Kepler/K2 Science Conference V

Transcript

1. Planetary Archaeology: Exploring Planets Transiting Evolved Stars Samuel Grunblatt, Daniel Huber, Eric Gaidos, Eric Lopez Institute for Astronomy, University of Hawaii— Manoa, Honolulu, HI skg3@hawaii.edu
2. Distribution of Kepler target stars: mostly Sunlike Kepler Huber+ (2014) @skgrunblatt skg3@hawaii.edu
3. Distribution of K2 target stars: more M stars, more giants Huber+ (2016) @skgrunblatt skg3@hawaii.edu
4. Huber+ (2016) @skgrunblatt skg3@hawaii.edu More giants: galactic, planetary archaeology possible
5. Why should you care about planets orbiting giant stars? @skgrunblatt skg3@hawaii.edu skg3@hawaii.edu
6. To solve long-standing planet inflation mysteries Can planets be inflated at late times? (Burrows+ 2000, Bodenheimer+ 2001, Lopez+ 2016, Grunblatt+ 2016, Grunblatt+ 2017) Why should you care about planets orbiting giant stars? skg3@hawaii.edu @skgrunblatt
7. The Mechanism of Planet Inflation e.g., Bodenheimer+ (2001), Showman & Guillot (2002),
 Batygin & Stevenson (2010), Ginzburg & Sari (2016) Class I: planet interior inflated directly by increased stellar irradiation Class II: cooling delayed after planet formation e.g., Burrows+ (2000), Chabrier & Baraffe (2007), Leconte & Chabrier (2012), Wu & Lithwick (2013) skg3@hawaii.edu @skgrunblatt
8. How to distinguish between Classes I and II? Class I: re-inflation Class II: no re-inflation skg3@hawaii.edu @skgrunblatt
9. delayed cooling ] re-inflation Grunblatt+ (2017) Is K2-97b re-inflated? Probably. Data implies significant post-MS planet heating. But how? K2-97b: skg3@hawaii.edu @skgrunblatt
10. delayed cooling ] re-inflation Grunblatt+ (2017) Is K2-97b re-inflated? Probably. Kepler-422b: 1.15 Msun 0.43 MJ 7.89 days Data implies significant post-MS planet heating. But how? K2-97b: skg3@hawaii.edu @skgrunblatt
11. delayed cooling ] re-inflation Grunblatt+ (2017) Is K2-97b re-inflated? Probably. Kepler-422b: 1.15 Msun 0.43 MJ 7.89 days Data implies significant post-MS planet heating. But how? K2-97b: skg3@hawaii.edu @skgrunblatt Berger+ (2018)
12. To solve long-standing planet inflation mysteries Can planets be inflated at late times? (Burrows+ 2000, Bodenheimer+ 2001, Lopez+ 2016, Grunblatt+ 2016, Grunblatt+ 2017) @skgrunblatt skg3@hawaii.edu Why should you care about planets orbiting giant stars?
13. To solve long-standing planet inflation mysteries Can planets be inflated at late times? (Burrows+ 2000, Bodenheimer+ 2001, Lopez+ 2016, Grunblatt+ 2016, Grunblatt+ 2017) To study planet evolution: as star evolves, planets must react inspiral, circularization, engulfment timescales still unknown (Villaver+ 2014, Fuller 2017, MacLeod+ 2018, Grunblatt+ 2018) @skgrunblatt skg3@hawaii.edu Why should you care about planets orbiting giant stars?
14. Hot Jupiters and Cool Stars Villaver, Livio, Mustill & Siess (2014) skg3@hawaii.edu @skgrunblatt
15. Hot Jupiters and Cool Stars Villaver, Livio, Mustill & Siess (2014) skg3@hawaii.edu @skgrunblatt Villaver+ (2014)
16. Hot Jupiters and Cool Stars Villaver, Livio, Mustill & Siess (2014) skg3@hawaii.edu @skgrunblatt Villaver+ (2014)
17. Do close-in giant planets orbiting evolved stars prefer eccentric orbits? Grunblatt+ (2018) skg3@hawaii.edu @skgrunblatt
18. Do close-in giant planets orbiting evolved stars prefer eccentric orbits? e = 0.15 +0.08-0.04 Grunblatt+ (2018) @skgrunblatt skg3@hawaii.edu
19. Do close-in giant planets orbiting evolved stars prefer eccentric orbits? e = 0.06 +0.02-0.01 e = 0.15 +0.08-0.04 Grunblatt+ (2018) @skgrunblatt skg3@hawaii.edu
20. Do close-in giant planets orbiting evolved stars prefer eccentric orbits? Grunblatt+ (2018) ? skg3@hawaii.edu @skgrunblatt
21. To solve long-standing planet inflation mysteries Can planets be inflated at late times? (Burrows+ 2000, Bodenheimer+ 2001, Lopez+ 2016, Grunblatt+ 2016, Grunblatt+ 2017) To study planet evolution: as star evolves, planets must react inspiral, circularization, engulfment timescales still unknown (Villaver+ 2014, Fuller 2017, MacLeod+ 2018, Grunblatt+ 2018) @skgrunblatt skg3@hawaii.edu Why should you care about planets orbiting giant stars?
22. To solve long-standing planet inflation mysteries Can planets be inflated at late times? (Burrows+ 2000, Bodenheimer+ 2001, Lopez+ 2016, Grunblatt+ 2016, Grunblatt+ 2017) To study planet evolution: as star evolves, planets must react inspiral, circularization, engulfment timescales still unknown (Villaver+ 2014, Fuller 2017, MacLeod+ 2018, Grunblatt+ 2018) To understand stellar variability: key to getting better star/planet parameters & finding currently undetectable planets with future missions motivates new models to characterize stellar variability (Grunblatt+ 2015, Grunblatt+ 2017, Jones+ 2018, RVxK2, RVxTESS) @skgrunblatt skg3@hawaii.edu Why should you care about planets orbiting giant stars?
23. Traces stellar granulation & oscillation signals Grunblatt+ (2017) SHO GP light curve model teaches us about stellar variability
24. Giant Planet Occurrence Within 0.2 AU of Low Luminosity Red Giant Branch Stars Grunblatt+ (in prep.)
25. A Search for Giants Orbiting Giants with K2 ➤ >10,000 Low Luminosity Red Giant Branch (LLRGB) targets ➤ Transit detection limit: ~9 Rsun ➤ K2 limit for asteroseismology: 283 μHz (~3 Rsun) ➤ Temperature limits: 4500—5500 K 
 (avoids horizontal branch stars) Huber+ (2016) @skgrunblatt skg3@hawaii.edu
27. Asteroseismic stellar parameters: Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
28. Asteroseismic stellar parameters: 2542 LLRGB stars in K2 LLRGB stars Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
29. LLRGB Planet Occurrence Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
30. LLRGB Planet Occurrence Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
31. LLRGB Planet Occurrence Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
32. LLRGB Planet Occurrence planet occurrence decreases with radius around MS stars… Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
33. LLRGB Planet Occurrence Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu planet occurrence decreases with radius around MS stars… …but seems to increase with radius around evolved stars!
34. What’s next?
35. Better statistics with TESS! Grunblatt (2018) @skgrunblatt skg3@hawaii.edu
36. Test migration dependencies on star, planet properties with >10x planets! @skgrunblatt skg3@hawaii.edu Campante+ (2016), Barclay+ (2018), Grunblatt (2018)
37. Summary: we should all care about planets orbiting giant stars! To solve planet inflation mysteries Can planets be inflated at late times? (Burrows+2000, Bodenheimer+2001, Lopez+2016, Grunblatt+2016, Grunblatt+2017) To study planet migration: as star evolves, planets must react inspiral, circularization, engulfment timescales still unknown (Villaver+2014, Fuller 2017, MacLeod+2018, Grunblatt+2018) To understand stellar variability: key to measuring better star/planet parameters and finding currently undetectable planets with future missions motivates new models to characterize stellar variability (Grunblatt+2015, Grunblatt+2017, Jones+2018, RVxK2, RVxTESS) skg3@hawaii.edu @skgrunblatt ifa.hawaii.edu/~skg
38. Thanks!
40. Extra Slides
41. K2-161b: validated with spectra, revised with Gaia+asteroseismology Mayo+ (2018)
42. Stellar activity: 10-30 m/s Planetary signal: 1.5 m/s HARPS-N HIRES Gaussian process RV analysis Grunblatt+ (2015)
43. Comparing different light curve models: Used squared exponential and simple harmonic oscillator GP kernel functions to account for astrophysical noise detrended light curve: no additional noise model
44. Used squared exponential and simple harmonic oscillator GP kernel functions to account for astrophysical noise Squared Exponential Gaussian Process Comparing different light curve models:
45. Simple Harmonic Oscillator GP ] correlated granulation
 & osc. signal minimized Used squared exponential and simple harmonic oscillator GP kernel functions to account for astrophysical noise Comparing different light curve models:
46. Combined transit + GP models Simple Harmonic Oscillator GP Squared Exponential GP Used squared exponential and simple harmonic oscillator GP kernel functions to account for granulation & oscillation noise Grunblatt+ (2017)
47. LLRGB Injection/Recovery Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
48. LLRGB Survey Completeness Grunblatt+ (in prep.) @skgrunblatt skg3@hawaii.edu
49. Appendix. Why are K2-97b, K2-132b, K2-161b so similar? 0.01 0.10 1.00 10.00 planet mass (Jupiters) 0.0 0.2 0.4 0.6 0.8 1.0 survey bias factor Short answer: probably survey bias * intrinsic planet occurrence
50. Appendix. Why is planet transit depth poorly constrained? Different lightcurves treat systematics differently. Somewhat accounted for with GP model Grunblatt+ (2016)
51. Asteroseismic stellar parameters: are they accurate? Calibrated asteroseismic relations with interferometry (~5% agreement), eclipsing binaries (5-10% agreements). Soon, calculating bolometric fluxes and radii from spectra, and Gaia parallaxes. ~500 bolometric fluxes in hand now. Grunblatt+ (in prep.)