Fast and precise light-curve model for transiting exoplanets with rings

Rein, Edan

doi:10.1093/mnras/stz2556

Cited by 13 publications

(9 citation statements)

References 33 publications

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“…Several well-known packages have been developed in recent years (see e.g. Kreidberg 2015;Lightkurve Collaboration et al 2018;Akinsanmi et al 2018;Rein and Ofir 2019), and most of them implement the experience accumulated in 20 years of transit observations and research. Those packages focus on two special features: precision and performance.…”

Section: Validation Against Other Transit Packagesmentioning

confidence: 99%

The bright side of the light curve: a general photometric model of non-transiting exorings

Zuluaga,

Sucerquia,

Alvarado-Montes

2022

Preprint

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Rings around exoplanets (exorings) are one of the most expected discoveries in exoplanetary research. There is an increasing number of theoretical and observational efforts for detecting exorings, but none of them have succeeded yet. Most of those methods focus on the photometric signatures of exorings during transits, whereas less attention has been paid to light diffusely reflected: what we denote here as the bright side of the light curve. This is particularly important when we cannot detect the typical stellar flux drop produced by transiting exoplanets. Here, we endeavour to develop a general method to model the variations on the light curves of both ringed non-transiting and transiting exoplanets. Our model (dubbed as Pryngles) simulates the complex interaction of luminous, opaque, and semitransparent objects in planetary systems, discretizing their surface with small circular plane discs that resemble sequins or spangles. We perform several numerical experiments with this model, and show its incredible potential to describe the light curve of complex systems under various orbital, planetary, and observational configurations of planets, moons, rings, or discs. As our model uses a very general approach, we can capture effects like shadows or planetary/ring shine, and since the model is also modular we can easily integrate arbitrarily complex physics of planetary light scattering. A comparison against existing tools and analytical models of reflected light reveals that our model, despite its novel features, reliably reproduces light curves under common circumstances. Pryngles source code is written in Python and made publicly available.

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Section: Validation Against Other Transit Packagesmentioning

confidence: 99%

The bright side of the light curve: a general photometric model of non-transiting exorings

Zuluaga,

Sucerquia,

Alvarado-Montes

2022

Preprint

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“…To perform the modelling of the elliptical occulter we use a modified version of the pyPplusS code developed by Rein & Ofir (2019). This code produces light curves in physical space, i.e.…”

Section: Eclipse Fittingmentioning

confidence: 99%

An Asymmetric Eclipse Seen Towards the Pre-Main Sequence Binary System V928 Tau

van Dam,

Kenworthy,

David

et al. 2020

Preprint

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K2 observations of the weak-lined T Tauri binary V928 Tau A+B show the detection of a single, asymmetric eclipse which may be due to a previously unknown substellar companion eclipsing one component of the binary with an orbital period > 66 days. Over an interval of about 9 hours, one component of the binary dims by around 60%, returning to its normal brightness about 5 hours later. From modeling of the eclipse shape we find evidence that the eclipsing companion may be surrounded by a disk or a vast ring system. The modeled disk has a radius of 0.9923 ± 0.0005 R * , with an inclination of 56.78 ± 0.03 • , a tilt of 41.22 ± 0.05 • , an impact parameter of −0.2506 ± 0.0002 R * and an opacity of 1.00. The occulting disk must also move at a transverse velocity of 6.637 ± 0.002 R * day −1 , which depending on whether it orbits V928 Tau A or B, corresponds to approximately 73.53 or 69.26 km s −1 . A search in ground based archival data reveals additional dimming events, some of which suggest periodicity, but no unambiguous period associated with the eclipse observed by K2. We present a new epoch of astrometry which is used to further refine the orbit of the binary, presenting a new lower bound of 67 years, and constraints on the possible orbital periods of the eclipsing companion. The binary is also separated by 18 (∼2250 au) from the lower mass CFHT-BD-Tau 7, which is likely associated with V928 Tau A+B. We also present new high dispersion optical spectroscopy that we use to characterize the unresolved stellar binary.

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“…To perform the modeling of the elliptical occulter, we use a modified version of the pyPplusS code developed by Rein & Ofir (2019). This code produces light curves in physical space, i.e., it determines the eclipse depth based on the physical area that has been blocked by the occulter (which can be a planet, disk, or planet disk/ring system combination of which we use the disk model).…”

Section: Eclipse Fittingmentioning

confidence: 99%

An Asymmetric Eclipse Seen toward the Pre-main-sequence Binary System V928 Tau

Dam

Kenworthy

Mamajek

et al. 2020

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K2 observations of the weak-lined T Tauri binary V928 Tau A and B show the detection of a single, asymmetric eclipse, which may be due to a previously unknown substellar companion eclipsing one component of the binary with an orbital period >66 days. Over an interval of about 9 hr, one component of the binary dims by around 60%, returning to its normal brightness about 5 hr later. From modeling of the eclipse shape, we find evidence that the eclipsing companion may be surrounded by a disk or a vast ring system. The modeled disk has a radius of 0.9923±0.0005 R * , with an inclination of 56°.78±0°. 03, a tilt of 41°.22±0°. 05, an impact parameter of −0.2506±0.0002 R * , and an opacity of 1.00. The occulting disk must also move at a transverse velocity of 6.637±0.002 R * day −1 , which, depending on whether it orbits V928 Tau A or B, corresponds to approximately 73.53 or 69.26 km s −1. A search in ground-based archival data reveals additional dimming events, some of which suggest periodicity, but no unambiguous period associated with the eclipse observed by K2. We present a new epoch of astrometry that is used to further refine the orbit of the binary, presenting a new lower bound of 67 yr, and constraints on the possible orbital periods of the eclipsing companion. The binary is also separated by 18″ (∼2250 au) from the lower-mass CFHT-BD-Tau 7, which is likely associated with V928 Tau A and B. We also present new high-dispersion optical spectroscopy that we use to characterize the unresolved stellar binary.

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Fast and precise light-curve model for transiting exoplanets with rings

Cited by 13 publications

References 33 publications

The bright side of the light curve: a general photometric model of non-transiting exorings

The bright side of the light curve: a general photometric model of non-transiting exorings

An Asymmetric Eclipse Seen Towards the Pre-Main Sequence Binary System V928 Tau

An Asymmetric Eclipse Seen toward the Pre-main-sequence Binary System V928 Tau

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