Sarah, Ellie, Adan and Sruthy. The Transit Method.

Slides:

Advertisements

Similar presentations

Dr Matt Burleigh The Sun and the Stars. Dr Matt Burleigh The Sun and the Stars Binary stars: Most stars are found in binary or multiple systems. Binary.

Advertisements

Binary Systems and Stellar Parameters The Classification of Binary Stars Mass Determination using visual Binaries Eclipsing,Spectroscopic Binaries The.

Other Planetary Systems. Detecting Extrasolar Planets  Extrasolar planets are planets orbiting other stars.  We usually detect these planets by the.

Binary Stars Astronomy 315 Professor Lee Carkner Lecture 9.

Binary Stars Astronomy 315 Professor Lee Carkner Lecture 9.

Lecture 14: Searching for planets orbiting other stars III: Using Spectra 1.The Spectra of Stars and Planets 2.The Doppler Effect and its uses 3.Using.

The Properties of Stars Masses. Using Newton’s Law of Gravity to Determine the Mass of a Celestial Body Newton’s law of gravity, combined with his laws.

Extra-Solar Planets Astronomy 311 Professor Lee Carkner Lecture 24.

Lecture 16: Searching for Habitable Planets: Remote Sensing Methods and parameters we can measure Mean density measurements: internal structure Measurements.

Copyright © 2012 Pearson Education, Inc. Extrasolar Planetary Systems.

Astronomy190 - Topics in Astronomy Astronomy and Astrobiology Lecture 19 : Extrasolar Planets Ty Robinson.

„We are not talking about cosmology...“ (A. Sozzetti)

Chapter 2 The Copernican Revolution. Units of Chapter Ancient Astronomy 2.2 The Geocentric Universe 2.3 The Heliocentric Model of the Solar System.

6.5 Other Planetary Systems Our goals for learning: How do we detect planets around other stars? How do extrasolar planets compare with those in our own.

What stellar properties can be learnt from planetary transits Adriana Válio Roque da Silva CRAAM/Mackenzie.

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.

The mass ratio of the stellar components of a spectroscopic binary can be directly computed from their ratio in radial velocities. To derive the total.

AST 111 Exoplanets I.

Chapter 2 The Copernican Revolution. Units of Chapter Ancient Astronomy 2.2 The Geocentric Universe 2.3 The Heliocentric Model of the Solar System.

Extrasolar planets. Detection methods 1.Pulsar timing 2.Astrometric wobble 3.Radial velocities 4.Gravitational lensing 5.Transits 6.Dust disks 7.Direct.

Physics 55 Friday, October 21, Doppler shift with application. 2.Conservation of angular momentum. 3.How star systems form, the nebular theory.

How do the planets stay in orbit around the sun?

Properties of Stars.

Diversity of Data in the Search for Exoplanets Rachel Akeson NASA Exoplanet Science Institute California Institute of Technology.

Stars Stellar radii –Stefan-Boltzman law Measuring star masses.

Stars: Binary Systems. Binary star systems allow the determination of stellar masses. The orbital velocity of stars in a binary system reflect the stellar.

Other Planets (Exoplanets). OGLE-2005-BLG-390Lb Discovered in 2005, via `gravitational microlensing’, which uses the properties of lensing of light to.

Lecture 14: The Discovery of the World of Exoplanets Indirect methods for planet detection The Astrometric method The Doppler shift method The Transit.

Extra-Solar Planet Populations Stephen Eikenberry 4 November 2010 AST

Newton’s Law of Universal Gravitation

23 November 2015what do we know from the exo-planets? Florian Rodler What do we know about the exo-planets? & How to detect direct signals from exo-planets?

The Search for Extra-Solar Planets Dr Martin Hendry Dept of Physics and Astronomy.

Extrasolar Planets Exo planets are planets outside the Solar System. They orbit another star. 861 confirmed…18,000 identified, but likely billions exist.

Extrasolar planets. Detection methods 1.Pulsar Timing Pulsars are rapidly rotating neutron stars, with extremely regular periods Anomalies in these periods.

Early science on exoplanets with Gaia A. Mora 1, L.M. Sarro 2, S. Els 3, R. Kohley 1 1 ESA-ESAC Gaia SOC. Madrid. Spain 2 UNED. Artificial Intelligence.

Lecture 34 ExoPlanets Astronomy 1143 – Spring 2014.

This exoplanet orbiting 51 pegasi is being vaporized by its’s parent star.

Extra Solar Planet Detection by the Doppler Detection method The following slides are a summary of the classroom presentation annotating the Doppler Detection.

Exoplanets Or extra-solar planets have recently been discovered. There are important to find to help fill in the Drake Equation that determines the probability.

The Solar System Missions. planets not shown to scale >> MercuryVenusEarthMarsJupiterSaturnUranusNeptunePluto Mean Distance from the Sun (AU)

Extra-Solar Planet Populations George Lebo 10 April 2012 AST

2003 UB313: The 10th Planet?. Extra-Solar or Exoplanets Planets around stars other than the Sun Difficult to observe Hundreds discovered (> 2000 so far)

2003 UB313: The 10th Planet?. Extra-Solar or Exoplanets Planets around stars other than the Sun Difficult to observe Hundreds discovered (> 2000 so far)

Tony Zhao Exo- outside, outer, out of Ayyo wut’s an exoplanet

Kepler Mission. Transit Method Planetary transits cause some light from a star to be blocked. The change in light is small for exoplanets. –Hard to detect.

Olivia Lowery The planetary system Kepler-113 hosts two planets, which were both discovered using the transit method. Kepler-113 B Kepler-113 C The two.

Section Orbital Motion of Satellites and Kepler’s Laws

Newton’s Law of Universal Gravitation. Law of Universal Gravitation.

Astro 18 – Section Week 2 EM Spectrum. ElectroMagnetic Radiation Energy moves in waves with electrical and magnetic components Energy moves in waves with.

11.2 Classifying Stars Our Goals for Learning How do we classify stars? Why is a star’s mass its most important property? What is a Hertzsprung–Russell.

Lectures 2 and 3 1. Kepler’s three laws 2. Use parallax, spectroscopic parallax, and the distance modulus to calculate distances to planetary systems 3.

Lecture Outlines Astronomy Today 8th Edition Chaisson/McMillan © 2014 Pearson Education, Inc. Chapter 2.

Extrasolar Planets. An Extrasolar planet, or exoplanet, is a planet outside the Solar System. First exoplanet was confirmed indirectly at G-type star.

Extrasolar planets - exoplanets Planets have been discovered orbiting other stars. The list of confirmed exoplanets has over 1900.list Evidence comes from.

Exoplanets: Direct Search Methods 31 March 2016 © 2014 Pearson Education, Inc.

Stability of (exo)moons Nagy Imre Research Group for Physical Geodesy and Geodynamics Department of Astronomy, Eötvös University.

Searching for Alien Worlds. Methods of Searching for Alien Planets Pulsar Timing Astrometry Radial Velocity Transits Lensing Imaging.

Chapter 13 Gravitation In this chapter we will explore the following topics: -Newton’s law of gravitation that describes the attractive force between two.

Exoplanets: Indirect Search Methods

Binary Stars Hypothesis. Masses of Stars  While we can find the radius of a star from the Stefan-Boltzmann Law, we still do not know the mass  How do.

Extrasolar Planets.

Chapter 13 Gravitation In this chapter we will explore the following topics: -Newton’s law of gravitation that describes the attractive.

Chapter 13 Gravitation In this chapter we will explore the following topics: -Newton’s law of gravitation, which describes the attractive force between.

What is an Exoplanet? Why is their search important?

Extrasolar planets - exoplanets

Where We Are…. As of November 21, 2016, over 3400 confirmed exoplanets had been found, with over 4500 additional candidate exoplanets. We can look at these.

Learning Goals: 4. Complex Knowledge: demonstrations of learning that go aboveand above and beyond what was explicitly taught. 3. Knowledge: meeting.

Exoplanets Ioannis Paraskevas.

Presentation transcript:

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 Mass1.199±0.052 M J Orbital Period ± d Radius1.341 ± R J Surface gravity3.284±0.016 g Temperature- Distance750±30 ly TypeGas Giant Star GSC ConstellationDraco

Duration of transit 0.042days Dip in brightness0.025 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 axis 2) orbital speed 3) radius 4)transit duration 5) impact parameter 6)Inclination Calculations based on Newton & Kepler’s Laws.

GJ-1214 b Mass6.55 ± 0.98 M ⊕ Orbital Period ± 1.6x10 -7 d Radius2.678 ± 0.13 R ⊕ Surface gravity 0.91 g Temperature 393–555 K Distance 42 ly (12 pc) TypeSuper-Earth StarGJ 1214 ConstellationOphiuchus

Duration of transit days Dip in brightness Ratio of planet to star radius 0.12

Qatar-1b. Mass1.09±0.08 M J Orbital Period ± 1.6x days Radius1.164 ±0.06 R Surface gravity- Temperature1380±45 K Distance550 ly (169 pc) TypeGas Giant StarQatar-1 ConstellationDraco

Duration of transit days Dip in brightness0.025 Ratio of planet to star radius 0.16

WASP-2bSP-2b Jupiter compared to WASP-2b Mass0.847 ± M J Orbital Period ± 4x10 -7 days Radius1.079 ± R J Surface gravity3.279 ± g Temperature1300 ± 54 K Distance470 ly (144 pc) TypeGas Giant StarWASP-2 ConstellationDelphinus

Duration of transit days Dip in brightness0.019 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 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