1. Phase Light Curves for Extrasolar Jupiters and Saturns ASA meeting, July 6, 2004 U. Dyudina(1), P.Sackett(1), D. Bayliss(1), L Dones(2), H. Throop (2), C. Porco(3), S. Seager(4) (1)Mount Stromlo Obs., Australian National University (2)Southwest Research Institute, Boulder, USA (3)Space Science Institute, Boulder, USA (4)DTM, Carnegie Institute at Washington, USA U. Dyudina(1), P.Sackett(1), D. Bayliss(1), L Dones(2), H. Throop (2), C. Porco(3), S. Seager(4) (1)Mount Stromlo Obs., Australian National University (2)Southwest Research Institute, Boulder, USA (3)Space Science Institute, Boulder, USA (4)DTM, Carnegie Institute at Washington, USA astro-ph/0406390

2. Method. Model reflected light from extrasolar planets (as if they were Jupiter or Saturn) Rings? (yes!) Inclination? (often yes) Clouds? (sometimes) Model reflected light from extrasolar planets (as if they were Jupiter or Saturn) Rings? (yes!) Inclination? (often yes) Clouds? (sometimes) Can we detect: Sackett, Dyudina, et al. astro-ph/0406390

3. Phase light curve of the orbiting planet Sackett, Dyudina, et al. astro-ph/0406390

4. Full-disk albedo (Lp/L*)X (Planet radius)²/(Orbital distance) ² For Saturn at 1 AU : 1.6 X 10 -7 Azimuth of the planet along the orbit (deg.) Jupiter versus Saturn (orbit seen edge-on ) Sackett, Dyudina, et al. astro-ph/0406390

5. Saturn as seen by Cassini spacecraft Surface scattering properties measured by Pioneer and Voyager spacecraft Sackett, Dyudina, et al. astro-ph/0406390

6. Full-disk albedo (L p /L * )X (Planet radius)²/(Orbital distance) ² Sackett, Dyudina, et al. astro-ph/0406390 Modeled phase light curves (edge-on)

7. Full-disk albedo (L p /L * )X (Planet radius)²/(Orbital distance) ² Sackett, Dyudina, et al. astro-ph/0406390 Modeled phase light curves (incl. 45 o )

8. Full-disk albedo (L p /L * )X (Planet radius)²/(Orbital distance) ² Sackett, Dyudina, et al. astro-ph/0406390 Modeled phase light curves (face-on)

9. Sackett, Dyudina, et al. astro-ph/0406390 Light curves. Planet with rings at different geometries. -ring’s tilt to ecliptic ω r -observer’s azimuth i -orbital inclination 

10. Inclination: i=0° (face on) Eccentric orbits. No rings Sackett, Dyudina, et al. astro-ph/0406390

11. Inclination: i=10° Sackett, Dyudina, et al. astro-ph/0406390

12. Inclination: i=45° Sackett, Dyudina, et al. astro-ph/0406390

13. Inclination: i~90° (edge on) Sackett, Dyudina, et al. astro-ph/0406390

14. Argument of pericentre: ω=0° To observer Orientation of the orbital plane - Argument of Pericentre Sackett, Dyudina, et al. astro-ph/0406390

15. To observer Argument of pericentre: ω=-90° Sackett, Dyudina, et al. astro-ph/0406390

16. To observer Argument of pericentre: ω=90° Sackett, Dyudina, et al. astro-ph/0406390

17. Example - HD 108147b Extra solar planet discovered by Pepe, Mayor, et al (2002, A&A, 388, 632). Properties: –Semi-major axis = 0.104 AU –Period = 10.9 days –Eccentricity = 0.498 –Argument of pericentre = -41° –Inclination = ? Sackett, Dyudina, et al. astro-ph/0406390

18. Light curve for HD 108147b with Jupiter’s surface Sackett, Dyudina, et al. astro-ph/0406390 pericentre

19. Light curve for HD 108147b viewed at different azimuth contrast t-shift Sackett, Dyudina, et al. astro-ph/0406390 pericentre

20. Contrast for e=0.6 Inclination (i) 90 0 -90 Scale at 1 AU (x10 -7 ) Argument of pericentre (ω) 090 100 10 1 0.1 Sackett, Dyudina, et al. astro-ph/0406390

21. Observable contrast for ringless planets at different geometries Sackett, Dyudina, et al. astro-ph/0406390

22. Light curve for HD 108147b viewed at different azimuth contrast t-shift Sackett, Dyudina, et al. astro-ph/0406390 pericentre

23. Observable t-shift for ringless planets at different geometries Sackett, Dyudina, et al. astro-ph/0406390

24. Rings? (yes!) Inclination? (often yes) Clouds? (sometimes) With light curves can we detect: : : Use of our predictions for planning observations Planet’s luminocity for many geometries Effects of Jupiter’s or Saturn’s clouds