1. The Transit Method
When a planet crosses in front of its star as viewed by an observer, the event is called a transit. Transits produce a very small change in a stars brightness.
If this change is caused by a planet it must be periodic and each transit must have the same change in brightness.
The transit method can be used to gain information about the planet as well as just detecting it. The planet’s size, transit time and radius of the orbit can all be determined from the data collected.

2. Transit Method
It is possible to study the atmosphere of the transiting planet.
When the planet transits the star, light from the star passes through the planets atmosphere.
By studying the high resolution stellar spectrum carefully, you can deduce what elements are present in the planet’s atmosphere (by spectroscopy of absorption lines from its atmosphere while it is transiting) and check it for indicators of life - such as the presence of free oxygen in the atmosphere.-

3. The main disadvantage of the transit method is that for us to detect a planet, the orbit must be precisely aligned with our point of view.

4. We used reference stars so we can capture the “noise”(darks, flats, biases)and subtract them from the images of the object taken.
More reference stars= more accurate data

5. Theory
Many characteristics determined through calculation, not observation
Radius mass of star, as well as planet’s period, are easily estimated through observation
You can then find:
semi-major axis
orbital speed
radius
transit duration
impact parameter
Inclination
The maths used is based around Kepler’s Laws and Newton’s Laws of Motion and of Gravitation.

6. Newton’s + Kepler’s Laws
Newton’s Third Law states: when one body exerts a force on another body, the second body exerts equal & opposite force on the first body.
This leads to Newton’s Law of Universal Gravitation
G gravitational constant
r radius.
We can then apply Kepler’s Third Law of Planetary Motion:
P2 ∝ a3
If we assume circular orbit, this becomes:
However, Mp is negligible compared to M* , leading to
M* is m1
Mp is m2

7. Finally, finding transit duration.
Once you know R* , RP, P, and a, you can find ttrans.
Two factors affect ttrans : impact parameter and inclination of the planet’s orbit (i).
In this diagram, b is the impact parameter and a is the semi-major axis.
We can obviously see that the longest transit duration will occur when b is 0, and as b increases ttrans decreases.
Trigonometry tells us that b =a cos(i)
Finally, we can use Pythagoras to find l, the length of the transit (from Earth POV)

8. GJ-1214 b Mass of 6.55 M⊕ Radius of 2.68 R⊕
Intermediate between Earth-like planets and gas giants.
13 parsecs / 42 light years away
Mainly H2O composition.
Measurements indicate period of 1.58 days
Our analysis of the light-curve shows:
t trans of days
Dip in brightness:
Rp - R* ratio: 0.12 (using )

9. Qatar-1b Planet name: Qatar 1b Planet Mass: 1.09±0.08 MJ
Planet radius: 1.17±0.06 RJ
Planet temp: 1380±45 Kelvin
Hot Jupiter
Gas giant
Located 550 light years away from Earth
Planet orbits its star every 34 hours, making it one of the shortest period planets yet found orbiting a star less massive than the sun
Detected by transit method .

10. Duration of transit: 0.06 days
Dip in brightness: 0.025
Ratio of planet to star radius: 0.16

11. WASP-2bSP-2b Orbits WASP 2 In constellation of Delphinus
Jupiter compared to WASP-2b size
Mass
(m)
0.847 ± MJ
Radius
(r)
1.079 ± RJ
Surface gravity
(g)
3.279 ± g
Temperature
(T)
1300 ± 54 K
Distance
470 ly
Constellation
Delphinus
Type
Gas Giant
Orbits WASP 2
In constellation of Delphinus
that WASP 2b was a planet.
Planet’s mass and radius indicate that it is a gas giant with a similar bulk composition to Jupiter.
Binary star

12. Duration of transit
0.060 days
using your final lightcurve
Dip in brightness
0.019
Ratio of planet to star radius
0.14
calculated from your final lightcurve

13. TrES-3b
Jupiter compared to TrES-3b size
Mass
(m)
1.92 ± 0.23 MJ
Radius
(r)
1.341 ± RJ
Density
(ρ)
1172 kg m-3
Surface gravity
(g)
2.7 g
The planet’s home star is slightly smaller and cooler than the Sun and is about 6 times larger than the planet. TrES-3b is a gas giant and TrES-3 is very close to its parent star and orbits it in 31 hours. That means that the year on TrES-3 lasts less than one and one-third Earth days. 

14. TrES-3b- Experimental data
The light curve shows a drop in the brightness of the light between around 4:30 and 5:30 which is when the planet is transiting the star.
brightness of 2.54%.
The measurements suggest the planet has a radius roughly 0.16 times that of the host star.

15. TrES-3b- Actual data Mass (m) 1.92 ± 0.23 MJ Radius (r)
Transit time ≈ hours
Dip in brightness ≈ 2.54%
Mass
(m)
1.92 ± 0.23 MJ
Radius
(r)
1.341 ± RJ
Density
(ρ)
1172 kg m-3
Surface gravity
(g)
2.7 g

16. Detecting - radial velocity.ppt