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Detection of Star-Planet Interaction with Future X-ray Missions

Detection of Star-Planet Interaction with Future X-ray Missions. Scott J. Wolk I. Pillitteri, O. Cohen, V. Kashyap, C. Lisse, J. Drake. What is Star Planet Interaction?. Cuntz et al. 2000. Could the Planet really Matter?. HD 189733b 1G (1/2 Jupiter). HD 189733 40G. Cohen et al. 2011.

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Detection of Star-Planet Interaction with Future X-ray Missions

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  1. Detection of Star-Planet Interaction with Future X-ray Missions Scott J. Wolk I. Pillitteri, O. Cohen, V. Kashyap, C. Lisse, J. Drake

  2. What is Star Planet Interaction? Cuntz et al. 2000

  3. Could the Planet really Matter? HD 189733b 1G (1/2 Jupiter) HD 189733 40G Cohen et al. 2011

  4. Why do we care about SPI? • X-rays from stars effect exoplanets… • Some hot Jupiters appear inflated beyond what the bolometric luminosity would predict. • X-Ray/UV flux  atmospheric expansion (Lammier et al. 2003) • X-Ray flux  photochemistry changing the thermal budget (Laing et al. 2004; Burrows et al. 2008) • …Exoplanets may effect their host stars. • Analytic Studies show  Frecon a ap-3(Saar et al. 2004) • Analytic models indicate field lines can connect the star to the planet, ruptures of the lines could give rise to flare-like activity. • MHD simulations show strong feedback visible in X-rays

  5. SPI induced flares? Cohen et al. 2011

  6. Cohen et al. 2011

  7. What is the evidence exists for Star-Planet Interaction? • Direct observation of phased emission from Ca II HK lines (Shkolnik et al. 2003, 2008) • Stars with hot Jupiters are brighter in X-rays (Kashyap et al. 2009) • But both results are disputed. (Poppenhager et al. 2010) Kayshap et al. 2009

  8. An example - HD 189733 • At a distance of 19.3 pc it is one of the closest transiting planets. • Somewhat X-ray active (Lx~10Lx) • Age estimated at 0.6 Gyr • XMM (Wheatley-PI) observed a planetary transit in April 2007 • We observed secondary eclipse with XMM in May 2009 • Secondary not detect in X-rays!

  9. Results Transit Eclipse

  10. X-Ray Softening With XMM time resolution~ 1ks at 5 counts/ks

  11. Was the timing of the flare related to SPI?(Lanza 2008) Phase 0.5 Phase 0.54

  12. The Flare

  13. Tantalizing evidence Blue shifted Oxygen lines? RIF

  14. The Benefits of Future Observatories To these Studies • More collecting area  more targets can be investigated. • Flux = time resolution. • Better spectral resolution at low energy allows us to measure flow dynamics. (need resolution ~4-10 RGS) • Softer sensitivity  Allows the detection of lower ionization states OVI, NV, CIV, SiIX, MgIX, Ne IIX Koutroumpa et al.2009

  15. MHD:Forward Flow

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