Stellar Limb Darkening’s Effects on Exoplanet Characterization

Csizmadia, Szilárd

doi:10.1007/978-3-319-30648-3_41-1

Cited by 1 publication

(2 citation statements)

References 43 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Given these assumptions, generally one next assumes a particular functional form for the limb darkening law (Csizmadia 2018). The parameterization of the limb darkening model can impact the precision of the computation of transit light curves.…”

Section: Discussionmentioning

confidence: 99%

“…And yet, all of these inferences are predicated on the precise computation of models of the planetary transit which may be used to infer the model parameters. Stars are non-uniform in brightness, with the general trend of growing dimmer towards the limb, and so limb darkening must be accounted for to accurately infer the planetary parameters (Csizmadia 2018). Indeed, fast and accurate computation of limb-darkened transit light curve models has enabled the detection and characterization of thousands of transiting exoplanets (Mandel & Agol 2002).…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Analytic Planetary Transit Light Curves and Derivatives for Stars with Polynomial Limb Darkening

2020

View full text Add to dashboard Cite

We derive analytic, closed-form solutions for the light curve of a planet transiting a star with a limb darkening profile which is a polynomial function of the stellar elevation, up to arbitrary integer order. We provide improved analytic expressions for the uniform, linear, and quadratic limb-darkened cases, as well as novel expressions for higher order integer powers of limb darkening. The formulae are crafted to be numerically stable over the expected range of usage. We additionally present analytic formulae for the partial derivatives of instantaneous flux with respect to the radius ratio, impact parameter, and limb darkening coefficients. These expressions are rapid to evaluate, and compare quite favorably in speed and accuracy to existing transit light curve codes. We also use these expressions to numerically compute the first partial derivatives of exposure-time averaged transit light curves with respect to all model parameters. An additional application is modeling eclipsing binary or eclipsing multiple star systems in cases where the stars may be treated as spherically symmetric. We provide code which implements these formulae in C++, Python, IDL, and Julia, with tests and examples of usage.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%