Transit of Mercury

On May 9, 2016, the planet Mercury will transit across the face of the Sun and for most of the Earth, the transit will be visible (or at least portions of it).


The transit begins at 11:12 UTC (Coordinated Universal Time measured at Greenwich, England) and ends at 18:42 UTC. To determine your time offset from UTC, Wikipedia has a good summary. For example, in Pittsburgh (where I live), we are currently only four hours behind UTC due to daylight savings time. So in Pittsburgh, the transit begins at 7:12 AM and ends at 2:42 PM.


To see the transit, you should not look directly at the Sun.. There are a couple of ways to look at it, however.

1. Have a Sun filter for a telescope, binoculars, or camera.
2. Watch it online at NASA.gov.

If you recall (or even if you don't), a transit is similar to an eclipse and an occultation. A transit is when a planet crosses in front of its parent star as seen from Earth. On Earth, only Mercury and Venus can transit the Sun. Unfortunately, many of us alive today will never witness another transit of Venus, as the last two took place in June of 2004 and June of 2012. The next transit of Venus will not take place until December of 2117. Mercury has a much shorter period of transits, approximately every three years, so if you miss this transit, you will only have to wait until November 2019.

Syzygy

In astronomy, objects can always cross in front of another object, if the alignments are right. They are usually referred to one of three terms: an eclipse, a transit, or an occultation. These three terms are part of a broader definition called a syzygy*.


   *Syzygy in astronomy is when three bodies are in a line.





Let's define the three of them.





Previously, I posted about eclipses of the Moon. These occur when the Moon, Sun, and the Earth are lined up in such a way that the Moon eclipses the Sun (a total solar eclipse), or the Moon goes through the Earth's shadow (a lunar eclipse). An eclipse can also happen in multiple star systems when one companion star passes in front of the other. What occurs is that the obscured body is either completed blocked out temporarily as it passes through the shadow of the eclipsing body (lunar eclipse) or the eclipsing body passes between the observer and the eclipsed object (total solar eclipse).





A transit is when a smaller body passes in front of a larger body, mostly a planet crossing in front of a star, but can also occur when a moon crosses in front of a planet, partially blocking out the Sun. Transits of extra-solar planets can be used to help astronomers find the planet and determine its size based on the light-curve of the star. Exoplanet transits are discussed more here. Transits occur in the inner solar system when Mercury and Venus cross in front of the Sun as seen from Earth. On my post about opposition and conjunction, what configuration(s) are Mercury and Venus in when they transit the Sun? Comment below if you know the answer. Also, the moons of Jupiter and Saturn can also transit across the face of their parent planets.

Released with Image The Galilean satellite Io floats above the cloudtops of Jupiter in this image captured on the dawn of the new millennium, January 1, 2001 10:00 UTC (spacecraft time), two days after Cassini's closest approach. The image is deceiving: there are 350,000 kilometers -- roughly 2.5 Jupiters -- between Io and Jupiter's clouds. Io is the size of our Moon, and Jupiter is very big.

Via NASA/JPL/University of Arizona

 

The last example of syzygy in astronomy is called occultation. In this case, the body that crosses between the observer and the more distant object appears much larger. These occur when the Moon, the Sun, or a planet pass in front of distant star, when the Moon passes in front of a planet, or when the satellite of a planet passes in front of an apparently smaller satellite.

Dione occulting Rhea (two moons of Saturn)

via NASA/Cassini-Huygens Mission

 

In picture form, this is what the three types of syzygy look like:

Extra-Solar Planets

For thousands of years, what humans knew of planets consisted of only six objects: Mercury, Venus, Earth, Mars, Jupiter and Saturn. The discoveries of Uranus, Neptune, and Pluto raised that number to nine (until Pluto was demoted). Then in the 1990s, we had an explosion of knowledge: exoplanets.

What is an exoplanet? Exoplanets, sometimes called extra-solar planets, are planets found to be orbiting around stars other than the Sun. They are extremely dim compared to their parent star so can only be inferred by the gravitational influence they exert on their star or the minute dimming of the star as the planet crosses in front.

The first way that a planet can be discovered is if the planetary orbit lies along our line of sight, we use the radial velocity method. Remember that the radial velocity of a star can cause the spectrum of the star shift either to the blue end of the spectrum (blue-shift) or the red end of the spectrum (red-shift). How does this work with a planet orbiting the star?

As seen in the above drawing, if the planet is between the star and us, the planet's small but measurable gravity will pull the star towards us, and we can observe the spectrum of the star to be minutely blue-shifted. If the star is between us and the planet, the planet will pull the star away from us, and the spectrum is red-shifted. Granted, these shifts in either direction are small, but can be measured. From the measurement, the radial velocity on the star can be calculated, and a mass of the planet can be inferred, as well as an idea of the planet's distance from the star.

Another way to determine if there is a planet is orbiting a star is to use astrometry and proper motion. If the orbit of the planet is across our line of sight (i.e. we are looking straight down on the pole of th orbit, this method works best.

In both these cases, the planet pulls the star slightly towards itself and even though the actual motion of the star is small, they can be measured. There are a couple of biases when using these methods including the larger the planetary mass or the closer the planet is to the star, the more the pull that can be observed. This is why when exoplanets were first discovered, they were biased towards what were referred to as hot Jupiters, i.e. large planets close to the parent star. As methods and observational protocols improved, smaller planets and planets farther from the central star began to be discovered.

There are also caveats to finding planets in these ways.

1.      In all likelihood, finding planets that are orbiting along our line of sight, or orbiting across our line of sight are statistically improbable.

2.      Using either method will only give the astronomer a minimum mass of the star.

The radial velocity will only find the velocity that is along our line of sight, i.e. V*sin(i). This will give the mass of the star as M*sin(i). The symbol i is the inclination of the orbit to an orbit across our line of sight. If i is 90°, the orbit lies along our line of sight and sin(i) is 1. The astrometric method will find V*cos(i) and in the same way, the mass of the star as M*cos(i). Combining these two methods will give a pretty good estimate of the planet's mass. However, using astrometry is much more difficult as the angles measured are extremely tiny compared to the actual parallax of the star. Not many planets have been found this way, if any at all.

There is a third way astronomers use to find planets: the transit method, i.e. the planet crossing in front of a star. An astronomer will look at the light-curve* of the star and look for a dip in the intensity of the light.

• Light-curve is the measure of a star's intensity over time. Most stars have a uniform light curve with slight bumps in the curve. Others can vary over time and are called variable stars. More on variable stars later.

Since the planet is so much smaller than the star, the dip is generally tiny and are hard to see in a light-curve because of noise. But if one is found and by looking at how long the dip lasts, astronomers can get an idea of the planet's mass and orbital distance from the star. However, this method is strongly biased towards orbits that are along our line of sight, and cannot be used for orbits that are across our line of sight.

 

Graphic of a Planet transiting its parent star with light curve

Image Credit:

NASA

 

There is a great website that has a lot of information about exoplanets called exoplanets.org. This website has information on all "confirmed" exoplanets from the above methods as well as unconfirmed planets using the Kepler telescope. The Kepler telescope unfortunately does not look at the entire sky, but only a small patch in the constellation Cygnus. Future missions may look at more of the sky and the number of planets discovered will skyrocket.