Catalogue of Algol type binary stars

Budding, E.; Erdem, A.; Çiçek, C.; Bulut, I.; Soydugan, F.; Soydugan, E.; Bakış, V.; Demirçan, Osman

doi:10.1051/0004-6361:20034135

Cited by 137 publications

(130 citation statements)

References 31 publications

Supporting

Mentioning

126

Contrasting

Order By: Relevance

“…-CL Aur: all the data for this Algol binary, including a value for T spot on the gainer, are given by Lee et al (2010). -U Cep: masses, radii, and effective temperatures of donor and gainer are given by Budding et al (2004). A value foṙ P = +9.796 × 10 −7 d y −1 was derived by ourselves from the "Eclipsing Binaries Minima Base" of Kundera, completed with the epochs of the most recent eclipses that can easily be found on the CDS website.…”

Section: Discussionmentioning

confidence: 99%

“…Van Rensbergen et al (2008) used the mass ratio and orbital period distribution of Algols out of a sample of 303 observed systems. These systems were taken from the catalog of Budding et al (2004) extended with semidetached Algols from the catalog of Brancewicz et al (1980). All these systems are issued from a binary with a B-type primary at birth.…”

Section: Loss Of Angular Momentummentioning

confidence: 99%

“…-SW Cyg: masses, radii, and effective temperatures can be found in the catalog of Budding (2004) and Richards & Albright (1999). Values forṖ (and thusṀ) are from Qian et al (2002).…”

Section: A2 Three Gainers With An Accretion Diskmentioning

confidence: 99%

“…The distribution of orbital periods of Algols is precisely known since the time between two subsequent eclipses for every system has been measured accurately. The catalog of Budding et al (2004) extended with the semidetached Algols from Brancewicz et al (1980) supplies us with 303 Algols that can be issued from binary evolution with a B-type primary at birth. Van Rensbergen et al (2006) showed that the distribution of mass ratios strongly depends on the method used to interpret the observations.…”

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

Mass loss out of close binaries

Rensbergen

Greve

Mennekens

et al. 2011

A&A

View full text Add to dashboard Cite

Context. Several authors have previously introduced liberal evolution of interacting binaries, with the purpose of meeting various observed binary characteristics better than with conservative evolution. Since Algols are eclipsing binaries, the distribution of their orbital periods is known precisely. The distribution of their mass ratios contains, however, more uncertainties. We try to reproduce these two distributions theoretically using a liberal scenario in which the gainer star can lose mass into interstellar space as a consequence of its rapid rotation and the energy of a hot spot. Aims. In a recent paper we calculated the liberal evolution of binaries with a B-type primary at birth where mass transfer starts during core hydrogen burning of the donor. In this paper we include the cases where mass transfer starts during shell hydrogen burning, and it is our aim to reproduce the observed distributions of the system parameters of Algol-type semidetached systems. Methods. Our calculations reveal the amount of time that an Algol binary lives with a well-defined value of mass ratio and orbital period. We used these data to simulate the distribution of mass ratios and orbital periods of Algols. Results. Binaries with a late B-type initial primary hardly lose any mass, whereas those with an early B primary evolve in a nonconservative way. Conservative binary evolution predicts only ∼12% of Algols with a mass ratio q above 0.4. This value is raised up to ∼17% using our scenario of liberal evolution, which is still far below the ∼45% that is observed. Conclusions. Observed orbital periods of Algol binaries longer than one day are faithfully reproduced by our liberal scenario. Mass ratios are reproduced better than with conservative evolution, but the resemblance is still poor.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Loss Of Angular Momentummentioning

confidence: 99%

“…-SW Cyg: masses, radii, and effective temperatures can be found in the catalog of Budding (2004) and Richards & Albright (1999). Values forṖ (and thusṀ) are from Qian et al (2002).…”

Section: A2 Three Gainers With An Accretion Diskmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

Mass loss out of close binaries

Rensbergen

Greve

Mennekens

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…In Fig. 4, we present the distance distribution for 152 objects (joint entries in the Budding et al (2004) and Hipparcos (ESA 1997) catalogues), which correspond to about 10% of all Algols in the Budding et al (2004) catalogue. To evaluate which among these systems might be detectable by IRAS, Fig.…”

Section: Distancementioning

confidence: 99%

Non-conservative evolution in Algols: where is the matter?

Deschamps

Braun

Jorissen

et al. 2015

A&A

View full text Add to dashboard Cite

Context. There is indirect evidence of non-conservative evolutions in Algols. However, the systemic mass-loss rate is poorly constrained by observations and generally set as a free parameter in binary-star evolution simulations. Moreover, systemic mass loss may lead to observational signatures that still need to be found. Aims. Within the "hotspot" ejection mechanism, some of the material that is initially transferred from the companion star via an accretion stream is expelled from the system due to the radiative energy released on the gainer's surface by the impacting material. The objective of this paper is to retrieve observable quantities from this process and to compare them with observations. Methods. We investigate the impact of the outflowing gas and the possible presence of dust grains on the spectral energy distribution (SED). We used the 1D plasma code Cloudy and compared the results with the 3D Monte-Carlo radiative transfer code Skirt for dusty simulations. The circumbinary mass-distribution and binary parameters were computed with state-of-the-art binary calculations done with the Binstar evolution code. Results. The outflowing material reduces the continuum flux level of the stellar SED in the optical and UV. Because of the timedependence of this effect, it may help to distinguish between different ejection mechanisms. If present, dust leads to observable infrared excesses, even with low dust-to-gas ratios, and traces the cold material at large distances from the star. By searching for this dust emission in the WISE catalogue, we found a small number of Algols showing infrared excesses, among which the two rather surprising objects SX Aur and CZ Vel. We find that some binary B[e] stars show the same strong Balmer continuum as we predict with our models. However, direct evidence of systemic mass loss is probably not observable in genuine Algols, since these systems no longer eject mass through the hotspot mechanism. Furthermore, owing to its high velocity, the outflowing material dissipates in a few hundred years. If hot enough, the hotspot may produce highly ionised species, such as Si iv, and observable characteristics that are typical of W Ser systems. Conclusions. If present, systemic mass loss leads to clear observational imprints. These signatures are not to be found in genuine Algols but in the closely related β Lyraes, W Serpentis stars, double periodic variables, symbiotic Algols, and binary B[e] stars. We emphasise the need for further observations of such objects where systemic mass loss is most likely to occur.

show abstract

Long‐term orbital period behaviors of the neglected Algol type binaries: CC Herculis and XZ Aquilae

Soydugan

İbanoǧlu

et al. 2006

Astron Nachr

Self Cite

View full text Add to dashboard Cite

Orbital period variations of two neglected Algol type binaries, CC Her and XZ Aql, are studied based on all available times of minima. In the case of CC Her, it is found that the O-C curve displays a tilted sinusoidal variation with an eccentricity of 0.54 ± 0.03 and a period of 52.4 ± 0.4 yr, which can be explained by the light-time effect due to the presence of an unseen component. The course of the orbital period change in XZ Aql appears less reliable but its O-C curve can be represented by a periodic variation with a period of 36.7 ± 0.6 yr superimposed on an upward parabola. The parabolic variation indicates a secular period increase with a rate of dP/dt = 7.1 s per century. The corresponding conservative mass transfer from less massive component to the more massive one is about 3.26 × 10 −7 M yr −1 . It is interesting to see that the O-C variation of CC Her displays no evidence (as upward parabola) on the mass transfer characteristic for Algols. The periodic change of the orbital period of XZ Aql, like CC Her, may be caused by the presence of the thirdbody. The lower limits of the masses of the hypothetical unseen components for CC Her and XZ Aql are found to be 2.69 M and 0.47 M , respectively. The third body of CC Her should be detectable not only spectroscopically but also photoelectrically, if it exists.

show abstract

Catalogue of Algol type binary stars

Cited by 137 publications

References 31 publications

Mass loss out of close binaries

Mass loss out of close binaries

Non-conservative evolution in Algols: where is the matter?

Long‐term orbital period behaviors of the neglected Algol type binaries: CC Herculis and XZ Aquilae

Contact Info

Product

Resources

About