Exoplanet Pursuit. PLANet B. Kalpaxis Georgios Vasilainas Athanasios Vatistas Andreas

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1 Exoplanet Pursuit PLANet B Kalpaxis Georgios Vasilainas Athanasios Vatistas Andreas

2 We must continue to go into space for the future of humanity. I do not think we will survive another 1,000 years without escaping our fragile planet. -Stephen Hawking

3 Project Goals Search for exoplanets using the Kepler Mission data and the transit method. Implement a new approach for this search, using two original computer programs written by us. Extract the orbital and transit parameters of the exoplanets. Explain the light variation in a case of other phenomena, like a pulsating variable star.

4 watch? v=51gnntlzj6g&feature=youtu.b e

5 How does the transit method work?

6 How does the transit method work? Light curve is a graph of light intensity of a star as a function of time

7

8 We used the data from the Kepler Mission and retrieved from the NASA Exoplanet Archive.

9 Some Light curves

10 The major difficulty

11 ????

12

13

14 So we thought about developing a program!

15 PLANET TRACKER 1.3 (pltrack 1.3)

16 Sliding Window Threshold

17

18 The produced file (named out.dat) and its graph

19

20 Pltrack2

21

22

23 The shape of Kepler-10c transit (KIC ).

24 Theoretical Background

25 The equations we used to extract the transit and orbital parameters are (Seager & Mallén, 2003): 1. The transit depth F and stellar radii respectively Δ, with F defined as the total observed flux, and, R* ΔF = F no transit F F no transit transit Rp = R * 2 R p the planetary 2. Kepler s Third Law, assuming a circular orbit, where P is the orbital period, G is the M p, M the planetary and stellar masses, and a the orbital universal gravitational constant, * radius, P 2 * 2 4π a = G( M + 3 M p )

26 3. The impact parameter b that defines the shape of the transit, where F T t t, is the total duration of the eclipse and the duration of the flat part, ( ) ( ) 2 1/ Δ + Δ = T F T F t t F t t F b 4. The orbital inclination i, = a R b i * 1 cos

27 ANALYSIS

28 Artificially created data

29 Kepler-10 (KIC ) An artist concept shows the Kepler-10 system, home to two rocky planets.

30

31

32 Kepler-10c Transit and orbital parameters Orbital period P (days) ( ) Transit dura>on (hours) (6.868) Radius ra>o (R p /R * ) ( ) Inclina>on i (deg) 88.8 (89.59) Distance to stellar radius Ra>o, a/r * (47.9) Impact parameter b (0.36) Planetary parameters Planet mass M p (Earth masses) - (17.2) Planet radius R p (Earth radii) (2.35) Orbital semi-major axis a (AU) (0.2372) Table. Transit, orbital and planetary parameters of Kepler-10c. Values in parenthesis are taken from the literature.

33 Kepler-745 (KIC )

34

35

36 Kepler-745b Transit and orbital parameters Orbital period P (days) ( ) Transit dura>on (hours) (5.659) Radius ra>o (R p /R * ) ( ) Inclina>on i (deg) ( - ) Distance to stellar radius Ra>o, a/r * ( - ) Impact parameter b ( - ) Planet mass M p (Earth masses) Planetary parameters - ( - ) Planet radius R p (Earth radii) 1.24 (2.16) Orbital semi-major axis a (AU) ( - ) Table. Transit, orbital and planetary parameters of Kepler-745b. Values in parenthesis are taken from the literature.

37 l in = ( 2 l a T b T ), * * in sun in in Lsun L 1/ 2 (Selsis et al, 2007) l out = ( 2 l a T b T ), * * out sun out out Lsun L 1/ 2 For Kepler 745 we calculated: l in = AU l out = AU while Kepler s 745b semimajor axis: a = AU

38 Ar>st s concept of CoRoT 7b, a planet similar to Kepler-745b.

39 KIC

40

41 KIC PulsaDon parameters Pulsa>on period P (days) Pulsa>on amplitude (rela>ve flux) Absolute magnitude Distance (Kpc) Table. Parameters of KIC under the hypothesis of a Cepheid variable.

42 Future Plans 1. A more accurate method should be applied to define the critical event threshold. 2. Implement more complex models taking into account additional stellar phenomena like the limb darkening. 3. Expand our research to the CoRoT and the K2 Missions.

43

44 Thank you for your attention!!

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