We present the results of a new series of nongray calculations of the atmospheres, spectra, colors, and evolution of extrasolar giant planets (EGPs) and brown dwarfs for effective temperatures below 1300 K This theory encompasses most of the mass/age parameter space occupied by substellar objects and is the first spectral study down to 100 K These calculations are in aid of the multitude of searches being conducted or planned around the world for giant planets and brown dwarfs and reveal the exotic nature of the class Generically, absorption by H2 at longer wavelengths and H2O opacity windows at shorter wavelengths conspire to redistribute flux blueward Below 1200 K, methane is the dominant carbon bearing molecule and is a universal diagnostic feature of EGP and brown dwarf spectra We find that the primary bands in which to search are Z (~105 ?m), J (~12 ?m), H (~16 ?m), K (~22 ?m), M (~5 ?m), and N (~10 ?m), that enhancements of the emergent flux over blackbody values, in particular in the near infrared, can be by many orders of magnitude, and that the infrared colors of EGPs and brown dwarfs are much bluer than previously believed In particular, relative to J and H, the K band flux is reduced by CH4 and H2 absorption Furthermore, we conclude that for Teff's below 1200 K most or all true metals may be sequestered below the photosphere, that an interior radiative zone is a generic feature of substellar objects, and that clouds of H2O and NH3 are formed for Teff's below ~400 and ~200 K, respectively This study is done for solar-metallicity objects in isolation and does not include the effects of stellar insulation Nevertheless, it is a comprehensive attempt to bridge the gap between the planetary and stellar realms and to develop a nongray theory of objects from 03MJ (Saturn) to 70MJ (~007 M?) We find that the detection ranges for brown dwarf/EGP discovery of both ground- and space-based telescopes are larger than previously estimated

https://iopscience.iop.org/article/10.1086/305002/pdf

A Nongray Theory of Extrasolar Giant Planets and Brown Dwarfs

We show that under certain circumstances the differences between the absorption mean and Planck mean opacities can lead to multiple solutions for an LTE atmospheric structure. Since the absorption and Planck mean opacities are not expected to differ significantly in the usual case of radiative equilibrium, nonirradiated atmospheres, the most interesting situations in which the effect may play a role are strongly irradiated stars and planets, and also possibly structures in which there is a significant deposition of mechanical energy, such as stellar chromospheres and accretion disks. We have presented an illustrative example of a strongly irradiated giant planet in which the bifurcation effect is predicted to occur for a certain range of distances from the star.

https://iopscience.iop.org/article/10.1086/377080/pdf

A Possible Bifurcation in Atmospheres of Strongly Irradiated Stars and Planets

The latest edition of the AFGL atmospheric absorption line parameters compilation for the seven most active infrared terrestrial absorbers is described. Major modifications to the atlas for this edition include updating of water-vapor parameters from 0 to 4300 per cm, improvements to line positions for carbon dioxide, substantial modifications to the ozone bands in the middle to far infrared, and improvements to the 7- and 2.3-micron bands of methane. The atlas now contains about 181,000 rotation and vibration-rotation transitions between 0 and 17,900 per cm. The sources of the absorption parameters are summarized.

AFGL atmospheric absorption line parameters compilation: 1982 edition.

▪ Abstract As progressively cooler stellar and substellar objects are discovered, the presence first of molecules and then of condensed particulates greatly complicates the understanding of their physical properties. Accurate model atmospheres that include these processes are the key to establishing their atmospheric parameters. They play a crucial role in determining structural characteristics by setting the surface conditions of model interiors and providing transformations to the various observational planes. They can reveal the spectroscopic properties of brown dwarfs and help establish their detectability. In this paper, we review the current state-of-the-art theory and modeling of the atmospheres of very low mass stars, including the coolest known M dwarfs, M subdwarfs, and brown dwarfs, i.e. Teff ≤ 4,000 K and −4.0 ≤ [M/H] ≤ +0.0. We discuss ongoing efforts to incorporate molecular and grain opacities in cool stellar spectra, as well as the latest progress in (a) deriving the effective temperature ...

Model atmospheres of very low mass stars and brown dwarfs

The Spherical Top Data System (STDS) software package for the simulation of spherical top spectra is presented. It consists of a single UNIX script with self-explanatory arguments allowing the non-expert user to calculate spectra from the results of the high resolution analyses performed over the recent decades on this type of molecules. More than one hundred parameter files are presently available including various band systems of 16 molecular species (among which methane is the most documented) and various types of calculations: rovibrational energy levels, i.r. absorption, Raman scattering and Stark coefficients. STDS is freely accessible by anonymous ftp at jupiter.u-bourgogne.fr. The basic instructions to get, install and execute STDS are explained. The current status of the STDS content is described.

Spherical top data system (STDS) software for the simulation of spherical top spectra

T.D.S. is a computer package concerned with high resolution spectroscopy of spherical top molecules like CH 4 , CF 4 , SiH 4 , SiF 4 , SnH 4 , GeH 4 , SF 6 , etc. T.D.S. contains information, fundamental spectroscopic data (energies, transition moments, spectroscopic constants) recovered from comprehensive modeling and simultaneous fitting of experimental spectra, and associated software written in C. The T.D.S. goal is to provide an access to all available information on vibration-rotation molecular states and transitions including various spectroscopic processes (Stark, Raman, etc.) under extended conditions based on extrapolations of laboratory measurements using validated theoretical models. Applications for T.D.S. may include: education/training in molecular physics, quantum chemistry, laser physics; spectroscopic applications (analysis, laser spectroscopy, atmospheric optics, optical standards, spectroscopic atlases); applications to environment studies and atmospheric physics (remote sensing); data supply for specific databases; and to photochemistry (laser excitation, multiphoton processes). The reported DOS-version is designed for IBM and compatible personal computers.

T.D.S. spectroscopic databank for spherical tops: DOS version

2014 A new simultaneous analysis of the v2 and v4 bands of 12CH4 has been carried out from infrared spectra recorded with a resolution of 0.05 cm-1. 973 transitions have been assigned to these two bands from P20 to R18. They have been fitted using a third order hamiltonian for diagonal terms as well as for off-diagonal terms. This model involves only 16 adjustable parameters which are all determined with an accuracy of the order of one per cent. The standard deviation of the fit is 17 mK. Tome 41 No 14 15 JUILLET 1980 LE JOURNAL DE PHYSIQUE LETTRES J. Physique LETTRES 41 (1980) L-319 L-323 15 JUILLET 1980,

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Extension de l'analyse simultanée des bandes v2 et v 4 de 12CH4

The paper analyzes line positions and absolute line strengths of Blatherwick et al. (1979), based on moderately high resolution spectra of methane between 1100 and 1800 per cm, obtained using the Fourier transform spectrometer and the multiple-pass cold cell at the NASA Ames Research Center. Hamiltonian models are used to calculate theoretical relative line strengths, which, in combination with measured line strengths, yield integrated band strengths for the fundamentals v2 and v4. Ratios of calculated intensities to experimental intensities are analyzed, and the systematic deviations in the P- and R-branches of the v2 band are found to be represented by a Herman-Wallis type factor for Coriolis interactions. An analysis of ratios of calculated to experimental intensities of the v4 band yields a small correction to the Herman-Wallis factor.

Quantum assignments and intensity measures for methane between 1100 and 1800 per CM - A comparison between theory and experiment

/pdf/les-bandes-de-difference-des-molecules-tetraedriques-5cb0k6pegc.pdf

C. Pierre

Papers

T.D.S. spectroscopic databank for spherical tops: DOS version

Extension de l'analyse simultanée des bandes v2 et v 4 de 12CH4

Quantum assignments and intensity measures for methane between 1100 and 1800 per CM - A comparison between theory and experiment

Les bandes de différence des molécules tétraédriques. Application : les bandes chaudes 2 ν4 — ν4 et ν 2 + ν4 — ν2 de 12CH 4