Kevin France University of Colorado AXIS Science Workshop August 6 th PDF Free Download

Kevin France University of Colorado AXIS Science Workshop August 6 th 2018

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.

Section 1 Disk clearing, the end of stellar mass accretion 1 10 Myr (Image: Karen Teramura)

Hot Jupiter Super-Earth WASP-18b, solar-type host M ~ 10 M J, R ~ 1.1 R J a ~ 0.02 AU T eff ~ 2400-3100 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 ~ 230-280 K

Hot Jupiter Super-Earth WASP-18b, solar-type host M ~ 10 M J, R ~ 1.1 R J a ~ 0.02 AU T eff ~ 2400-3100 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 ~ 230-280 K (Wittenmyer et al. 2014)

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 (10 1000 Myr):: Shaping the exoplanet population Late Times (> 1000 Myr): Mass loss and biomarker destruction on rocky planets around red dwarfs

The role of XUV emission in the dispersal of protoplanetary disks Ercolano & Pascucci 2017 ; Alexander et al. 2014 (PPVI)

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. 2014 (PPVI)

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)

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 (10 1000 Myr): Shaping the exoplanet population Late Times (> 1000 Myr): Mass loss and biomarker destruction on rocky planets around red dwarfs

X-ray/EUV Figure borrowed from James Owen s Exoplanets-2 Talk, July 2018

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% (!)

X-ray/EUV Figure borrowed from James Owen s Exoplanets-2 Talk, July 2018

Owen & Jackson 2012

Figure borrowed from James Owen s Exoplanets-2 Talk, July 2018

Fulton & Petigura 2018

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?

Impacts on rocky planets, coordinating with IR transit spectroscopy

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

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

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

8 x F! 5 x F! UV flares on inactive M dwarfs increase emission line brightness by factors of 10 100 (next section) Adapted from Youngblood, France et al. 2016 M dwarf EUV: Allison Youngblood - CU

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. 2016 M dwarf EUV: Allison Youngblood - CU

(Ribas et al. 2016)

Bolmont et al. (2017): H 2 O photolysis and hydrogen escape from TRAPPIST-1 planets (b, c, and d).

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)

UV variability in inactive M dwarf exoplanet host stars Optically Inactive dm1 GJ 832. Flare/quiescent flux ratios ~10 100 in intermediate temperature emission lines for most M dwarfs (30,000 K < T form < 150,000 K) MUSCLES Treasury, July 07 2015 France et al. (ApJ-2016 ) Loyd et al. (ApJ-2018)

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)

GOES 1 8 Å and proton fluxes Yashiro et al. 2006 Belov et al. 2007, Cliver et al. 2012 Youngblood et al. (ApJ-2017)

GOES 1 8 Å and proton fluxes C M X Belov et al. 2005 Yashiro et al. 2006 Belov et al. 2007, Cliver et al. 2012 Youngblood et al. (ApJ-2017)

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. 2016 Loyd et al. in prep. Youngblood, France et al. (ApJ - 2017)

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 - 2017) also Tilley et al. (2017)

Summary: Early Times (< 10 Myr): Dissipation of the protoplanetary disk and the characterization of the raw materials for planet formation Intermediate Times (10 1000 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

Kevin France University of Colorado END