Searching for 3D effects in the optical, high spectral resolution emission spectrum of KELT-9b

2021 ◽  
Author(s):  
Lorenzo Pino ◽  
Matteo Brogi ◽  
Jean-Michel Désert ◽  
Emily Rauscher
Keyword(s):  
Emission Spectrum ◽  
Spectral Resolution ◽  
Planet Formation ◽  
Emission Spectra ◽  
Optical Emission ◽  
High Spectral Resolution ◽  
Optical Emission Spectrum ◽  
Hot Jupiters ◽  
Atmospheric Structure ◽  
3D Effects

<p>Ultra-hot Jupiters (UHJs; T<sub>eq</sub> ≥ 2500 K) are the hottest gaseous giants known. They emerged as ideal laboratories to test theories of atmospheric structure and its link to planet formation. Indeed, because of their high temperatures, (1) they likely host atmospheres in chemical equilibrium and (2) clouds do not form in their day-side. Their continuum, which can be measured with space-facilities, can be mostly attributed to H- opacity, an indicator of metallicity. From the ground, the high spectral resolution emission spectra of UHJs contains thousands of lines of refractory (Fe, Ti, TiO, …) and volatile species (OH, CO, …), whose combined atmospheric abundances could track planet formation history in a unique way. In this talk, we take a deeper look to the optical emission spectrum of KELT-9b covering planetary phases 0.25 - 0.75 (i.e. between secondary eclipse and quadrature), and search for the effect of atmospheric dynamics and three-dimensionality of the planet atmosphere on the resolved line profiles, in the context of a consolidated statistical framework. We discuss the suitability of the traditionally adopted 1D models to interprete phase-resolved observations of ultra-hot Jupiters, and the potential of this kind of observations to probe their 3D atmospheric structure and dynamics. Ultimately, understanding which factors affect the line-shape in UHJs will also lead to more accurate and more precise abundance measurements, opening a new window on exoplanet formation and evolution.</p>

Metals in the day-side of ultra-hot Jupiter atmospheres: a key test for planetary formation

2020 ◽  
Author(s):  
Lorenzo Pino ◽  
Jean-Michel Désert ◽  
Matteo Brogi ◽  
Valerio Nascimbeni ◽  
Aldo Stefano Bonomo ◽  
...  
Keyword(s):  
Emission Spectrum ◽  
Planet Formation ◽  
High Spectral Resolution ◽  
Optical Data ◽  
Thermal Inversion ◽  
Hot Jupiters ◽  
Refractory Elements ◽  
Metal Abundances ◽  
A New Technique ◽  
Side Emission

<p>Ultra-hot Jupiters (T<sub>eq</sub> ≥ 2,500 K) are the hottest gaseous giants known. They emerged as ideal laboratories to test theories of atmospheric structure and its link to planet formation. Indeed, because of their high temperatures, (1) they likely host atmospheres in chemical equilibrium and (2) clouds do not form in their day-side. Thousands of lines of refractory elements such as iron, normally inaccessible in planets, can be studied through high spectral resolution emission spectroscopy, providing a first look into the chemistry of refractory elements in exoplanets. In this talk we report the detection of neutral iron in the day-side emission spectrum of KELT-9b (T<sub>day</sub> ~ 4,000<span>  </span>K), the first detection of an atomic species in the emission spectrum of an exoplanet, obtained with HARPS-N optical data gathered in the framework of the GAPS collaboration. Our detection unambiguously indicates the presence of a thermal inversion in the atmosphere of the planet. We also present a new technique to extract planetary parameters from the cross-correlation function in a statistically sound framework, which makes possible the combination with information from the planetary continuum that can be obtained with complementary space facilities.<span> </span>This is a crucial step towards the measurement of metal abundances in exoplanets, a quantity that can be compared to predictions of planet formation theories. In the near future, our technique will be extended to cooler exoplanets. In the era of EELTs and JWST, this kind of measurements could ultimately open a new window on exoplanet formation and evolution.</p>

Time Evolution of Optical Emission Spectrum of a Hg-HID Lamp Exposed to X-ray

2010 ◽  
Vol 30 (4) ◽  
pp. 449-459 ◽  
Author(s):  
N. A. Harabor ◽  
A. Harabor ◽  
I. Palarie ◽  
I. M. Popescu ◽  
G. Zissis
Keyword(s):  
Emission Spectrum ◽  
Time Evolution ◽  
Optical Emission ◽  
Optical Emission Spectrum ◽  
X Ray

scholarly journals High spectral resolution interferometric planetary observations in the 7–25 μ region

1971 ◽  
Vol 40 ◽  
pp. 44-47
Author(s):  
R. A. Hanel ◽  
V. G. Kunde ◽  
T. Meilleur ◽  
G. Stambach
Keyword(s):  
Spectral Range ◽  
Spectral Resolution ◽  
Thermal Emission ◽  
Emission Spectra ◽  
Rotational Structure ◽  
High Spectral Resolution ◽  
The Moon ◽  
Broad Absorption ◽  
Ratio Spectrum ◽  
Venusian Atmosphere

The thermal emission spectra of Venus, Mars, Jupiter, and the moon were observed at the coude focus of the McDonald Observatory 107-inch telescope in the 400–1400 cm−1 spectral range with spectral resolutions of 0.3–0.7 cm−1. A preliminary interpretation of the Venus/lunar ratio spectrum allows identification of four upper state CO2 bands in the Venusian atmosphere at 791, 828, 865, and 961 cm−1 and confirms previous observations of the broad absorption-like depression around 890 cm−1. The rotational structure of the 791 and 961 cm−1 bands is well developed at this spectral resolution.

Etude des molécules diatomiques. Partie II : Intensités

1977 ◽  
Vol 55 (20) ◽  
pp. 1775-1786
Author(s):  
Jean-Louis Féménias
Keyword(s):  
Emission Spectrum ◽  
Electronic States ◽  
Optical Emission ◽  
Wave Functions ◽  
Effective Hamiltonian ◽  
Intensity Factors ◽  
Optical Emission Spectrum ◽  
Analytical Expressions ◽  
General Method ◽  
Numerical Approaches

Theory of perturbations, giving the diatomic effective Hamiltonian, is used for calculating actual molecular wave functions and intensity factors involved in transitions between states arising from Hund's coupling cases a, b, intermediate a–b, and c tendency. The Herman and Wallis corrections are derived, without any knowledge of the analytical expressions of the wave functions, and generalized to transitions between electronic states with whatever symmetry and multiplicity. A general method for studying perturbed intensities is presented, taking in good part the spectroscopic modern numerical approaches. The method is used in the study of the ScO optical emission spectrum.

Optical Emission Spectrum Processing Using Wavelet Compression During Wafer Fabrication

2017 ◽  
Vol 30 (4) ◽  
pp. 380-387 ◽  
Author(s):  
Taikang Ning ◽  
Chung Ho Huang ◽  
John Albert Jensen ◽  
Vincent Wong ◽  
Henry Chan
Keyword(s):  
Emission Spectrum ◽  
Optical Emission ◽  
Wafer Fabrication ◽  
Optical Emission Spectrum ◽  
Wavelet Compression

scholarly journals Characterizing the Atmospheres of Hot Jupiters: From Spectra to Multi-Color Maps

2008 ◽  
Vol 4 (S253) ◽  
pp. 255-261
Author(s):  
Heather A. Knutson
Keyword(s):  
Emission Spectrum ◽  
Inversion Layer ◽  
Emission Spectra ◽  
Phase Curve ◽  
Hot Jupiters ◽  
Thermal Phase ◽  
Additional Support ◽  
Temperature Inversions ◽  
The Relationship ◽  
Hot Jupiter

AbstractWe present new observations of the emission spectrum of the hot Jupiter TrES-4 designed to test the theory that the presence of temperature inversions in the atmospheres of these planets are correlated with the amount of radiation received by the planet. Our observations reveal that TrES-4 has an emission spectrum similar to that of HD 209458b, which requires the presence of an inversion layer high in the atmosphere and water emission bands in order to explain the observed features, providing additional support for that theory. We also present new observations of the thermal phase curve of HD 189733b at 24 μm, which we combine with our previous observations at 8 μm to examine how circulation in this planet's atmosphere varies as a function of depth. We discuss the relationship between the strength of the day-night circulation on both planets and their other observable properties, in particular their emission spectra.

Determination of the reduced electric field in surface dielectric barrier discharge plasmas

2021 ◽  
Vol 103 (3) ◽  
pp. 35-44
Author(s):  
А.А. Mutalip ◽  
◽  
Y.А. Ussenov ◽  
А.K. Akildinova ◽  
М.K. Dosbolayev ◽  
...  
Keyword(s):  
Electric Field ◽  
Emission Spectrum ◽  
Barrier Discharge ◽  
Block Diagram ◽  
Average Energy ◽  
Optical Emission ◽  
Spectral Lines ◽  
Surface Barrier ◽  
Optical Emission Spectrum

In this paper, the experimental determination of the reduced electric field (E/n) in plasma of dielectric coplanar surface barrier discharge (DCSBD) at atmospheric pressure was demonstrated. The plasma characteristics and the experimental setup properties were described, and the optical emission spectrum of the plasma was also measured. The results of optical emission spectroscopy showed the presence of nitrogen molecular bands in the emission spectrum of DCSBD. In particular, the second positive and the first negative systems, as well as low intensity OH and NO lines were identified. The main transport properties of electrons, such as mobility, mean average energy, and diffusion coefficients were calculated using the BOLSIG+ open source software. The dependence of the ratio of intensities of the nitrogen spectral lines on the reduced electric field, the dependence of the E/n on plasma power, and the dependence of the electron energy distribution function (EEDF) on E/n were obtained. An algorithm in the form of a block diagram for determining the reduced electric field by the BOLSIG + program and experimentally measured spectral line intensities are presented. The utilized method is quite simple, accessible and versatile.

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