The asymptotic evolution of the stellar merger V1309 Sco: a Blue Straggler in the making?

Ferreira, T. S.; Saito, R. K.; Minniti, D.; Navarro, María Gabriela; Ramos, R. Contreras; Smith, Leigh C.; Lucas, P. W.

doi:10.1093/mnras/stz878

Cited by 31 publications

(18 citation statements)

References 37 publications

(46 reference statements)

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“…Photometric solutions show that CSS J135012.1+272259 is an A-subtype extreme mass ratio OC binary with mass ratio q = 0.147 that is predicted to merge and make a blue straggler or FK Com type star in the center (Tylenda et al, 2011;Ferreira et al, 2019). A-type is a sub-type of the W UMa's, and the W UMa's are a sub-type of the OCs (Binnendijk, 1970).…”

Section: Discussionmentioning

confidence: 99%

Photometric observations of an extreme mass ratio overcontact binary

Xiao¹,

Soonthornthum²,

Qian³

2020

caosp

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Our RC and IC light curves of CSS J135012.1+272259 were analyzed with the Wilson-Devinney (W-D) program. The results reveal that CSS J135012.1+272259 is an extreme mass ratio overcontact binary with mass ratio q = 0.147. It may be in the final evolutionary stage of cool short-period binaries and merge into a single rapid-rotation star to form a blue straggler or FK Com type star. Also, 25 extreme mass ratio overcontact binary systems (q ≤ 0.15) are collected for long-term monitoring. These targets will improve understanding of the pre-outburst state of overcontact binaries and enrich knowledge of the merger mechanism.

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Section: Discussionmentioning

confidence: 99%

Photometric observations of an extreme mass ratio overcontact binary

Xiao¹,

Soonthornthum²,

Qian³

2020

caosp

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“…At present, a lot of such type binaries have been analyzed (e.g., Yang et al 2009;Qian et al 2011;Liao et al 2017). However, there is only one target, V1309 Sco, whose merging progress has been observed (Tylenda et al 2011), and it is making a blue straggler (Ferreira et al 2019). Zhu et al (2016) derived that V1309 Sco is a very deep contact binary (f = 89.5%) with extremely low mass ratio (q ∼ 0.095) before the merge.…”

Section: Introductionmentioning

confidence: 99%

Two contact binaries with mass ratios close to the minimum mass ratio

Li,

Xia,

Kim

et al. 2021

Preprint

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The cut-off mass ratio is under debate for contact binaries. In this paper, we present the investigation of two contact binaries with mass ratios close to the low mass ratio limit. It is found that the mass ratios of VSX J082700.8+462850 (hereafter J082700) and 1SWASP J132829.37+555246.1 (hereafter J132829) are both less than 0.1 (q ∼ 0.055 for J082700, and q ∼ 0.089 for J132829). J082700 is a shallow contact binary with a contact degree of ∼19%, and J132829 is a deep contact system with a fillout factor of ∼70%. The O − C diagram analysis indicated that both the two systems manifest long-term period decrease. In addition, J082700 exhibits a cyclic modulation which is more likely resulted from Applegate mechanism. In order to explore the properties of extremely low mass ratio contact binaries (ELMRCBs), we carried out a statistical analysis on contact binaries with mass ratios of q 0.1 and discovered that the values of J spin /J orb of three systems are greater than 1/3. Two possible explanations can interpret this phenomenon. One is that some physical processes, unknown to date, are not considered when Hut presented the dynamically instability criterion. The other is that the dimensionless gyration radius (k) should be smaller than the value we used (k 2 = 0.06). We also found that the formation of ELMRCBs possibly has two channels. The study of evolutionary states of ELMRCBs reveals that their evolutionary states are similar with those of normal W UMa contact binaries.

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“…Accurate basic physical parameters (masses, radii and luminosities of each component) are the key information for studying these two physical processes. Furthermore, contact binaries may be progenitors of luminous red novae (LRNs; e.g., V1309 Sco, Tylenda et al 2011;Stȩpień 2011;Zhu et al 2016;Pietrukowicz et al 2017) and blue stragglers (BSs; e.g., Eggleton 2012;Ferreira et al 2019). The basic physical parameters of contact binaries are also necessary to understand the formation of these peculiar objects.…”

Section: Introductionmentioning

confidence: 99%

Error Analysis of the Light Curve Solution of Contact Binaries Based on the W-D Code

Liu

2021

Preprint

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We use the idea of repeat measurement to determine the mean value and error of light curve solution parameters of contact binaries. Our simulation is realized by the Monte Carlo algorithm and Wilson-Devinney code. This method can obtain the systematic and random error simultaneously. Within our 48 models, the systematic errors are smaller than the random errors in most case. According to the numerical calculations, it is found that the relative errors of photometric mass ratios are less than 1 % for totally eclipsing contact binaries, while they are generally between 10 % and 20 % for partly eclipsing ones. The effect of third light on the errors of photometric solution is also investigated. With a third light, these errors are close to 10 % for totally eclipsing contact binaries. Specially, it is better to set the third light to zero in flux if that light is very faint (e.g., less than 1 % contribution in luminosity), because such faint third light will bring big errors to the light curve solutions.

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The asymptotic evolution of the stellar merger V1309 Sco: a Blue Straggler in the making?

Cited by 31 publications

References 37 publications

Photometric observations of an extreme mass ratio overcontact binary

Photometric observations of an extreme mass ratio overcontact binary

Two contact binaries with mass ratios close to the minimum mass ratio

Error Analysis of the Light Curve Solution of Contact Binaries Based on the W-D Code

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