Kepler: a space mission to detect earth-class exoplanets

Koch, David; Borucki, W. J.; Webster, L. D.; Dunham, E. W.; Jenkins, Jon M.; Marriott, John; Reitsema, H. J.

doi:10.1117/12.324482

Cited by 56 publications

(23 citation statements)

References 18 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Farmer, E. Agol, & S. Wyithe (2002, in preparation) apply the formulae derived here to estimate how many white dwarfs can be found in transit searches for extrasolar planets. For example, the Kepler survey (Koch et al 1998) may find $10-100 white dwarfs, comparable to the expected number of terrestrial planets. White dwarf transit events require the inclusion of both lensing and occultation in modeling the light curves.…”

Section: Discussionmentioning

confidence: 99%

Occultation and Microlensing

Agol

2002

ApJ

View full text Add to dashboard Cite

Occultation and microlensing are different limits of the same phenomenon of one body passing in front of another body. We derive a general exact analytic expression that describes both microlensing and occultation in the case of spherical bodies with a source of uniform brightness and a nonrelativistic foreground body. We also numerically compute the case of a source with quadratic limb darkening. In the limit that the gravitational deflection angle is comparable to the angular size of the foreground body, both microlensing and occultation occur as the objects align. Such events can be used to constrain the size ratio of the lens and source stars, the limb-darkening coefficients of the source star, and the surface gravity of the lens star (if the lens and source distances are known). Application of these results to microlensing during transits in binaries and giant-star microlensing is discussed. These results unify the microlensing and occultation limits and should be useful for rapid model fitting of microlensing, eclipse, and '' micro-occultation '' events.

show abstract

Section: Discussionmentioning

confidence: 99%

Occultation and Microlensing

Agol

2002

ApJ

View full text Add to dashboard Cite

show abstract

“…The chosen parameters reflect the quantities typically extracted 7 from stars in the Kepler (Koch et al 2004;Borucki et al 2010) field. Our analysis focuses on the truncated grid of models 8 (see §3).…”

Section: Explained Variance Of the Principle Componentsmentioning

confidence: 99%

On the Statistical Properties of the Lower Main Sequence

Angelou

Bellinger

Hekker

et al. 2017

ApJ

View full text Add to dashboard Cite

Astronomy is in an era where all-sky surveys are mapping the Galaxy. The plethora of photometric, spectroscopic, asteroseismic and astrometric data allows us to characterise the comprising stars in detail. Here we quantify to what extent precise stellar observations reveal information about the properties of a star, including properties that are unobserved, or even unobservable. We analyse the diagnostic potential of classical and asteroseismic observations for inferring stellar parameters such as age, mass and radius from evolutionary tracks of solar-like oscillators on the lower main sequence. We perform rank correlation tests in order to determine the capacity of each observable quantity to probe structural components of stars and infer their evolutionary histories. We also analyse the principal components of classic and asteroseismic observables to highlight the degree of redundancy present in the measured quantities and demonstrate the extent to which information of the model parameters can be extracted. We perform multiple regression using combinations of observable quantities in a grid of evolutionary simulations and appraise the predictive utility of each combination in determining the properties of stars. We identify the combinations that are useful and provide limits to where each type of observable quantity can reveal information about a star. We investigate the accuracy with which targets in the upcoming TESS and PLATO missions can be characterized. We demonstrate that the combination of observations from GAIA and PLATO will allow us to tightly constrain stellar masses, ages and radii with machine learning for the purposes of Galactic and planetary studies.

show abstract

“…Such events are easily observed from the ground using telescopes of modest aperture (Henry et al 2000;Seagroves et al 2003). The forthcoming Kepler mission (Koch et al 1998) will monitor ∼3600 M dwarf stars with m V < 16 over its 4-year lifetime, and will easily detect transits of objects of Earth size or larger in orbit around M dwarf stars. Assuming that icy core masses of M ∼ 1M ⊕ can accrete at a ∼ 1 AU, the Kepler sample size will be large enough to provide a statistical test of our hypothesis.…”

Section: Potential Observational Testsmentioning

confidence: 99%

M dwarfs: planet formation and long term evolution

Adams¹,

Bodenheimer

Laughlin

2005

Astron Nachr

View full text Add to dashboard Cite

Abstract. The first part of this paper discusses how planet formation proceeds in the disks orbiting M dwarf stars. These environments are different from those associated with solar-type stars in several ways: The planet forming clock (set by orbits) runs slower, the disks are more prone to evaporation, the supply of raw material is lower, the snowline is closer in, and planetary systems are more easily disrupted. Because of these considerations, red dwarfs are less likely to harbor giant planets, but can readily produce smaller planets. The second part of this paper describes stellar evolution calculations for M dwarfs, which live far longer than the current age of the universe. These diminutive stellar objects remain convective over most of their lives, continue to burn hydrogen for trillions of years, and do not experience red giant phases in their old age. Instead, red dwarfs turn into blue dwarfs and finally white dwarfs. This work also shows (in part) why larger stars become red giants.

show abstract

Kepler: a space mission to detect earth-class exoplanets

Cited by 56 publications

References 18 publications

Occultation and Microlensing

Occultation and Microlensing

On the Statistical Properties of the Lower Main Sequence

M dwarfs: planet formation and long term evolution

Contact Info

Product

Resources

About