Kevin France University of Colorado AXIS Science Workshop August 6 th 2018
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1 Kevin France University of Colorado AXIS Science Workshop August 6 th 2018
2 Star-Planet Interactions at High-energies Introduction: In the solar system: Solar Influences, Living with a Star, etc. Afar: Exoplanet Space Weather, Stellar Habitable Zone, Living with a Red Dwarf, Hot Jupiters, etc.
3 Section 1 Disk clearing, the end of stellar mass accretion 1 10 Myr (Image: Karen Teramura)
4 Hot Jupiter Super-Earth WASP-18b, solar-type host M ~ 10 M J, R ~ 1.1 R J a ~ 0.02 AU T eff ~ K (Hellier et al. 2009) GJ 832c, red dwarf host M sin(i) ~ 5.2 M E, R ~ 1.7 R E a ~ 0.16 AU (Wittenmyer et al. 2014) T eff ~ K
5 Hot Jupiter Super-Earth WASP-18b, solar-type host M ~ 10 M J, R ~ 1.1 R J a ~ 0.02 AU T eff ~ K (Hellier et al. 2009) GJ 832c, red dwarf host M sin(i) ~ 5.2 M E, R ~ 1.7 R E a ~ 0.16 AU T eff ~ K (Wittenmyer et al. 2014)
6 Hot Jupiter Super-Earth WASP-18b, solar-type host M ~ 10 M J, R ~ 1.1 R J a ~ 0.02 AU T eff ~ K (Hellier et al. 2009) GJ 832c, red dwarf host M sin(i) ~ 5.2 M E, R ~ 1.7 R E a ~ 0.16 AU T eff ~ K (Wittenmyer et al. 2014)
7 Star-Planet Interactions at High-energies Overview: Early Times (< 10 Myr): Dissipation of the protoplanetary disk and the characterization of the raw materials for planet formation Intermediate Times ( Myr):: Shaping the exoplanet population Late Times (> 1000 Myr): Mass loss and biomarker destruction on rocky planets around red dwarfs
8 Star-Planet Interactions at High-energies Overview: Early Times (< 10 Myr): Dissipation of the protoplanetary disk and the characterization of the raw materials for planet formation Intermediate Times ( Myr):: Shaping the exoplanet population Late Times (> 1000 Myr): Mass loss and biomarker destruction on rocky planets around red dwarfs
9 The role of XUV emission in the dispersal of protoplanetary disks Ercolano & Pascucci 2017 ; Alexander et al (PPVI)
10 The role of XUV emission in the dispersal of protoplanetary disks EUV FUV X-ray Total Disk Mass Loss Rate L(X-ray) Font 2004; Owen 2012; Gorti 2009; Ercolano et al. 2009; Alexander et al (PPVI)
11 The role of X-ray spectroscopy to measure the gasto-dust ratio in the youngest disks Bright Dip Time (days) Ansdell et al. (2016); Schneider et al. (2015a,b)
12 Star-Planet Interactions at High-energies Overview: Early Times (< 10 Myr): Dissipation of the protoplanetary disk and the characterization of the raw materials for planet formation Intermediate Times ( Myr): Shaping the exoplanet population Late Times (> 1000 Myr): Mass loss and biomarker destruction on rocky planets around red dwarfs
13 X-ray/EUV Figure borrowed from James Owen s Exoplanets-2 Talk, July 2018
14 X-ray/EUV Figure borrowed from James Owen s Exoplanets-2 Talk, July 2018
15 Transit Spectroscopy of Short-period Planets XUV heating driving mass-loss from short-period planets Most spectacular example has been on the short-period Neptune-mass planet GJ 436b Hydrogen detected in the upper atmosphere of GJ436b (Kulow et al. 2014; Ehrenreich et al. 2015; Bourrier et al. 2016; Lavie et al. 2017) Transit depth ~ 50% (!)
16 X-ray/EUV Figure borrowed from James Owen s Exoplanets-2 Talk, July 2018
17 Owen & Jackson 2012
18 Figure borrowed from James Owen s Exoplanets-2 Talk, July 2018
19 Figure borrowed from James Owen s Exoplanets-2 Talk, July 2018
20 Figure borrowed from James Owen s Exoplanets-2 Talk, July 2018
21 Fulton & Petigura 2018
22 Fulton & Petigura 2018
23 Star-Planet Interactions at High-energies Overview: Early Times (< 10 Myr): Dissipation of the protoplanetary disk and the characterization of the raw materials for planet formation Intermediate Times ( Myr):: Shaping the exoplanet population Late Times (> 1000 Myr): Mass loss and biomarker destruction on rocky planets around red dwarfs
24 Biomarker Production & Atmospheric Stability on Rocky Planets Orbiting Red Dwarfs Rocky planets in the habitable zones around red dwarfs (M dwarfs, e.g., Proxima Cen, TRAPPIST-1, etc) will likely be the first planets that can be probed for signs of life (2020s: 30-m telescopes, possibly JWST, 2030s: LUVOIR Surveyor) How do high-energy star-planet interactions impact what we expect to find?
25 Impacts on rocky planets, coordinating with IR transit spectroscopy
26 Impacts on rocky planets, coordinating with vis/ir atmospheric spectroscopy F - star ~2 AU G - star ~1 AU M - star ~0.15 AU not to scale
27 The liquid water Habitable Zone F - star ~2 AU G - star ~1 AU M - star Are these worlds habitable? ~0.15 AU not to scale
28 8 x F! 5 x F! F(EUV) from inactive M dwarfs 5 10 x larger than from the quiet Sun Adapted from Youngblood, France et al. 2016
29 8 x F! 5 x F! UV flares on inactive M dwarfs increase emission line brightness by factors of (next section) Adapted from Youngblood, France et al M dwarf EUV: Allison Youngblood - CU
30 463 x F! 105 x F! 8 x F! 5 x F! F(EUV) on an active M dwarf ~ 20 60x higher than on an inactive M dwarf Adapted from Youngblood, France et al M dwarf EUV: Allison Youngblood - CU
31 (Ribas et al. 2016)
32 Bolmont et al. (2017): H 2 O photolysis and hydrogen escape from TRAPPIST-1 planets (b, c, and d).
33 Related Question: How do time variable stellar emissions impact orbiting planets? Flares & CMEs Credit: SDO Loyd & France, 2014 France et al. (2013a, 2016) Youngblood, France et al. (2017) Loyd, France et al. (2018)
34 UV variability in inactive M dwarf exoplanet host stars Optically Inactive dm1 GJ 832. Flare/quiescent flux ratios ~ in intermediate temperature emission lines for most M dwarfs (30,000 K < T form < 150,000 K) MUSCLES Treasury, July France et al. (ApJ-2016 ) Loyd et al. (ApJ-2018)
35 X-ray variability in inactive M dwarf exoplanet host stars Optically Inactive dm4/5 GJ 876 (P rot ~ 100 days). France et al. (ApJ-2016) Loyd et al. (ApJ-2018)
36 GOES 1 8 Å and proton fluxes Yashiro et al Belov et al. 2007, Cliver et al Youngblood et al. (ApJ-2017)
37 GOES 1 8 Å and proton fluxes C M X Belov et al Yashiro et al Belov et al. 2007, Cliver et al Youngblood et al. (ApJ-2017)
38 X-ray Flare on GJ 876. X1 ~2400 > 10 MeV protons/ cm 2 /s/sr in the HZ M2 X1 at 1 AU, 30x larger in the HZ ( ~X30) France et al Loyd et al. in prep. Youngblood, France et al. (ApJ )
39 Question: How do time variable stellar emissions impact orbiting Atmospheric Evolution: Conservative flare rate (T dep (O 3 ) = 318 kyr) GJ 876 flare rate (T dep (O 3 ) = 160 yr) planets? Youngblood, France et al. (ApJ ) also Tilley et al. (2017)
40 Summary: Early Times (< 10 Myr): Dissipation of the protoplanetary disk and the characterization of the raw materials for planet formation Intermediate Times ( Myr):: Shaping the exoplanet population Late Times (> 1000 Myr): Mass loss and biomarker destruction on rocky planets around red dwarfs Kevin France University of Colorado
41 Kevin France University of Colorado END
The Ultraviolet Radiation Environment in the Habitable Zones Around Low-Mass Exoplanet Host Stars. Kevin France. University of Colorado at Boulder
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