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The Solar-Type Contact Binary BX Pegasi Revisited
Solar and Stellar Astrophysics · Submitted 20 Oct 2009
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The complex period changes of BX Peg can be sorted into a secular period decrease caused dominantly by angular momentum loss due to magnetic stellar wind braking, a light-travel-time (LTT) effect due to the orbit of a low-mass third companion, and a previously unknown short-term oscillation.
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The abstract, sentence by sentence
We present the results of new CCD photometry for the contact binary BX Peg, made during three successive months beginning on September 2008. As do historical light curves, our observations display an O'Connell effect and the November data by themselves indicate clear evidence for very short-time brightness disturbance. For these variations, model spots are applied separately to the two data set of Group I (Sep.--Oct.) and Group II (Nov.). The former is described by a single cool spot on the secondary photosphere and the latter by a two-spot model with a cool spot on the cool star and a hot one on either star. These are generalized manifestations of the magnetic activity of the binary system. Twenty light-curve timings calculated from Wilson-Devinney code were used for a period study, together with all other minimum epochs. The complex period changes of BX Peg can be sorted into a secular period decrease caused dominantly by angular momentum loss due to magnetic stellar wind braking, a light-travel-time (LTT) effect due to the orbit of a low-mass third companion, and a previously unknown short-term oscillation. This last period modulation could be produced either by a second LTT orbit with a period of about 16 yr due to the existence of a fourth body or by the effect of magnetic activity with a cycle length of about 12 yr.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present the results of new CCD photometry for the contact binary BX Peg, made during three successive months beginning on September 2008. | contribution 0.67 | 0.97 | 0.02 | asserted 0.99 |
| s1 | As do historical light curves, our observations display an O'Connell effect and the November data by themselves indicate clear evidence for very short-time brightness disturbance. | result 1.00 | 0.88 | 0.06 | asserted 0.78 |
| s2 | For these variations, model spots are applied separately to the two data set of Group I (Sep.--Oct.) and Group II (Nov.). | method 0.98 | 0.86 | 0.03 | asserted 0.98 |
| s3 | The former is described by a single cool spot on the secondary photosphere and the latter by a two-spot model with a cool spot on the cool star and a hot one on either star. | result 0.73 | 0.88 | 0.05 | asserted 1.00 |
| s4 | These are generalized manifestations of the magnetic activity of the binary system. | interpretation 1.00 | 0.41 | 0.06 | asserted 1.00 |
| s5 | Twenty light-curve timings calculated from Wilson-Devinney code were used for a period study, together with all other minimum epochs. | method 0.99 | 0.90 | 0.03 | asserted 0.98 |
| s6 | The complex period changes of BX Peg can be sorted into a secular period decrease caused dominantly by angular momentum loss due to magnetic stellar wind braking, a light-travel-time (LTT) effect due to the orbit of a low-mass third companion, and a previously unknown short-term oscillation. | result 0.71 | 0.89 | 0.60 | asserted 1.00 |
| s7 | This last period modulation could be produced either by a second LTT orbit with a period of about 16 yr due to the existence of a fourth body or by the effect of magnetic activity with a cycle length of about 12 yr. | interpretation 0.99 | 0.69 | 0.14 | hedged possibility 0.99 |
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Original abstract
We present the results of new CCD photometry for the contact binary BX Peg, made during three successive months beginning on September 2008. As do historical light curves, our observations display an O'Connell effect and the November data by themselves indicate clear evidence for very short-time brightness disturbance. For these variations, model spots are applied separately to the two data set of Group I (Sep.--Oct.) and Group II (Nov.). The former is described by a single cool spot on the secondary photosphere and the latter by a two-spot model with a cool spot on the cool star and a hot one on either star. These are generalized manifestations of the magnetic activity of the binary system. Twenty light-curve timings calculated from Wilson-Devinney code were used for a period study, together with all other minimum epochs. The complex period changes of BX Peg can be sorted into a secular period decrease caused dominantly by angular momentum loss due to magnetic stellar wind braking, a light-travel-time (LTT) effect due to the orbit of a low-mass third companion, and a previously unknown short-term oscillation. This last period modulation could be produced either by a second LTT orbit with a period of about 16 yr due to the existence of a fourth body or by the effect of magnetic activity with a cycle length of about 12 yr.
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