Gravitational microlensing of stars with transiting planets

Lewis, Geraint F.

doi:10.1051/0004-6361:20011446

Cited by 8 publications

(7 citation statements)

References 40 publications

(74 reference statements)

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“…Such an effect would be extremely pronounced and easily identified but no examples of a transiting system acting as a lens star are known to exist. Lewis (2001) estimate a very low probability, ∼ 10 −6 , of such an event being detected.…”

Section: A6) There Are No Background Luminous Objectsmentioning

confidence: 88%

The Transits of Extrasolar Planets with Moons

Kipping¹

2011

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I, David Mathew Kipping, confirm that the work presented in this thesis is my own.Where information has been derived from other sources, I confirm that this has been indicated in the thesis. AbstractThe search for extrasolar planets is strongly motivated by the goal of characterizing how frequent habitable worlds and life may be within the Galaxy. Whilst much effort has been spent on searching for Earth-like planets, large moons may also be common, temperate abodes for life as well. The methods to detect extrasolar moons, or "exomoons" are more subtle than their planetary counterparts and in this thesis I aim to provide a method to find such bodies in transiting systems, which offer the greatest potential for detection.Before one can search for the tiny perturbations to the planetary signal, an understanding of the planetary transit must be established. Therefore, in Chapters 3 to 5 I discuss the transit model and provide several new insights. Chapter 4 presents new analytic expressions for the times of transit minima and the transit duration, which will be critical in the later search for exomoons. Chapter 5 discusses two sources of distortion to the transit signal, namely blending (with a focus on the previously unconsidered self-blending scenario) and light curve smearing due to long integration times. I provide methods to compensate for both of these effects, thus permitting for the accurate modelling of the planetary transit light curve.In Chapter 6, I discuss methods to detect exomoons through their gravitational influence on the host planet, giving rise to transit timing and duration variations (TTV and TDV). The previously known TTV effect is updated with a new model and the associated critical problems are outlined. I then predict a new effect, TDV, which solves these problems, making exomoon detection viable. Chapter 7 presents a feasibility study for detecting habitable-zone exomoons with Kepler, where it is found that moons down to 0.2 M ⊕ are detectable. Finally, conclusions and future work are discussed in Chapter 8.

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Section: A6) There Are No Background Luminous Objectsmentioning

confidence: 88%

The Transits of Extrasolar Planets with Moons

Kipping¹

2011

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“…This convention provides names for multiple components of the source star system. For example, OGLE-2022-BLG-876Sb would refer to a planetary companion to the source star (which would be difficult, but not impossible (Graff & Gaudi, 2000;Lewis, 2001)to detect. It is interesting to note that this event was discovered by a procedure that differs from both the alert-plus-followup strategy suggested by Gould & Loeb (1992) and the high magnification strategy suggested by Griest & Safizadeh (1998).…”

Section: Microlensing Planet Detectionsmentioning

confidence: 99%

Detection of Extrasolar Planets by Gravitational Microlensing

Bennett

Exoplanets

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Gravitational microlensing provides a unique window on the properties and prevalence of extrasolar planetary systems because of its ability to find low-mass planets at separations of a few AU. The early evidence from microlensing indicates that the most common type of exoplanet yet detected are the so-called "super-Earth" planets of ~10 Earth-masses at a separation of a few AU from their host stars. The detection of two such planets indicates that roughly one third of stars have such planets in the separation range 1.5-4 AU, which is about an order of magnitude larger than the prevalence of gas-giant planets at these separations. We review the basic physics of the microlensing method, and show why this method allows the detection of Earth-mass planets at separations of 2-3 AU with ground-based observations. We explore the conditions that allow the detection of the planetary host stars and allow measurement of planetary orbital parameters. Finally, we show that a low-cost, space-based microlensing survey can provide a comprehensive statistical census of extrasolar planetary systems with sensitivity down to 0.1 Earth-masses at separations ranging from 0.5 AU to infinity.Comment: 43 pages. Very similar to chapter 3 of Exoplanets: Detection, Formation, Properties, Habitability, John Mason, ed. Springer (April 3, 2008

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“…Transiting Source Stars: If the planet transits the source star, we can also simultaneously observe the transiting signal during the microlensing event (Lewis 2001;Rybicki & Wyrzykowski 2014). Typical amplitudes of the transit signal for Jupiter-size planet would be ∼ 1% of the source brightness, which will be easily detectable for most xallarap planetary events.…”

Section: How To Distinguish Lens Orbital Motionmentioning

confidence: 99%

Revealing Short-period Exoplanets and Brown Dwarfs in the Galactic Bulge using the Microlensing Xallarap Effect with the \textit{Nancy Grace Roman Space Telescope}

Miyazaki,

Johnson,

Sumi

et al. 2020

Preprint

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The Nancy Grace Roman Space Telescope (Roman) will provide an enormous number of microlensing light curves with much better photometric precisions than ongoing ground-based observations. Such light curves will enable us to observe high-order microlensing effects which have been previously difficult to detect. In this paper, we investigate Roman's potential to detect and characterize short-period planets and brown dwarfs (BDs) in source systems using the orbital motion of source stars, the socalled xallarap effect. We analytically estimate the measurement uncertainties of xallarap parameters using the Fisher matrix analysis. We show that the Roman Galactic Exoplanet Survey (RGES) can detect warm Jupiters with masses down to 0.5 M Jup and orbital period of 30 days via the xallarap effect. Assuming a planetary frequency function from Cumming et al. (2008), we find Roman will detect ∼ 10 hot and warm Jupiters and ∼ 30 close-in BDs around microlensed source stars during the microlensing survey. These detections are likely to be accompanied by the measurements of the companion's masses and orbital elements, which will aid in the study of the physical properties for close-in planet and BD populations in the Galactic bulge.

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Gravitational microlensing of stars with transiting planets

Cited by 8 publications

References 40 publications

The Transits of Extrasolar Planets with Moons

The Transits of Extrasolar Planets with Moons

Detection of Extrasolar Planets by Gravitational Microlensing

Revealing Short-period Exoplanets and Brown Dwarfs in the Galactic Bulge using the Microlensing Xallarap Effect with the \textit{Nancy Grace Roman Space Telescope}

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