Circumstellar material in Algol - A study of the Balmer line profiles

Richards, Mercedes T.

doi:10.1086/191778

Cited by 62 publications

(66 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Note that absorption in Hα and profiles of He and Na lines at phases around 0.8 in AX Mon are very similar to those of V505 Mon at phase zero. Various absorption components in Hα -probably due to clouds -were also observed in Algol (Richards 1993).…”

Section: The Cloudy Nature Of the Circumstellar Mattermentioning

confidence: 81%

V505 Mon -An early-type binary with a disk

Mayer

Chochol

Drechsel³

et al. 2001

A&A

View full text Add to dashboard Cite

Abstract. New spectra of the eclipsing binary V505 Mon (usually classified as B5 Ib) were obtained in the optical and UV regions. Only spectral lines of one component are visible, with K = 93 km s −1 . According to arguments based on the extent of the disk the mass ratio might be about 0.30. The star with the visible spectral lines would then have a mass of 2.3, the other component of 7.7 M , i.e. their supergiant nature can be ruled out. The distance to the system appears to be about 1 kpc. Together with published photometric data, the spectroscopy provides clear evidence for the presence of a disk around the secondary component. The profiles of the C ii 1335/6 doublet lines are used to derive the rotational velocity of the disk. The structure of the disk can be characterized by a central ionized zone surrounded by neutral outer parts. Additional matter of cloudy nature has to be present, and both components are embedded in an extended atmosphere. Abundance of carbon was found to be very low. Similarity with some other non-eclipsing binaries is discussed.

show abstract

Section: The Cloudy Nature Of the Circumstellar Mattermentioning

confidence: 81%

V505 Mon -An early-type binary with a disk

Mayer

Chochol

Drechsel³

et al. 2001

A&A

View full text Add to dashboard Cite

show abstract

“…Intensities or EW analysis of any extra absorption and/or emission feature in the system are not possible because of blending effects with photospheric absorption. One way to analyse these emission/absorption features is by subtracting the stellar photospheric absorption profiles from the observed spectra to produce the so-called difference profiles (Richards 1993).…”

Section: Difference Profilesmentioning

confidence: 99%

Exploring the long-term variability and evolutionary stage of the interacting binary DQ Velorum

Barría

Mennickent

Graczyk

et al. 2014

A&A

View full text Add to dashboard Cite

Aims. In order to better understand the double periodic variable (DPV) phenomenon, we analyse a series of optical spectra of the DPV system DQ Velorum during much of its long-term cycle. In addition, we investigate the evolutionary history of DQ Vel using theoretical evolutionary models to obtain the best representation for the current observed stellar and orbital parameters of the binary. We investigate the evolution of DQ Vel through theoretical evolutionary models to estimate the age and the mass transfer rate which are then compared with those of its twin V393 Scorpii. Methods. We subtracted the donor star contribution from the composite spectra of DQ Vel using a synthetic spectrum as a donor template. Donor-subtracted spectra covering around 60% of the long-term cycle allowed us to investigate time-modulated spectral variations of the gainer star plus the disc. We used Gaussian fits to measure the equivalent widths (EWs) of Balmer and helium lines in the separated spectra during the long-term cycle and thus analyse EW variabilities. We compared the observed stellar parameters of the system with a grid of theoretical evolutionary tracks computed under a conservative and a non-conservative evolution regime. Results. We have found that the EW of Balmer and helium lines in the donor-subtracted spectra are modulated with the long-term cycle. We observe a strengthening in the EWs in all analysed spectral features at the minimum of the long-term cycle which might be related to an extra line emission during the maximum of the long-term variability. Difference spectra obtained at the secondary eclipse support this scenario. We have found that a non-conservative evolutionary model where DQ Vel has lost mass at some stage of its binary history, is a better representation of the current observed properties of the system. The best evolutionary model suggests that DQ Vel has an age of 7.40 × 10 7 yr and is currently in a low mass transfer rate (−9.8 × 10 −9 M /yr) stage, after a mass transfer burst episode. Comparing the evolutionary stages of DQ Vel and V393 Sco we observed that the former is an older system with a lower mass transfer rate. This might explain the differences observed in the physical parameters of their accretion discs.

show abstract

“…Short period close binaries (e.g., EP And) i.e., those having an orbital period P , 5À6 days, possess the above mentioned characteristics, due to rapid rotation (Richard & Albright 1993). Many authors (see e.g., Richards 1993Richards , 1992Hall 1989& Olson 1981 have discussed that the secondary and/or primary in the close binaries having a late type component show a variety of time dependent magnetic properties, which may cause, brightness variations in the LC (particularly at mid primary eclipse), radiations of X-ray, Ultraviolet, infrared, and cyclic variations in the orbital period of the binary (through a mechanism purposed by Applegate 1992 and modified by Lanza et al 1998& Lanza 2005. This mechanism is based on the variation of the active star shape through a change in the Gravitational Quadrupole Moment (GQM) of the star.…”

Section: Magnetic Cycle Effectmentioning

confidence: 99%

A Model for Contact Binary EP Andromedae

Manzoori¹

2012

Publ. – Astron. Soc. Aust

View full text Add to dashboard Cite

This paper presents the first comprehensive study of the EP And system, a contact binary. In this work the solution of the standard V light curve was obtained using the PHOEBE program (version 0.3c). Absolute parameters of the stellar components were then determined, enabling us to discuss the structure and evolutionary status of the close binary EP And. The times of minima data ('OÀC curve') were analyzed. It was found that a third body with a period of 41.20 yr and mass 0.15 M } is orbiting around the system. Also a modulating period of an 11.72-yr cycle along with a relative period increase of DP P ¼ 1:79 Â 10 À7 were obtained, which were attributed to the magnetic activity cycle and mass transfer with rate Dm m ¼ 9:98 Â 10 À8 yr À1 between the components, respectively.

show abstract

Circumstellar material in Algol - A study of the Balmer line profiles

Cited by 62 publications

References 0 publications

V505 Mon -An early-type binary with a disk

V505 Mon -An early-type binary with a disk

Exploring the long-term variability and evolutionary stage of the interacting binary DQ Velorum

A Model for Contact Binary EP Andromedae

Contact Info

Product

Resources

About