Temperature inversions on hot super-Earths: the case of CN in nitrogen-rich atmospheres

ABSTRACT We show that in extremely irradiated atmospheres of hot super-Earths shortwave absorption of CN can cause strong temperature inversions. We base this study on previous observations of 55 Cancri e, which lead us to believe that ultrashort-period super-Earths can sustain volatile atmospheres, rich in nitrogen and/or carbon. We compute our model atmospheres in a radiative-convective equilibrium for a variety of nitrogen-rich cases and orbital parameters. We demonstrate the effects caused by thermal inversions on the chemistry and compute low-resolution synthetic emission spectra for a range of 0.5–28 $\rm{\mu m}$. Our results indicate that due to shortwave absorption of CN, atmospheres with temperatures above 2000 K and C/O ≥ 1.0 are prone to thermal inversions. CN is one of the few molecules that is extremely stable at large temperatures occurring on the dayside of short-period super-Earths. The emission spectrum of such atmospheres will differ substantially from non-inverted cases. In the case of inversions, absorption features become inverted, showing higher than expected flux. We propose that inversions in hot atmospheres should be the expected norm. Hot super-Earths are some of the most extreme natural laboratories for testing predictions of atmospheric chemistry and structure. They are frequently occurring, bright in emission and have short orbital periods. All these factors make them perfect candidates to be observed with JWST and ARIEL missions.

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

Proceedings of the International Astronomical Union ◽

10.1017/s1743921308026471 ◽

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.

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From the Oort cloud to Halley-type comets

International Astronomical Union Colloquium ◽

10.1017/s0252921100031638 ◽

1999 ◽

Vol 173 ◽

pp. 327-338 ◽

Cited By ~ 5

Author(s):

J.A. Fernández ◽

T. Gallardo

Keyword(s):

Total Population ◽

Complex Function ◽

Dynamical Evolution ◽

Oort Cloud ◽

Capture Process ◽

Influx Rate ◽

Short Period ◽

Dynamical Properties ◽

Orbital Periods ◽

Probability Of Capture

AbstractThe Oort cloud probably is the source of Halley-type (HT) comets and perhaps of some Jupiter-family (JF) comets. The process of capture of Oort cloud comets into HT comets by planetary perturbations and its efficiency are very important problems in comet ary dynamics. A small fraction of comets coming from the Oort cloud − of about 10−2− are found to become HT comets (orbital periods < 200 yr). The steady-state population of HT comets is a complex function of the influx rate of new comets, the probability of capture and their physical lifetimes. From the discovery rate of active HT comets, their total population can be estimated to be of a few hundreds for perihelion distancesq <2 AU. Randomly-oriented LP comets captured into short-period orbits (orbital periods < 20 yr) show dynamical properties that do not match the observed properties of JF comets, in particular the distribution of their orbital inclinations, so Oort cloud comets can be ruled out as a suitable source for most JF comets. The scope of this presentation is to review the capture process of new comets into HT and short-period orbits, including the possibility that some of them may become sungrazers during their dynamical evolution.

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The White Dwarf Mass and Orbital Period Distribution in Zero-Age Cataclysmic Binaries

International Astronomical Union Colloquium ◽

10.1017/s0252921100100028 ◽

1989 ◽

Vol 114 ◽

pp. 440-442

Author(s):

M. Politano ◽

R. F. Webbink

Keyword(s):

Star Formation ◽

White Dwarf ◽

Galactic Disk ◽

Orbital Energy ◽

Orbital Parameter ◽

Orbital Parameters ◽

Cataclysmic Binaries ◽

Magnetic Braking ◽

Orbital Periods ◽

The Individual

A zero-age cataclysmic binary (ZACB) we define as a binary system at the onset of interaction as a cataclysmic variable. We present here the results of calculations of the distributions of white dwarf masses and of orbital periods in ZACBs, due to binaries present in a stellar population which has undergone continuous, constant star formation for 1010 years.Distributions of ZACBs were calculated for binaries formed t years ago, for log t = 7.4 (the youngest age at which viable ZACBs can form) to log t = 10.0 (the assumed age of the Galactic disk), in intervals of log t = 0.1. These distributions were then integrated over time to obtain the ZACB distribution for a constant rate of star formation. To compute the individual distributions for a given t, we require the density of systems forming (number of pre-cataclysmics forming per unit volume of orbital parameter space), n£(t), and the rates at which the radii of the secondary and of its Roche lobe are changing in time, s (t) and L, s (t), respectively. In calculating nf(t), we assume that the distribution of the orbital parameters in primordial (ZAMS) binaries may be written as the product of the distribution of masses of ZAMS stars (Miller and Scalo 1979), the distribution of mass ratios in ZAMS binaries (cf. Popova, et al., 1982), and the distribution of orbital periods in ZAMS binaries (Abt 1983). In transforming the the orbital parameters from progenitor (ZAMS) to offspring (ZACB) binaries, we assume that all of the orbital energy deposited into the envelope during the common envelope phase leading to ZACB formation goes into unbinding that envelope. R.L, s (t) is determined from orbital angular momentum loss rates due to gravitational radiation (Landau and Lifshitz 1951) and magnetic braking (γ = 2 in Rappaport, Verbunt, and Joss 1983). We turn off magnetic braking if the secondary is completely convective.

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

10.5194/epsc2021-308 ◽

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

Ultra-hot Jupiters (UHJs; Teq &#8805; 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, &#8230;) and volatile species (OH, CO, &#8230;), 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.

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VLT/SPHERE astrometric confirmation and orbital analysis of the brown dwarf companion HR 2562 B

Astronomy and Astrophysics ◽

10.1051/0004-6361/201732476 ◽

2018 ◽

Vol 615 ◽

pp. A177 ◽

Cited By ~ 3

Author(s):

A.-L. Maire ◽

L. Rodet ◽

C. Lazzoni ◽

A. Boccaletti ◽

W. Brandner ◽

...

Keyword(s):

Orbital Motion ◽

Orbital Plane ◽

Real Data ◽

Far Infrared ◽

Brown Dwarf ◽

Orbital Parameters ◽

System A ◽

Low Mass ◽

Debris Disk ◽

Orbital Periods

Context. A low-mass brown dwarf has recently been imaged around HR 2562 (HD 50571), a star hosting a debris disk resolved in the far infrared. Interestingly, the companion location is compatible with an orbit coplanar with the disk and interior to the debris belt. This feature makes the system a valuable laboratory to analyze the formation of substellar companions in a circumstellar disk and potential disk-companion dynamical interactions. Aims. We aim to further characterize the orbital motion of HR 2562 B and its interactions with the host star debris disk. Methods. We performed a monitoring of the system over ~10 months in 2016 and 2017 with the VLT/SPHERE exoplanet imager. Results. We confirm that the companion is comoving with the star and detect for the first time an orbital motion at high significance, with a current orbital motion projected in the plane of the sky of 25 mas (~0.85 au) per year. No orbital curvature is seen in the measurements. An orbital fit of the SPHERE and literature astrometry of the companion without priors on the orbital plane clearly indicates that its orbit is (quasi-)coplanar with the disk. To further constrain the other orbital parameters, we used empirical laws for a companion chaotic zone validated by N-body simulations to test the orbital solutions that are compatible with the estimated disk cavity size. Non-zero eccentricities (>0.15) are allowed for orbital periods shorter than 100 yr, while only moderate eccentricities up to ~0.3 for orbital periods longer than 200 yr are compatible with the disk observations. A comparison of synthetic Herschel images to the real data does not allow us to constrain the upper eccentricity of the companion.

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On the synergy between Ariel and ground-based high-resolution spectroscopy

Experimental Astronomy ◽

10.1007/s10686-021-09824-7 ◽

2022 ◽

Author(s):

Gloria Guilluy ◽

Alessandro Sozzetti ◽

Paolo Giacobbe ◽

Aldo S. Bonomo ◽

Giuseppina Micela

Keyword(s):

High Resolution ◽

Near Infrared ◽

Major Axis ◽

High Resolution Spectroscopy ◽

Correlation Technique ◽

Temperature Structure ◽

Low Resolution ◽

Semi Major Axis ◽

Species Discovery ◽

Orbital Parameters

AbstractSince the first discovery of an extra-solar planet around a main-sequence star, in 1995, the number of detected exoplanets has increased enormously. Over the past two decades, observational instruments (both onboard and on ground-based facilities) have revealed an astonishing diversity in planetary physical features (i. e. mass and radius), and orbital parameters (e.g. period, semi-major axis, inclination). Exoplanetary atmospheres provide direct clues to understand the origin of these differences through their observable spectral imprints. In the near future, upcoming ground and space-based telescopes will shift the focus of exoplanetary science from an era of “species discovery” to one of “atmospheric characterization”. In this context, the Atmospheric Remote-sensing Infrared Exoplanet Large (Ariel) survey, will play a key role. As it is designed to observe and characterize a large and diverse sample of exoplanets, Ariel will provide constraints on a wide gamut of atmospheric properties allowing us to extract much more information than has been possible so far (e.g. insights into the planetary formation and evolution processes). The low resolution spectra obtained with Ariel will probe layers different from those observed by ground-based high resolution spectroscopy, therefore the synergy between these two techniques offers a unique opportunity to understanding the physics of planetary atmospheres. In this paper, we set the basis for building up a framework to effectively utilise, at near-infrared wavelengths, high-resolution datasets (analyzed via the cross-correlation technique) with spectral retrieval analyses based on Ariel low-resolution spectroscopy. We show preliminary results, using a benchmark object, namely HD 209458 b, addressing the possibility of providing improved constraints on the temperature structure and molecular/atomic abundances.

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Causes of Color in Minerals and Gemstones

Microscopy Today ◽

10.1017/s1551929500056406 ◽

2001 ◽

Vol 9 (2) ◽

pp. 14-17

Author(s):

Paul F. Hlava

Keyword(s):

Emission Spectrum ◽

White Light ◽

Emission Spectra ◽

Light Sources ◽

Physical Phenomena

The colors that one sees when looking at a mineral or gemstone are due to the response of that person's eye to the energies of the light, the emission spectrum of the illumination, and, most importantly, physical phenomena in the material that cause some colors to be absorbed while others are undisturbed or enhanced. It is beyond the scope of this article to do more than touch on the physiology of the eye that allows us to see colors. Likewise, we will not dwell on the emission spectra of various light sources. Rather, we will concentrate on the various ways in which materials, especially minerals and their heights of perfection, gemstones, produce color from white light.

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The impact of time-dependent stellar activity on the atmospheric chemistry and observability of exoplanets

10.5194/epsc2021-685 ◽

2021 ◽

Author(s):

Amy Louca ◽

Yamila Miguel ◽

Shang-Min Tsai

Keyword(s):

Atmospheric Chemistry ◽

Emission Spectra ◽

Time Dependent ◽

Radiative Transfer Model ◽

Transfer Model ◽

Stellar Spectrum ◽

Stellar Spectra ◽

Chemical Tracers ◽

Atmospheric Escape ◽

The Impact

Observations of exoplanets used to characterize the chemistry and dynamics of atmospheres have developed considerably throughout the years. Nonetheless, it remains a difficult task to give a full and detailed description using solely observations. With future space missions such as JWST and ARIEL, both expected to be launched within this decade, it becomes even more crucial to be able to fully explain and predict the underlying chemistry and physics involved. In this research, we focus on modeling star-planet interactions by using synthetic flare spectra to predict chemical tracers for future missions. We make use of a chemical kinetics code that includes synthetic time-dependent stellar spectra and thermal atmospheric escape to simulate the atmospheres of known exoplanets. Using a radiative transfer model we then retrieve emission spectra. This ongoing study is focused on various known planetary systems of which the stellar spectrum has been obtained by the (mega-)MUSCLES collaboration. Preliminary results on these systems show that stellar flares and thermal escape can have a significant effect on the chemistry in atmospheres.&#160;

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Radial Velocity Variations in Cool Supergiants

International Astronomical Union Colloquium ◽

10.1017/s0252921100098900 ◽

1984 ◽

Vol 88 ◽

pp. 283-288

Author(s):

Hugh C. Harris

Keyword(s):

Radial Velocity ◽

Main Sequence ◽

Short Period ◽

Cool Stars ◽

Synchronous Rotation ◽

Red Supergiants ◽

Velocity Variations ◽

Orbital Periods ◽

Low Amplitude ◽

Good Agreement

AbstractA survey of F, G, and W supergiants has been carried out with the DAO radial velocity spectrometer, an efficient instrument for detecting low-amplitude velocity variations in cool stars. Observations of 78 stars over five seasons show generally good agreement with OORAVEL results for spectroscopie binaries. The majority of supergiants show low-amplitude variability, with amplitudes typically 1 to 2 km s−1. The width of the cross-correlation profile has been measured for 58 supergiants. It reveals 14 stars with unusually broad lines, indicative of rotation velocities of 15 to 35 km s−1. Several have short-period binary companions and may be in synchronous rotation. The other broad-lined stars are apparently single or with long orbital periods; they may be making their first transition from the main sequence to become red supergiants.

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Classical Novae – Before and After Outburst

International Astronomical Union Colloquium ◽

10.1017/s0252921100093908 ◽

1988 ◽

Vol 108 ◽

pp. 226-231

Author(s):

Mario Livio

Keyword(s):

White Dwarf ◽

Main Sequence ◽

Orbital Parameters ◽

Classical Novae ◽

Classical Nova ◽

Before And After ◽

Low Mass ◽

Orbital Periods ◽

Thermonuclear Runaway ◽

Nova Outburst

Classical nova (CN) and dwarf nova (DN) systems have the same binary components (a low-mass main sequence star and a white dwarf) and the same orbital periods. An important question that therefore arises is: are these systems really different ? (and if so, what is the fundamental difference ?) or, are these the same systems, metamorphosing from one class to the other ?The first thing to note in this respect is that the white dwarfs in DN systems are believed to accrete continuously (both at quiescence and during eruptions). At the same time, both analytic (e.g. Fujimoto 1982) and numerical calculations show, that when sufficient mass accumulates on the white dwarf, a thermonuclear runaway (TNR) is obtained and a nova outburst ensues (see e.g. reviews by Gallagher and Starrfield 1978, Truran 1982). It is thus only natural, to ask the question, is the fact that we have not seen a DN undergo a CN outburst (in about 50 years of almost complete coverage) consistent with observations of DN systems ? In an attempt to answer this question, we have calculated the probability for a nova outburst not to occur (in 50 years) in 86 DN systems (for which at least some of the orbital parameters are known).

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