The role of planetary formation and evolution in shaping the composition of exoplanetary atmospheres

Turrini, D.; Nelson, Richard P.; Barbieri, M.

doi:10.1007/s10686-014-9401-6

Cited by 26 publications

(43 citation statements)

References 49 publications

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“…However, once it reaches its final mass Jupiter is more efficient in ejecting the planetesimals from the Solar System than in accreting them (Weidenschilling 1975;Guillot and Gladman 2000;Turrini et al 2014). Moreover, the flux of material crossing the orbit of the planet rapidly decreases with time.…”

Section: Implications For the Origins Of Jupiter And The Solar Systemmentioning

confidence: 99%

JIRAM, the Jovian Infrared Auroral Mapper

et al. 2014

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JIRAM is an imager/spectrometer on board the Juno spacecraft bound for a polar orbit around Jupiter. JIRAM is composed of IR imager and spectrometer channels. Its scientific goals are to explore the Jovian aurorae and the planet's atmospheric structure, dynamics and composition. This paper explains the characteristics and functionalities of the instrument and reports on the results of ground calibrations. It discusses the main subsystems to the extent needed to understand how the instrument is sequenced and used, the purpose of the calibrations necessary to determine instrument performance, the process for generating the commanding sequences, the main elements of the observational strategy, and the format of the scientific data that JIRAM will produce.

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Section: Implications For the Origins Of Jupiter And The Solar Systemmentioning

confidence: 99%

JIRAM, the Jovian Infrared Auroral Mapper

et al. 2014

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“…The study of the contributions of comets to the composition of giant planet atmospheres will not only benefit the Solar System atmosphere field but also the growing field of exoplanet atmosphere characterization (Turrini et al 2014). …”

Section: New Impacts?mentioning

confidence: 99%

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

et al. 2015

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Comets play a dual role in understanding the formation and evolution of the solar system. First, the composition of comets provides information about the origin of the giant planets and their moons because comets formed early and their composition is not expected to have evolved significantly since formation. They, therefore serve as a record of conditions during the early stages of solar system formation. Once comets had formed, their orbits were perturbed allowing them to travel into the inner solar system and impact the planets. In this way they contributed to the volatile inventory of planetary atmospheres. We review here how knowledge of comet composition up to the time of the Rosetta mission has contributed to understanding the formation processes of the giant planets, their moons and small icy bodies in the solar system. We also discuss how comets contributed to the volatile inventories of the giant and terrestrial planets.

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“…Because giant planets play a pivotal role in shaping planetary systems (e.g. [172,173]), determining precisely their internal structure and composition is essential to understand how planets form. In particular, the abundances of high-Z elements compared to the stellar values and the relative ratios of the different elements (e.g.…”

Section: Major Classes Of Planetary Atmospheres: What Should We Expect?mentioning

confidence: 99%

“…& understand the early stage of planetary and atmospheric formation during the nebular phase and the immediately following few millions years [173] & test the effectiveness of the physical processes directly responsible for their evolution.…”

Section: Gaseous Exoplanetsmentioning

confidence: 99%

“…For the purpose of illustration, Turrini et al [173] have considered a number of simplified planetary accretion and migration (i) Giant planet formation via gravitational instability that occurs during the earliest phases of protoplanetary disc evolution will result initially in planets with bulk and atmospheric abundances reflecting that of the protoplanetary disc. Recent studies show that formation is followed by rapid inward migration on time scales1 0 3 years [14,196], too short for significant dust growth or planetesimal formation to arise between formation and significant migration occurring.…”

Section: Chemical Composition Of Gaseous Planets: a Pointer To Planetmentioning

confidence: 99%

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The EChO science case

et al. 2015

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The discovery of almost two thousand exoplanets has revealed an unexpectedly diverse planet population. We see gas giants in few-day orbits, whole multi-planet systems within the orbit of Mercury, and new populations of planets with masses between that of the Earth and Neptune-all unknown in the Solar System. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? How do planetary systems work and what causes the exceptional diversity observed as compared to the Solar System? The EChO (Exoplanet Characterisation Observatory) space mission was conceived to take up the challenge to explain this diversity in terms of formation, evolution, internal structure and planet and atmospheric composition. This requires in-depth spectroscopic knowledge of the atmospheres of a large and well-defined planet sample for which precise physical, chemical and dynamical information can be obtained. In order to fulfil this ambitious scientific program, EChO was designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large, diverse and well-defined planet sample within its 4-year mission lifetime. The transit and eclipse spectroscopy method, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allows us to measure atmospheric signals from the planet at levels of at least 10 −4 relative to the star. This can only be achieved in conjunction with a carefully designed stable payload and satellite platform. It is also necessary to provide broad instantaneous wavelength coverage to detect as many molecular species as possible, to probe the thermal structure of the planetary atmospheres and to correct for the contaminating effects of the stellar photosphere. This requires wavelength coverage of at least 0.55 to 11 μm with a goal of covering from 0.4 to 16 μm. Only modest spectral resolving power is needed, with R~300 for wavelengths less than 5 μm and R~30 for wavelengths greater than this. spectroscopy technique means that no spatial resolution is required. A telescope collecting area of about 1 m 2 is sufficiently large to achieve the necessary spectro-photometric precision: for the Phase A study a 1.13 m 2 telescope, diffraction limited at 3 μm has been adopted. Placing the satellite at L2 provides a cold and stable thermal environment as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. EChO has been conceived to achieve a single goal: exoplanet spectroscopy. The spectral coverage and signal-to-noise to be achieved by EChO, thanks to its high stability and dedicated design, would be a game changer by allowing atmospheric composition to be measured with unparalleled exactness: at least a factor 10 more precise and a factor 10 to 1000 more accurate tha...

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The role of planetary formation and evolution in shaping the composition of exoplanetary atmospheres

Cited by 26 publications

References 49 publications

JIRAM, the Jovian Infrared Auroral Mapper

JIRAM, the Jovian Infrared Auroral Mapper

Constraints from Comets on the Formation and Volatile Acquisition of the Planets and Satellites

The EChO science case

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