Stellar activity effects on high energy transits Joe Llama | - - PowerPoint PPT Presentation

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Stellar activity effects on high energy transits Joe Llama | - - PowerPoint PPT Presentation

Nov 08, 2023 247 likes •455 views

Stellar activity effects on high energy transits Joe Llama | joe.llama@lowell.edu | @joe_llama Evgenya Shkolnik Andrew Cameron Moira Jardine Why observe high energy transits? Shallow transit Deep transit Why observe high energy

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Stellar activity effects on high energy transits

Joe Llama | joe.llama@lowell.edu | @joe_llama

Evgenya Shkolnik Andrew Cameron Moira Jardine

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Shallow
 transit Deep
 transit

Why observe high energy transits?

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Lower activity Higher activity

Why observe high energy transits?

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High energy transits of HD 189733b

X-rays

Poppenhaeger et al. (2013)

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Bourrier et al. (2013)

High energy transits of HD 189733b

Lyman-⍺

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Soft X-Ray 9.4 nm 6.3 x 106 K Extreme UV 21.1 nm 2.0 x 106 K Far UV 170 nm 5 x 103 K Optical 450 nm 5 x 103 K

The ultraviolet Sun

Llama & Shkolnik (2015)

Data from SDO/AIA

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450 nm (optical) 13.1 nm (EUV)

Limb-brightened transits

Llama & Shkolnik (2015)

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Phase Flux

0.00 0.02

  • 0.02

1.00 0.99 0.98

Phase Flux

0.00 0.02

  • 0.02

1.00 0.99 0.98

450 nm (optical) 13.1 nm (EUV)

Limb-brightened transits

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Phase Flux Soft X-Ray 9.4 nm

EUV 21.1 nm

Optical 450 nm

FUV 170 nm

Transiting the Sun I

0.00 0.02

  • 0.02

0.00 0.02

  • 0.02

0.00 0.02

  • 0.02

0.00 0.02

  • 0.02

1.00 0.98 0.96 1.00 0.98 0.96 1.00 0.98 0.96 1.00 0.98 0.96

Llama & Shkolnik (2015)

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Carrington rotation 2149 (April 2014)

Transiting the Sun I

Phase

Flux

1.00 0.98 0.96 1.00 0.98 0.96 1.00 0.98 0.96 1.00 0.98 0.96

08 April 2014 14 April 2014 20 April 2014 26 April 2014 02 May 2014

0.02

  • 0.02

0.02

  • 0.02

0.02

  • 0.02

0.02

  • 0.02

0.02

  • 0.02

Llama & Shkolnik (2015)

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Transiting the Sun I

Llama & Shkolnik (2015)

Soft X-ray (9.4 nm) FUV (170 nm) Optical (450 nm) Input Rp/R = 0.1

Histogram Fraction 0.2 0.4 0.6 0.8 1.0 0.1 0.15 0.05 Measured Rp/R 0.0

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Transiting the Sun I

Llama & Shkolnik (2015)

Histogram Fraction 0.2 0.4 0.6 0.8 1.0 0.0 0.1 0.15 0.05 Measured Rp/R

Soft X-ray (9.4 nm) FUV (170 nm) Optical (450 nm) Input Rp/R = 0.1

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Transiting the Sun II: Lyman-⍺

Llama & Shkolnik (2016) Data from SDO/EVE

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Llama & Shkolnik (2016)

Transiting the Sun II: Lyman-⍺

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Llama & Shkolnik (2016)

Transiting the Sun II: Lyman-⍺

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Llama & Shkolnik (2016)

Transiting the Sun II: Lyman-⍺

0.10

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Llama & Shkolnik (2016)

Transiting the Sun II: Lyman-⍺

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Llama & Shkolnik (2016)

Transiting the Sun II: Lyman-⍺

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Summary

  • Stellar activity needs to be taken into account in the

interpretation of these observations.

  • Simultaneous optical observations may help disentangle

stellar activity signatures in high energy transits.

  • X-ray / UV transits are a great tool to investigate the upper

atmospheres of exoplanets.