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The Kepler Eclipsing System KIC 5621294 and its Substellar Companion
Solar and Stellar Astrophysics · Submitted 23 Dec 2014
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The sinusoidal variation with a period of 961 d and a semi-amplitude of 22.5 s most likely arise from a light-time effect due to a third component with a mass of $M_3 \sin i_3$=46.9 M$\rm_{Jup}$, which is in good agreement with that calculated from the light curve itself.
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The abstract, sentence by sentence
We present the physical properties of KIC 5621294 showing light and timing variations from the ${\it Kepler}$ photometry. Its light curve displays partial eclipses and O'Connell effect with Max II fainter than Max I, which was fitted quite well by applying third-body and spot effects to the system. The results indicate that the eclipsing pair is a classical Algol-type system with parameters of $q$=0.22, $i$=76$^\circ$.8, and $\Delta$($T_{1}$--$T_{2}$)=4,235 K, in which the detached primary component fills about 77\% of its limiting lobe. Striking discrepancies exist between the primary and secondary eclipse times obtained with the method of Kwee \& van Woerden. These are mainly caused by surface inhomogeneities due to spot activity detected in our light-curve synthesis. The 1,253 light-curve timings from the Wilson-Devinney code were used for a period study. It was found that the orbital period of KIC 5621294 has varied due to a periodic variation overlaid on a downward parabola. The sinusoidal variation with a period of 961 d and a semi-amplitude of 22.5 s most likely arise from a light-time effect due to a third component with a mass of $M_3 \sin i_3$=46.9 M$\rm_{Jup}$, which is in good agreement with that calculated from the light curve itself. If its orbital inclination is larger than about 40$^\circ$, the mass of the circumbinary object would possibly match a brown dwarf. The parabolic variation could not be fully explained by either a mass transfer between the binary components or an angular momentum via magnetic braking. It is possible that the parabola may only be the observed part of a period modulation caused by the presence of another companion in a wider orbit.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present the physical properties of KIC 5621294 showing light and timing variations from the ${\it Kepler}$ photometry. | contribution 1.00 | 0.94 | 0.09 | asserted 1.00 |
| s1 | Its light curve displays partial eclipses and O'Connell effect with Max II fainter than Max I, which was fitted quite well by applying third-body and spot effects to the system. | result 0.95 | 0.87 | 0.08 | asserted 1.00 |
| s2 | The results indicate that the eclipsing pair is a classical Algol-type system with parameters of $q$=0.22, $i$=76$^\circ$.8, and $\Delta$($T_{1}$--$T_{2}$)=4,235 K, in which the detached primary component fills about 77\% of its limiting lobe. | result 0.97 | 0.91 | 0.19 | hedged possibility 0.51 |
| s3 | Striking discrepancies exist between the primary and secondary eclipse times obtained with the method of Kwee \& van Woerden. | result 1.00 | 0.86 | 0.05 | asserted 1.00 |
| s4 | These are mainly caused by surface inhomogeneities due to spot activity detected in our light-curve synthesis. | interpretation 0.93 | 0.93 | 0.06 | asserted 0.98 |
| s5 | The 1,253 light-curve timings from the Wilson-Devinney code were used for a period study. | method 0.99 | 0.88 | 0.03 | asserted 0.97 |
| s6 | It was found that the orbital period of KIC 5621294 has varied due to a periodic variation overlaid on a downward parabola. | result 1.00 | 0.95 | 0.15 | asserted 1.00 |
| s7 | The sinusoidal variation with a period of 961 d and a semi-amplitude of 22.5 s most likely arise from a light-time effect due to a third component with a mass of $M_3 \sin i_3$=46.9 M$\rm_{Jup}$, which is in good agreement with that calculated from the light curve itself. | result 0.67 | 0.93 | 0.31 | hedged possibility 0.99 |
| s8 | If its orbital inclination is larger than about 40$^\circ$, the mass of the circumbinary object would possibly match a brown dwarf. | interpretation 0.96 | 0.74 | 0.13 | hedged possibility 0.99 |
| s9 | The parabolic variation could not be fully explained by either a mass transfer between the binary components or an angular momentum via magnetic braking. | interpretation 0.72 | 0.84 | 0.08 | asserted 0.82 |
| s10 | It is possible that the parabola may only be the observed part of a period modulation caused by the presence of another companion in a wider orbit. | interpretation 1.00 | 0.56 | 0.14 | hedged possibility 0.97 |
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The paper
Original abstract
We present the physical properties of KIC 5621294 showing light and timing variations from the ${\it Kepler}$ photometry. Its light curve displays partial eclipses and O'Connell effect with Max II fainter than Max I, which was fitted quite well by applying third-body and spot effects to the system. The results indicate that the eclipsing pair is a classical Algol-type system with parameters of $q$=0.22, $i$=76$^\circ$.8, and $\Delta$($T_{1}$--$T_{2}$)=4,235 K, in which the detached primary component fills about 77\% of its limiting lobe. Striking discrepancies exist between the primary and secondary eclipse times obtained with the method of Kwee \& van Woerden. These are mainly caused by surface inhomogeneities due to spot activity detected in our light-curve synthesis. The 1,253 light-curve timings from the Wilson-Devinney code were used for a period study. It was found that the orbital period of KIC 5621294 has varied due to a periodic variation overlaid on a downward parabola. The sinusoidal variation with a period of 961 d and a semi-amplitude of 22.5 s most likely arise from a light-time effect due to a third component with a mass of $M_3 \sin i_3$=46.9 M$\rm_{Jup}$, which is in good agreement with that calculated from the light curve itself. If its orbital inclination is larger than about 40$^\circ$, the mass of the circumbinary object would possibly match a brown dwarf. The parabolic variation could not be fully explained by either a mass transfer between the binary components or an angular momentum via magnetic braking. It is possible that the parabola may only be the observed part of a period modulation caused by the presence of another companion in a wider orbit.
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