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- KAISEY MANDEL, ERIC AGOL
- 2002

We present exact analytic formulae for the eclipse of a star described by quadratic or nonlinear limb darkening. In the limit that the planet radius is less than a tenth of the stellar radius, we show that the exact lightcurve can be well approximated by assuming the region of the star blocked by the planet has constant surface brightness. We apply these… (More)

- Heather A Knutson, David Charbonneau, +6 authors S Thomas Megeath
- Nature
- 2007

'Hot Jupiter' extrasolar planets are expected to be tidally locked because they are close (<0.05 astronomical units, where 1 au is the average Sun-Earth distance) to their parent stars, resulting in permanent daysides and nightsides. By observing systems where the planet and star periodically eclipse each other, several groups have been able to estimate the… (More)

- Eric Agol, Jason Steffen, Re’em Sari, Will Clarkson
- 2005

The transits of a planet on a Keplerian orbit occur at time intervals exactly equal to the period of the orbit. If a second planet is introduced the orbit is not Keplerian and the transits are no longer exactly periodic. We compute the magnitude of these variations in the timing of the transits, δt. We investigate analytically several limiting cases: (i)… (More)

- ERIC AGOL
- 2002

Occultation and microlensing are different limits of the same phenomena of one body passing in front of another body. We derive a general exact analytic expression which describes both microlensing and occultation in the case of spherical bodies with a source of uniform brightness and a non-relativistic foreground body. We also compute numerically the case… (More)

- William J Borucki, Eric Agol, +62 authors Joshua N Winn
- Science
- 2013

We present the detection of five planets--Kepler-62b, c, d, e, and f--of size 1.31, 0.54, 1.95, 1.61 and 1.41 Earth radii (R⊕), orbiting a K2V star at periods of 5.7, 12.4, 18.2, 122.4, and 267.3 days, respectively. The outermost planets, Kepler-62e and -62f, are super-Earth-size (1.25 R⊕ < planet radius ≤ 2.0 R⊕) planets in the habitable zone of their host… (More)

- Heather A. Knutson, Nikku Madhusudhan, +10 authors Sara Seager
- 2011

In this paper, we describe a uniform analysis of eight transits and eleven secondary eclipses of the extrasolar planet GJ 436b obtained in the 3.6, 4.5, and 8.0 μm bands using the IRAC instrument on the Spitzer Space Telescope between UT 2007 June 29 and UT 2009 February 4. We find that the best-fit transit depths for visits in the same bandpass can vary by… (More)

We make predictions for the rate of discovery of eclipsing white dwarf–main sequence (WD–MS) binaries in terrestrial-planet transit searches, taking the planned Kepler and Eddington missions as examples. We use a population synthesis model to characterize the Galactic WD–MS population, and we find that, despite increased noise due to stellar variability… (More)

- ERIC AGOL
- 2003

We prove a gravitational lensing theorem: the magnification of a source of uniform brightness by a foreground spherical lens is µ = 1 + π(2R 2 E − R 2 L)/A, where A is the area of the source and R E and R L are the Einstein radius and size of the lens projected into the source plane; this provides an accurate approximation to the exact magnification for R 2… (More)

- Daniel J Eisenstein, David H Weinberg, +314 authors Bo Zhao
- 2013

The Open University's repository of research publications and other research outputs SDSS-III: massive spectroscopic surveys of the distant universe, the Milky Way, and extra-solar planetary systems Journal Article Eisenstein et al. ABSTRACT Building on the legacy of the Sloan Digital Sky Survey (SDSS-I and II), SDSS-III is a program of four spectroscopic… (More)

- Thomas Barclay, Jason F Rowe, +55 authors Susan E Thompson
- Nature
- 2013

Since the discovery of the first exoplanets, it has been known that other planetary systems can look quite unlike our own. Until fairly recently, we have been able to probe only the upper range of the planet size distribution, and, since last year, to detect planets that are the size of Earth or somewhat smaller. Hitherto, no planets have been found that… (More)