Calculation of the H Lyman α emission of the hot Jupiters HD 209458b and HD 189733b

Menager, H.; Barthélemy, Mathieu; Koskinen, Tommi; Lilensten, Jean; Ehrenreich, D.; Parkinson, C. D.

doi:10.1016/j.icarus.2013.02.028

Cited by 18 publications

(25 citation statements)

References 65 publications

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“…Since Lyman a is by far the most intense line in the FUV solar spectrum, this line, alone, can significantly modify the atmospheric structure and thermodynamics. Recent models showed that the Lyman a cooling can significantly modify the temperature of the upper atmosphere of hot Jupiters (Menager et al 2013). In these cases, the problem is to know precisely the full solar disk intensity and the profile of one particular emission line.…”

Section: Optically Thick Cases: Example Of the Planetary H-lyman A Emmentioning

confidence: 99%

“…Since the discovery of a large panel of exoplanets (940 at the end of August 2013; www.exoplanet.eu) and the detection by transit absorption of two atmospheres (Vidal-Madjar et al 2003;Lecavelier Des Etangs et al 2010), the question of a diagnostic of their upper atmospheres using the thermospheric emissions is open (Menager et al 2013). As stated in Menager et al (2013) for exoplanets and in Section 5 of this paper for giant planets, the problem of the intensity and shape of the Lyman a line is critical to model the emission coming from the planet considering the fact that it represents the main part of the planetary emission.…”

Section: Stellar Uv Flux In the Case Of Exoplanetsmentioning

confidence: 99%

“…As stated in Menager et al (2013) for exoplanets and in Section 5 of this paper for giant planets, the problem of the intensity and shape of the Lyman a line is critical to model the emission coming from the planet considering the fact that it represents the main part of the planetary emission. It is also important to notice that the exosphere or hydrogen corona of these planets can reach very high temperatures above 10 4 K, and thus enhance the planetary line width.…”

Section: Stellar Uv Flux In the Case Of Exoplanetsmentioning

confidence: 99%

“…In order to explore possible future auroral or dayglow diagnostic of exoplanets, the calculations in Menager et al (2013) also used the family of Trans* code simulations, calculating the transport of the electrons through the atmosphere. This simulation thus needs the EUV and FUV flux (the stellar wind and the magnetospheric interactions also) of a large panel of stars hosting planets.…”

Section: Stellar Uv Flux In the Case Of Exoplanetsmentioning

confidence: 99%

“…These processes induce electron production and photo excitation that can be measured remotely, and give rise to a large panel of observable quantities. This opens the possibility to diagnose the upper atmospheres of solar system objects but also, in the near future, of exoplanets (Menager et al 2013). In most cases, except for the Earth case and space missions, information about planetary upper atmosphere is derived from remote sensing of the light emissions and thus the photoexcitation.…”

Section: Introduction and Motivationsmentioning

confidence: 99%

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Sensitivity of upper atmospheric emissions calculations to solar/stellar UV flux

Barthélemy

Cessateur

2014

J. Space Weather Space Clim.

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The solar UV (UltraViolet) flux, especially the EUV (Extreme UltraViolet) and FUV (Far UltraViolet) components, is one of the main energetic inputs for planetary upper atmospheres. It drives various processes such as ionization, or dissociation which give rise to upper atmospheric emissions, especially in the UV and visible. These emissions are one of the main ways to investigate the upper atmospheres of planets. However, the uncertainties in the flux measurement or modeling can lead to biased estimates of fundamental atmospheric parameters, such as concentrations or temperatures in the atmospheres. We explore the various problems that can be identified regarding the uncertainties in solar/stellar UV flux by considering three examples. The worst case appears when the solar reflection component is dominant in the recorded spectrum as is seen for outer solar system measurements from HST (Hubble Space Telescope). We also show that the estimation of some particular line parameters (intensity and shape), especially Lyman a, is crucial, and that both total intensity and line profile are useful. In the case of exoplanets, the problem is quite critical since the UV flux of their parent stars is often very poorly known.

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Section: Optically Thick Cases: Example Of the Planetary H-lyman A Emmentioning

confidence: 99%

Section: Stellar Uv Flux In the Case Of Exoplanetsmentioning

confidence: 99%

Section: Stellar Uv Flux In the Case Of Exoplanetsmentioning

confidence: 99%

Section: Stellar Uv Flux In the Case Of Exoplanetsmentioning

confidence: 99%

Section: Introduction and Motivationsmentioning

confidence: 99%

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Sensitivity of upper atmospheric emissions calculations to solar/stellar UV flux

Barthélemy

Cessateur

2014

J. Space Weather Space Clim.

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Building galaxies, stars, planets and the ingredients for life between the stars. The science behind the European Ultraviolet-Visible Observatory

Castro

Appourchaux

Barstow

et al. 2014

Astrophys Space Sci

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This contribution gathers the contents of the white paper submitted by the UV community to the Call issued by the European Space Agency in March 2013, for the definition of the L2 and L3 missions in the ESA science program. We outlined the key science that a large UV facility would make possible and the instrumentation to be implemented. The growth of luminous structures and the building blocks of life in the Universe began as primordial gas was processed in stars and mixed at galactic scales. The mechanisms responsible for this development are not wellunderstood and have changed over the intervening 13 billion years. To follow the evolution of matter over cosmic time, it is necessary to study the strongest (resonance) transitions of the most abundant species in the Universe. Most of them are in the ultraviolet (UV; 950 Å–3000 Å) spectral range that is unobservable from the ground. A versatile space observatory with UV sensitivity a factor of 50–100 greater than existing facilities will revolutionize our understanding of the Universe. Habitable planets grow in protostellar discs under ultraviolet irradiation, a by-product of the star-disk interaction that drives the physical and chemical evolution of discs and young planetary systems. The electronic transitions of the most abundant molecules are pumped by this UV field, providing unique diagnostics of the planet-forming environment that cannot be accessed from the ground. Earth’s atmosphere is in constant interaction with the interplanetary medium and the solar UV radiation field. A 50–100 times improvement in sensitivity would enable the observation of the key atmospheric ingredients of Earth-like exoplanets (carbon, oxygen, ozone), provide crucial input for models of biologically active worlds outside the solar system, and provide the phenomenological baseline to understand the Earth atmosphere in context

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Can hydrogen coronae be inferred around a CO2-dominated exoplanetary atmosphere?

Bernard

Lilensten

Barthélemy

et al. 2014

Icarus

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Calculation of the H Lyman α emission of the hot Jupiters HD 209458b and HD 189733b

Cited by 18 publications

References 65 publications

Sensitivity of upper atmospheric emissions calculations to solar/stellar UV flux

Sensitivity of upper atmospheric emissions calculations to solar/stellar UV flux

Building galaxies, stars, planets and the ingredients for life between the stars. The science behind the European Ultraviolet-Visible Observatory

Can hydrogen coronae be inferred around a CO2-dominated exoplanetary atmosphere?

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