agent exoplanet
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AGENT EXOPLANET. Sarah, Ellie, Adan and Sruthy. The Transit Method. 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. Our Project. TrES-3b. Jupiter compared to TrES-3b. Theory. - PowerPoint PPT PresentationTRANSCRIPT
AGENT EXOPLANET
Sarah, Ellie, Adan and Sruthy
The Transit Method
• 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.
Our Project
TrES-3b
Jupiter compared to TrES-3b
Mass 1.199±0.052 MJ
Orbital Period 2.4706 ± 0.00001 d
Radius 1.341 ± 0.081 RJ
Surface gravity 3.284±0.016 g
Temperature -
Distance 750±30 ly
Type Gas Giant
Star GSC 03549-02811
Constellation Draco
Duration of transit 0.042days
Dip in brightness 0.025
Ratio of planet to star radius 0.16
Theory•Radius, mass of star, as well as planet’s period, estimated through observation
•Then you can calculate:1) semi-major axis2) orbital speed3) radius4) transit duration5) impact parameter 6) Inclination
• Calculations based on Newton & Kepler’s Laws.
GJ-1214 b
Mass 6.55 ± 0.98 M⊕
Orbital Period 1.5804 ± 1.6x10-7d
Radius 2.678 ± 0.13 R⊕
Surface gravity 0.91 g
Temperature 393–555 K
Distance 42 ly (12 pc)
Type Super-Earth
Star GJ 1214
Constellation Ophiuchus
Duration of transit 0.039 days
Dip in brightness 0.0144
Ratio of planet to star radius 0.12
Qatar-1b
.
Mass 1.09±0.08 MJ
Orbital Period 1.4200 ± 1.6x10-05 days
Radius 1.164 ±0.06 R
Surface gravity -
Temperature 1380±45 K
Distance 550 ly (169 pc)
Type Gas Giant
Star Qatar-1
Constellation Draco
Duration of transit 0.060 days
Dip in brightness 0.025
Ratio of planet to star radius 0.16
WASP-2bSP-2b
Jupiter compared to WASP-2bMass 0.847 ± 0.045 MJ
Orbital Period 2.1522 ± 4x10-7 days
Radius 1.079 ± 0.033 RJ
Surface gravity 3.279 ± 0.036 g
Temperature 1300 ± 54 K
Distance 470 ly (144 pc)
Type Gas Giant
Star WASP-2
Constellation Delphinus
Duration of transit 0.060 days
Dip in brightness 0.019
Ratio of planet to star radius 0.14
Detecting Exoplanets
Using Radial Velocity or the Doppler Method
What is radial velocity?
Velocity along the line of sight toward or away from the observer.
This diagram shows how an orbiting planet will change the position of the star it orbits due to its gravitational tug.
What is spectroscopic radial velocity and how can it be used to determine a planet’s radial velocity?
S.R.V is the radial component of the velocity of the source at emission and the observer at observation, as determined by spectroscopy.
Advantages and Disadvantages of using the radial velocity method.
Advantage:• The planet's
eccentricity can be measured directly.
Disadvantage:• Can only estimate a
planet’s minimum mass.
Easier to detect planets orbiting low mass stars because....
• More affected by the planets’ gravitational tug.
• Generally, the planets rotate more slowly when orbiting a low mass star.
R.V. Method is the most productive method used...
456 Exoplanets – 31 confirmed and 323 candidates.
Of the 31 confirmed Exoplanets – 1 Exoplanet has been identified as having the potential for habitability – Gliese 581-d