchical triple stellar systems

Variable Stars Observed in the Galactic Disk by AST3-1 from Dome A, Antarctica

On the detectability of long period perturbations in close hierarchical triple stellar systems

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