# Microlensing Light Curve for Stellar Objects

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Gravitational microlensing is a phenomenon in which a compact, massive foreground object (the lens) bends the light of a background object (the source, such as a star or galaxy) so that multiple images of the source can be seen. If the source travels close enough to the lens in the sky, there is a chance of observing a microlensing event, during which the brightness of the source, and therefore of the entire system, increases for a brief period. This interactive graph shows the light curve of such an event, based on various parameters of the system.

Contributed by: Bryan Brzycki (October 2015)

Open content licensed under CC BY-NC-SA

## Snapshots

## Details

The plot measures the change in brightness of the system as a function of time, where is the time of closest (projected) approach between the lens and the source objects. Specifically, equals the magnification of the source brightness; is the original brightness.

The quantity is the closest projected approach in the sky of the source to the lens, and is the relative angular motion of the source divided by an angle termed the Einstein ring radius. The other two values control the bounds of the graph; is the farthest time displayed in the positive and negative directions, and is the height of the graph.

The Einstein ring radius is defined to be the angular radius from the lens at which the image of the source would appear if the source and the lens were perfectly aligned along the line of sight. We define a function to be the angular distance between the source and the lens divided by (so that is dimensionless).

From the geometry of the situation, we can derive . But the magnification of the source brightness can be expressed as a function of , according to (see a longer explanation here). So, combining these expressions for and to give magnification as a function of time, we get the plot shown in the graphic.

Note that we can define a natural timescale , the time it takes the source to travel one Einstein radius, which makes . It turns out that the square of this timescale varies as the mass of the lens, and one can verify mathematically that increasing the mass of the lens ends up stretching the light curve horizontally. This effect can be seen by decreasing .

For some further reading, there is a broad overview of the math behind the light curve here.

References

[1] The Planetary Society. "Microlensing." (Oct 2, 2015) www.planetary.org/explore/space-topics/exoplanets/microlensing.html.

[2] P. Murdin, ed., "Microlensing," *Encyclopedia of Astronomy and Astrophysics*, Basingstoke, UK: Nature Publishing Group, 2001. www.astro.caltech.edu/~george/ay20/eaa-microlensing.pdf.

[3] Scholarpedia. "Microlensing Exoplanets." (Oct. 2, 2015) www.scholarpedia.org/article/Microlensing_exoplanets.

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