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Ge/Ay133

What (exo)-planetary science can be done with microlensing?. Ge/Ay133. Other routes to Earth-like planets?. α = 4GM/bc 2. b. Microlensing example:. Microlensing example:. Best geometry uses stars at a few kpc (the lens) against the Galactic Bulge (light source).

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Ge/Ay133

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  1. What (exo)-planetary science can be done with microlensing? Ge/Ay133

  2. Other routes to Earth-like planets? α = 4GM/bc2 b

  3. Microlensing example:

  4. Microlensing example:

  5. Best geometry uses stars at a few kpc (the lens) against the Galactic Bulge (light source). 5.5 MEarth planet at 2.6 AU around a M-dwarf (0.22 M) primary at 6.6 ± 1.0 kpc. J.-P. Beaulieu et al. Nature 439, 437-440 (26Jan2006)

  6. Magnification map of the lensing system in OGLE 2003-BLG-235/MOA 2003-BLG-53. Biggest perturbation when planet is near Einstein ring AND the location of the background stellar image (so, some/ many planets missed). I.A. Bond et al. 2004, ApJ, 606, L155

  7. OGLE 2003-BLG-235/MOA 2003-BLG-53 Animations: I.A. Bond et al. 2004, ApJ, 606, L155

  8. Are there Earth-like planets beyond the snow-line?

  9. Something like ten systems so far, +’s/-’s ? Advantages of the microlensing technique to detect exoplanets include: * More sensitive than most other techniques to small-mass planets (like Earth) * Most sensitive to planets in our Galaxy that have orbit sizes of a few astronomical units (like those of Mars or Jupiter) * Only method capable of detecting planets in other galaxies * The most common stars in the Galaxy will be the most likely lenses * Capable of detecting (with some probability) multiple planets in a single lightcurve. In summary, the microlensing can be used to study the statistical abundance of exoplanets in our Galaxy with properties similar to the planets in our own Solar System.

  10. Something like ten systems so far, +’s/-’s ? Disadvantages of the microlensing technique to detect exoplanets include: * Millions of stars must be monitored to find the few that are microlensing at any given time * Planetary deviations in lightcurve are short-lived and could be missed due to inopportune timing * Substantial probability that any planet will not be detected in lens system, even if present * Deviations in microlensing lightcurves due to planets will not repeat (as they are due to a chance alignment) * Planetary parameters (such as mass, orbit size, etc) depend on the properties of the host star, which are typically unknown In sum, the microlensing technique requires intensive use of telescope time, and is unsuitable for continued detailed study of individual exoplanets.

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