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recent improvements in the capabilities of space- and ground-based telescopes as well as data reduction techniques have enabled us to characterize the atmospheres of exoplanets in exquisite detail, revealing a diverse range of properties. phase curve observations, which track the variation in the infrared brightness of... | multiband spitzer phase curves of three highly-irradiated hot jupiters |
in climate evolution studies, nitrogen once had the reputation of being a rather dull gas, thanks to its chemical stability and lack of direct greenhouse effects. this reputation has been decisively broken over the last few years by studies suggesting that its long-term cycling on earth may have been significant and th... | nitrogen, redox and life on the early earth |
with a large variety of observations available for some exoplanets and the development of sophisticated software suites, we are now able to conduct comprehensive global analyses to understand their composition and atmospheric properties. here we present a global analysis of spitzer observations, tess photometry, ground... | a comprehensive study of the hot jupiter kelt-14 b/wasp-122 b |
the composition of a planet reflects the primordial composition of the proto-planetary disk, location of formation, as well as post-processing mechanisms (such as giant impacts and atmospheric escape) that can alter the final inventory of a planet. i will focus on the results from composition constraints on low-mass ex... | super-earths composition: signatures of planet formation |
planetary transits of ultracool dwarfs (ucds, teff < 3000 k) provide our only opportunity to characterize terrestrial exoplanets in detail in the next 20 years. the speculoos transit survey is leading the effort to discover these worlds, using a network of six 1-meter telescopes on three continents to search for pla... | spectroscopic confirmation of dozens of nearby ultracool dwarfs from speculoos |
we used a suite of planetary atmospheres to calculate the refracted light signal. we have selected a combination of solar system analogs as well possible super-earth and mini-neptune atmospheres to cover a wide range of potential planetary atmospheres. we assumed the h2-dominated atmospheres have a solar h/he ratio (90... | vizier online data catalog: refracted light signals to discriminate exoplanets (misra+, 2014) |
1. introductionfor exoplanets with t < ~1500 k, photochemistry can seriously affect the atmospheric gas-phase composition [1] — on the one hand by destructing major molecules such as carbon monoxide (co), water (h2o), or methane (ch4) and on the other hand by enhancing the formation of more complex species such as a... | experimental investigation of the photochemical production of hydrocarbons in warm giant exoplanet atmospheres |
we propose to build a versatile set of self-consistent atmospheric models for hot rocky exoplanets and use them to predict their transit and eclipse spectra. hot rocky exoplanets will form the majority of small planets in close-in orbits to be discovered by the tess and kepler k2 missions, and offer the best opportunit... | model atmospheres and transit spectra for hot rocky planets |
it has been found that sub-neptune-sized planets, although not existing in our solar system, are ubiquitous in our interstellar neighborhood. this revelation is profound because, due to their special sizes and proximity to their host stars, neptune- and sub-neptune-sized exoplanets may have highly evolved atmospheres. ... | equilibrium and disequilibrium chemistry in evolved exoplanet atmospheres |
context. substellar objects such as brown dwarfs and hot jupiter exoplanets are cool enough that clouds can form in their atmospheres (helling & casewell 2014; a&arv 22)). unlike earth, where cloud condensation nuclei are provided by the upward motion of sand or ash, in brown dwarf and hot jupiters these conden... | assessing nucleation in cloud formation modelling for brown dwarf and exoplanet atmospheres |
on october 31, 2009, the photodetector array camera and spectrometer (pacs) onboard the herschel space observatory observed far infrared (fir) spectra of jupiter in the wavelength range between 55 and 210 µm in the framework of the program "water and related chemistry in the solar system" [hartogh et al., 2009]. we aim... | retrieval of jupiter's atmospheric parameters using far infrared spectra measured with pacs onboard the herschel space observatory |
wasp-121b is one of the standout exoplanets available for atmospheric characterization, both in transmission and emission, due to its large radius (1.8 jupiter radii), high temperature ( 2700k), and bright host star (h=9.4mag). recent hst/wfc3 eclipse observations made by our group have revealed the 1.4 micron water ba... | a global map of the atmospheric circulation and thermal structure for an ultrahot exoplanet |
science goals and objectives: the determination of accurate physical parameters for stars which host exoplanets is a crucial step in characterizing the size and nature of the planets themselves; one can only know the planet to the level that the host star is known. this program will carry out a detailed spectral analys... | it's elementary: chemical compositions and characterization of exoplanet-hosting m-dwarfs using apogee |
clouds in atmospheres of exoplanets play a key role in understanding their climate and radiative balance. they can also complicate the detection of chemical species in the atmosphere by flattening the spectra or by creating degeneracies between observables (kitzmann et al. 2011, line and parmentier 2016) polarimetry pr... | using polarimetry to retrieve the cloud coverage of earth-like exoplanets |
of the various techniques for discovering exoplanets, direct imaging is one of the most challenging, yet most rewarding. it allows us to not only visibly see a planetary companion, but to determine its orbit and atmospheric composition. the wide field infrared survey telescope (wfirst) will launch in 2025, with a coron... | wfirst cgi precursor imaging |
interactions between exoplanets and their host stars are the dominant factors in determining the composition, chemical state, and stability of planetary atmospheres. in this talk, i will discuss the various forms that these star-planet interactions (spi) can take, and in particular how these processes are traced with u... | ultraviolet observations of star-planet interactions - current status and future directions |
young brown dwarfs act as powerful analogs to the directly-imaged exoplanets, with similar temperatures, masses, ages and compositions. photometric variability monitoring of brown dwarfs is a unique probe of their atmospheres as it is sensitive to condensate clouds as they rotate in and out of view. variability has now... | let the great world spin: revealing the turbulent, stormy atmospheres of giant planet analogs |
one of the main goals of current exoplanet research is in studying the atmospheric composition and dynamics of exoplanet atmospheres. recent success has been made in identifying the spectral features of carbon monoxide and titanium oxide in the atmospheres of highly irradiated planets as well as identification of broad... | detecting analogues of the l-t transition in eccentric warm jupiters. |
as we increase our capacity to resolve the atmospheric composition of exoplanets, we must continue to refine our ability to distinguish true biosignatures from false positives in order to ultimately distinguish a life-bearing from a lifeless planet. of the possible true and false biosignatures, methane (ch4) and carbon... | developing tighter constraints on exoplanet biosignatures by modeling atmospheric haze |
young gas giant planets still glow hot from formation, sometimes even showing signs of active accretion. studying the atmospheres of these directly imaged planets may help placing constraints on how they formed, which may also shed light on the formation process of the planetary systems they reside in. in general, this... | retrieving the atmospheric properties of directly imaged planets |
observations of close-in rocky exoplanets (55 cnc e, k2-141b) with jwst are imminent. previous studies suggest that these planets hold permanent dayside magma oceans due to the strong solar flux. meanwhile, past observations found unexplained time-variation and a weak day-night gradient on 55 cnc e. close-in, rocky exo... | gone with the rock wind: a boundary layer model of close-in, rocky exoplanets with condensable-rich atmospheres |
analyses of exoplanet spectra from jwst have already revealed tantalizing insights into the atmospheres of these new worlds. previous exoplanetary observations have established their atmospheric diversity, not just in temperature, but also composition. it is therefore expected that the number of molecular signatures th... | hitran and hitemp data in the era of jwst |
over the past 25 years, weve found thousands of worlds beyond our solar system. nonetheless, some categories of exoplanets remain elusive for instance, planets that orbit their hosts on long, slow paths. a new study shows how we might hunt these worlds down.observational limitsartists impression of a hot jupiter transi... | identifying a slow planet from a single tess transit |
ultra-short period (usp) planets, with radii < 2 rearth and periods < 1 day, are a rare but very valuable planet class that can provide a glimpse at the surface compositions of worlds outside our solar system. most usp planets appear ~uniform in their bulk densities, consistent with earth-like compositions, and h... | phase curve observations of toi-561 b to study atmosphere-interior exchange |
the internal constitution of rocky exoplanets can be inferred only indirectly via their atmospheric composition. to address this issue with confidence requires the coupling of interior and atmospheric models to each other. in the past, various atmospheric redistribution models were developed to determine the compositio... | the formation of secondary exoplanet atmospheres via volcanic degassing in the c-h-o-n-s system |
rocky planets in exoplanetary systems have equilibrium temperatures up to a few 1000 k. the thermal evolution after a giant impact is sensitive to the equilibrium temperature. post-impact rocky bodies are thermally stratified, with cooler, lower-entropy silicate overlain by vaporized, higher-entropy silicate. the radii... | raining a magma ocean: thermodynamics of rocky planets after a giant impact |
the nature of the coolest brown dwarfs - their formation, their atmospheres, including their composition, temperature, pressure structures, and the nature of any clouds that may be present is of particular interest for a number of reasons. since they form where the initial mass function is rolling off they provide impo... | nircam y-dwarfs |
the atmospheric characterization of resolved brown dwarf companions are unique observational treasures as they help tell a story of giant planet formation and evolution far from a given star (>>10 au). brown dwarfs have better quality data than exoplanets and are ideal objects to test and verify models and atmosp... | a data driven approach to unlocking planet formation: the atmospheric retrieval of the bd +60 1417 system |
the successful launch of jwst ushers in a new era of astrophysics in which we will measure the compositions of exoplanet atmospheres with exquisite precision. the jwst transiting exoplanet early release science program was designed to test jwst's instrument capabilities for transit spectroscopy and provide lessons lear... | jwst transiting exoplanet early release science: a transmission spectrum of wasp-39b with nirspec g395h |
recent surveys have revealed an extraordinary and unexplained diversity of low-mass exoplanets. the main frontier for constraining the nature and origins of these planets is atmospheric characterization to reveal their detailed physical properties. previous spectroscopic observations of small exoplanets have been focus... | emission spectroscopy of the super-earth 55 cnc e |
because the composition of stellar atmospheres preserves the composition of the nebulae in which the stars formed, stellar abundances offer a unique glimpse into the epoch of planet formation and evolution of planetary systems. comparing the demographics of planet-hosting stars with field stars has shown strong correla... | detailed stellar chemistry and its role in planet occurrence |
the recent jwst early release science (ers) exoplanet program using the nirspec prism and g395h modes discovered an unexpected feature at 4.05 um in the transit spectrum of wasp-39b thought to be caused by so2. photochemical modelling of the atmosphere has shown so2 to be a robust outcome of the chemical environment in... | miri lrs follow up on so2 detection in wasp-39b |
the successful kepler and tess missions have discovered thousands of exoplanets and let the community focus on the characterisation of these bodies. one area of research utilises ultra-high-precision photometric and spectroscopic follow-up observations in order to accurately constrain the bulk densities of terrestrial ... | characterising the internal structures of small exoplanets with cheops |
we try to reconcile contrasting results about the composition of exoplanet atmospheres investigated with high-resolution and low-resolution spectroscopy. | the hr-lr duality of exoplanet atmospheres |
stellar granulation generates fluctuations in both photometric and spectroscopic data with properties that depend on the type of the star, its composition, and its evolutionary state. characterizing precisely these properties is key for the understanding of stellar atmospheres, but also for exoplanet detection where th... | contemporaneous photometric and spectroscopic stellar granulation signals seen by cheops and espresso |
exoplanets are discovered during occultation events. spectral lines characteristic of stellar emissions are modified and shaped by traversing exoplanetary atmosphere. several models for radiation transport are presented and compared with observational data. the relative contributions of scattering, absorption and colli... | spectral line shaping by exoplanetary atmosphere |
we report preliminary measurements from two separate laboratory studies: (a) collision-induced absorption (cia) of nitrogen in the far-infrared at temperatures between 78 and 130 k; and (b) temperature dependence of h2-broadening of ch4 in the near infrared at temperatures between 100 and 370 k.(a) nitrogen collision-i... | progress in the measurement of temperature-dependent n2-n2 collision-induced absorption and h2-broadening of cold and hot ch4 |
our goal is to understand the atmospheric condition of self-luminous, fairly young companions below the deuterium burning mass limit.can metallicity or isotopic composition be determined and do those give clues about the formation mechanism of these exoplanets?this jwst gto observing program concentrates on the 3.0 - 5... | jwst nircam gto program: ifu spectroscopy of spatially resolved exoplanets with nirspec |
photochemical hazes are common in exoplanetary systems, serving as important reservoirs for atmospheric molecules while influencing our ability to measure the local physical conditions in a planet's atmosphere. characterization and modeling of aerosol and hazes have taken on added importance as jwst examines exoplanet ... | the m dwarf fuv continuum: a missing driver of atmospheric hazes in exoplanet atmospheres |
brown dwarfs have cool atmospheres with the temperatures of giant planets. their atmospheres are cool enough to form clouds and their temperature determines which species condense. thick layers of dust, likely made of silicates, blanket l dwarf atmospheres, limiting the depths probed by spectra; these clouds clear dram... | empirically determining substellar cloud compositions in the era of jwst |
protoplanetary disks are circumstellar disks of matter, including gas and dust, from which planets eventually form. the disk midplane is the coldest region of the disk, which is caused from the stellar radiation not being able to get through it. within the disk midplane, there is a "great deal" of chemistry involved, p... | the role c/o ratio plays in the abundances of specific molecules in a disk midplane |
liquid water is generally assumed to be the most important factor for the emergence of life, and so a major goal in exoplanet science is the search for planets with water oceans. on terrestrial planets, the silicate mantle is a large source of water, which can be outgassed into the atmosphere via volcanism. outgassing ... | water oceans on high-density exoplanets from coupled interior-atmosphere modeling |
a new optical constant facility has been developed at nasa ames that will allow the determination of optical constants in the infrared of various materials, analogs of (exo)planetary hazes and cloud particles. our facility is composed of a fourier transform infrared (ftir) spectrometer continuously covering the near-ir... | introducing nasa ames' new infrared optical constant facility. determinations of complex refractive indices for titan aerosol analogs and other applications. |
the pandora smallsat is planned for launch in 2025 and is designed to disentangle star and planet signals in transmission spectra to reliably determine exoplanet atmosphere compositions. | pandora: multiwavelength characterization of exoplanets and their host stars |
in this talk, i will discuss the current state of the mascara and bring networks, and go into detail on how our observations can be combined with tess to search for long period transiting exoplanets. these networks have discovered four exciting transiting exoplanets which are ideal for follow up atmospheric characteriz... | mascara and bring, finding bright transiting planets and synergies with tess |
future exoplanet direct imaging missions, such as habex and luvoir, will select target stars to maximize the number of earth-like exoplanets that can have their atmospheric compositions characterized. because one of these missions' aims is to detect biosignatures, they should also consider the long-term habitability of... | relative biosignature yields: assessing the habitable histories of stellar systems |
with atmospheric temperatures ranging from roughly 3,000 to 6,500 degrees fahrenheit, ultra-hot jupiters are ready-made laboratories for extreme planetary science. for instance, any molecules in the atmosphere of an ultra-hot jupiter will be broken down into their component atoms and ions. so what can be found in the a... | there's metal in the air |
as the ultra-hot jupiter kelt-9b blazes across the face of its host star, we have an excellent opportunity to examine its scalding atmosphere. a new study now reports on what weve found.a passing glancein our efforts to learn more about worlds beyond our solar system, atmospheres provide a critical key. characterizing ... | peering into the atmosphere of the hottest planet known |
rocky (exo)planets can be classified based on their mantle viscous state. the mantle viscosity influences the efficiency of convection and heat loss of the planet, altering the outgassing rate. low viscous planets are hypothesized to have strong volcanic activity reshaping the surface and changing the atmosphere. this ... | rocky worlds: what do a planet's orbital parameters tell us about its mantle state? |
warm jupiters (jupiter-sized planets with equilibrium temperatures of ~1000 k) are uniquely favorable for atmospheric characterization since (1) they have strong spectroscopic features and (2) their compositions are highly sensitive to temperature variations and subjected to disequilibrium processes. we propose to obse... | warm jupiters dis-equilibrium and thermo-chemistry in transmission spectroscopy |
the composition and structure of the upper atmosphere of extrasolar giant planets (egps) are affected by the high-energy spectrum of the host star from soft x-rays to extreme ultraviolet (euv) (0.1-10 nm). this emission depends on the activity level of the star, which is primarily determined by its age [1]. in this stu... | modelling the ionosphere of gas-giant exoplanets irradiated by low-mass stars |
where, when and how do (gas giant) planets form? - up to now the formation process of planets was mostly a subject of theroretical studies and computer simulations. empirical data were only used to constrain the initial conditions (e.g., the physical and chemical conditions in circumstellar disks) or the outcome of the... | young planets embedded in circumstellar disks |
the atmospheric characterization of resolved brown dwarf companions are unique observational treasures as they help tell a story of substellar mass (including giant planet) formation and evolution far from a given star (≫10 au). brown dwarfs have better quality data than exoplanets and are ideal objects to test and ver... | retrieval of the bd+60 1417 b system: a nearby planetary-mass companion |
the bulk density of a planet is a result of its structure and composition. relative proportions of iron core, rocky mantle, and gaseous envelopes, however, are degenerate for a given density. this degeneracy is reduced for rocky planets without significant gaseous envelopes when the structure is assumed to be a differe... | the rock-star relationship: assessing the probability that a rocky planet's composition reflects its host star |
it could be useful to collect the only known living planet's and other well-known planet's light curves and spectra for the future comparison and habitability modeling. for this, we need to seek possibilities to measure earth's and other terrestrial planet's transits, occultations, and reflections from different locati... | transits in the solar system and the composition of the exoplanet atmospheres |
the fuv transit technique specific to hst is unique at characterizing the upper atmospheres of exoplanets. indeed, the uppermost layers of a planet orbiting close to an euv-bright star undergo great heating, inflation and mass escape. fuv transit observations of the warm-neptune gj 436b have revealed an immense h i clo... | connecting the lower and upper atmospheres of a warm-neptune. implications for planetary evolution. |
because of their common origin, it is expected (or assumed) that the composition of planet building blocks should (to a first order) correlate with stellar atmospheric composition, especially for refractory elements. in fact, information on the relative abundance of refractory and major rock-forming elements such as fe... | observational evidence of the compositional link between rocky planets and their hosts |
the field of exoplanet science has matured over the past two decades with over 3500 confirmed exoplanets. however, many fundamental questions regarding the composition, and formation mechanism remain unanswered. atmospheres are a window into the properties of a planet, and spectroscopic studies can help resolve many of... | exoplanet meteorology: characterizing the atmospheres of directly imaged sub-stellar objects |
my team has been searching for another planet to replace earth once humans have completely depleted its finite resources, however, a suitable planet with the necessary resources that can be easily terraformed has yet to be discovered. the purpose of this research was to find a planet and find out the best way to make i... | using earth analogue from 2.5 billion years ago to research exo-planet |
when studying planetary atmospheres, scattering signatures, such as rayleigh scattering, can often be the most easily characterized signal. this is especially true in terrestrial atmospheres, where rayleigh scattering is the dominant spectral feature in optical wavelengths. these scattering signatures, unlike molecular... | blue skies through a blue sky: an attempt to detect rayleigh scattering in an exoplanet atmosphere from a ground-based telescope |
observations of exoplanets during transit and eclipse have revealed the atmospheric compositions and thermal properties of some of these objects. in this context, ground-based facilities provide the opportunity to study close in transiting exoplanets through spectral characterization studies. we show visible-light and ... | probing transiting exoplanet atmospheres with multi-object spectrophotometry |
studies of directly imaged planets extend exoplanet surveys to greater separations from the stars, test giant planet formation models, probe the composition of the progenitor disks and can reveal circumplanetary disks, but these objects are rare. we report a faint, co-moving companion to an m dwarf member of the taurus... | photometry of a young planetary-mass companion to a taurus m dwarf star |
*embargoed* we present the follow-up analysis (crouse et al. in prep) of the discovery of the fourth closest known terrestrial exoplanet in the habitable zone by kossakowski et al. (2022) using radial velocity measurements. we use two general circulation models (gcms) to simulate various atmosphere and surface scenario... | climate analysis on a newly discovered non-transiting nearby terrestrial exoplanet |
thanks to the advances in modern instrumentation we learned about many exoplanets that spawn a wide range of masses and composition. studying their atmospheres provides insight into planetary diversity, origin, evolution, dynamics, and habitability. present and future observing facilities will address these important t... | studying physics and chemistry in atmospheres of hot jupiters from future ground-based and space facilities |
a main goal of the atmospheric characterization of exoplanets is to unveil planet formation and evolution processes. many previous studies investigated the possibility of constraining planetary formation locations from atmospheric carbon-to-oxygen (c/o) ratios. recent studies also suggested that atmospheric nitrogen pr... | can we use atmospheric nitrogen as a tracer of giant planet formation? complexities in diagnosing bulk nitrogen abundance from ammonia observations |
exoplanet characterization is one of the main foci of current exoplanetary science. for super-earths and sub-neptunes, we mostly rely on mass and radius measurements, which allow to derive the body"s mean density and give a rough estimate of the planet"s bulk composition. however, the determination of planetary interio... | the impact of exoplanets' measured parameters on the inferred internal structure. |
the destruction of molecules by photodissociation influences the composition and dynamics of exoplanets, particularly in the presence of a uv-rich stellar environments, where molecules are hot. current photodissociation calculations generally assume $t= 0$ k, appropriate for the cold interstellar medium but inadequate ... | exomolhd: photodissociation of diatomic molecules |
the abstract uses the solar system analogy to try and answer the following questions important for exoplanetary systems: what role do small bodies play in the formation of planetary systems? how do the planets or protoplanetary disks evolve subsequent to impacts? what composition markers in the atmospheres of planets c... | understanding the volatile history in the planetary building blocks |
the successful kepler and tess missions have discovered thousands of exoplanets and let the community focus on the characterisation of these bodies. one area of research utilises ultra-high-precision photometric and spectroscopic follow-up observations in order to accurately constrain the bulk densities of terrestrial ... | characterising the internal structures of exoplanets with cheops |
the search for life on exoplanets must be done in the context of a rigorous understanding of "false positives" for life. these false positives are non-biological processes with the potential to produce the signals that would otherwise be interpreted as biosignatures. here, we present studies of two such "false positive... | biosphere false positives from thin air: abiotic mechanisms for o2 and o3 generation in planetary stratospheres |
iarps (giano & harps) is an observing mode that allows having on the same focal station of the telescopio nazionale galileo (tng) both the high-resolution spectrographs, harps-n (visible, vis) and giano-b (near-infrared, nir), working simultaneously. to date, giarps is the first and unique worldwide instrument prov... | the first four years of giarps@tng observations |
jupiter exhibits dynamical as well as chemical trends in its atmosphere that have been observed by ground-based observatories and spacecraft alike. these observations are limited to the upper layers of the atmosphere and are therefore subject to the atmospheric processes that dominate the cloud layers. observations of ... | moist convection induced local enhancement of carbon monoxide – implications for the deep water abundance |
since the discovery of the first transiting exoplanet in 1999, shortly after the initial discovery by the radial velocity method, over 3189 such systems have been discovered. as a result in recent years the field has started to transition from a discovery phase to one of characterisation and understanding more about th... | citizen scientist participation in transiting exoplanet science |
the benchmark hot jupiters hd209458b and hd189733b have provided the foundations of comparative planetology for giant exoplanets, making them of paramount importance for atmospheric studies of short-period planets. hd189733b is the closest transiting hot jupiter to earth and transit observations have been obtained and ... | nuv transit spectroscopy of hd189733b: measuring the mass-loss and ionization state of a prototypical escaping atmosphere |
a pseudo 3d exoplanet climate model is presented in which the ocean and atmosphere are simulated via stacked 2d meshes with a one dimensional vertical coupling. both the ocean and atmosphere are simulated using a hydrodynamic solution in spherical polar coordinates, vertically coupled to climate models for water evapor... | simulating climate on slowly rotating exoplanets |
the next generation of space and ground-based telescopes (jwst, ariel, elts) should give us improved transmission/emission spectra for a large diversity of exoplanets, allowing to probe their atmospheric composition. for a better understanding of this data, atmospheric models taking into account photochemistry are requ... | photochemistry of planetary atmospheres with 3d global climate model |
the large diversity of planetary worlds has been firmly established, since the discovery of the first exoplanet in 1995. some planets have the size of jupiter and orbit at very close distances from their host star, making them "hot jupiter" with atmospheric temperatures as high as 2000 k. to understand how such diversi... | high temperature vuv cross section measurements of acetylene for hot exoplanets study |
for terrestrial exoplanets with thin atmospheres or no atmospheres, the surface will dominate to the reflected light signal of the planet. direct observation of the disk-integrated brightness of bodies in the solar system, and the variation with illumination angle, wavelength, and planetary longitude, is essential for ... | the galilean satellites observed by cassini: a testbed for icy terrestrial exoplanets |
future missions to directly image exoplanets aim to measure the spectra of earth-like planets in the habitable zones of their stars to infer their atmospheric compositions and search for biosignatures. in addition to selecting target stars to maximize the number of earth-like planets that will be discovered and charact... | long-term habitability and the emergence of biosignatures |
discovering and characterizing gas giants is important to the search for other life, as gas giants greatly affect the habitability of a solar system. transits of exoplanets observed in visual photometric bands have been used to characterize their atmospheres and confirm planet parameters. we observed two primary transi... | characterizing giant exoplanets through multiwavelength transit observations: hat-p-8b |
knowledge of both the mass and radius of an exoplanet allows us to estimate its mean density, and therefore, its composition. exoplanets seem to fill a very large parameter space in terms of mass and composition, and unlike the solar-system's planets, exoplanets have intermediate masses (~ 5-50 m⊙) with various densiti... | on the mass-radius relation of methane planets |
m stars are very abundant in our galaxy, and very likely harbour the majority of planetary systems. but a particularity of m stars is that they are the most active class of stars. indeed, they experience stellar variability such as flares. these violent and unpredictable outbursts originate from the photosphere and are... | effect of flares on the chemical composition of exoplanets atmospheres |
exoplanet atmospheres can be characterized with transmission spectroscopy, a method that reveals the atmospheric shape and composition, among other qualities. ultraviolet (uv) transmission spectroscopy probes the presence and relative abundance of atoms and ions in the upper atmospheric layers and the shape of the uv t... | the colorado ultraviolet transit experiment (cute): 1-year in-flight update and first science results |
the formation of clouds significantly alters the spectra of cool substellar atmospheres from terrestrial planets to brown dwarfs. in cool planets like earth and jupiter, volatile species like water and ammonia condense to form ice clouds. in hot planets and brown dwarfs, iron and silicates instead condense, forming dus... | clouds and hazes in exoplanets and brown dwarfs |
ultra-short period planets (usp) that are rocky in nature are plentiful in the exoplanet catalogue and may host tectonic regimes without analogues in the solar system. recently, the transit phase-curve of the super-earth lhs 3844b (radius = 1.303 earth radii) has been mapped by a 100 h spitzer observing campaign and is... | interior dynamics of tidally locked super-earths: the case of lhs 3844b |
this work aims to determine the mass-radius rela-tionships of highly irradiated (500< tirr<2000k)small planets (0.2<m<2.3m⊕) with water con-tents up to 5%. to do so, we coupled an internalmodel of small terrestrial planets (brugger et al.,2017) to the atmosphere model elaborated by marcqet al. (2017, 2019),... | mass-radius relationships of small, highly irradiated exoplanets with small water mass fractions |
jupiter-like exoplanets – planets with masses, semi-major axes, and ages similar to those of jupiter – will be directly imaged in reflected light for the first time by the coronagraph instrument (cgi) on board nasa's upcoming nancy grace roman space telescope. cgi will image these exoplanets (previously detected by rad... | jupiter as an exoplanet-analog: how do atmospheric color changes affect unresolved photometry? |
observations of super-earth atmospheres have revealed information regarding the surface conditions of these exoplanets. more advanced instruments will allow future missions to observe atmospheres of exoplanets down to earth size. atmospheres of terrestrial planets form under interaction with their rocky interiors, by d... | the controls of planetary bulk composition and tectonic style on the long-term evolution of outgassed atmospheres |
we investigate the past evolution of the climate of earth and earth-like planets as a coupled interior/atmosphere system. we compare climatic states obtained through parameterized modelling versus a physics-based 3d general circulation model (gcm). finally, we identify characteristics in the 3d simulations that most af... | the climate of earth and earth-like (exo)planets in coupled evolution models: insights from 3d gcm. |
the importance of water in our everyday life as well as in biochemical processes on earth is undeniable. water is also one of the main molecular species in different astrophysical environments, such as prestellar cores, protostellar envelopes, planet-forming disks, and planetary atmospheres, and it is evidently require... | solid-state water inside the snowline in planet-forming disks: exploring the origin of water on terrestrial planets |
detection of superflares on active g to m dwarf stars opened a new avenue in understanding the properties of eruptive events and their impact on exoplanetary environments. energetic solar flares are usually associated with fast coronal mass ejections (cmes) that produce extended shocks, the sites of efficient particle ... | stellar cme driven energetic particles events from young active stars |
in this talk, i present the discovery and characterization of two transiting planets around the bright m1 v star toi-776 (j=8.5 mag), detected during sector 10 observations of the transiting exoplanet survey satellite (tess). combining them with harps radial velocities, as well as ground-based follow-up transit observa... | toi-776: a multi-planetary system around a bright m dwarf optimal for jwst |
twinkle is a small, dedicated satellite that has been conceived to measure the atmospheric composition of exoplanets. this cost-effective spacecraft is being constructed on a short timescale in the uk and is planned for launch in early 2022. the satellite uses a high-heritage satellite platform and instrumentation buil... | twinkle - a low-earth orbit visible and infrared exoplanet spectroscopy observatory |
the current context of space exploration missions is extremely favourable, especially regarding rocky planets. several orbiters and rovers currently investigate the surface and atmosphere of mars; more are planned in the future. three medium-class missions have been approved by nasa and esa to study venus in the coming... | heterogeneous reactivity in the atmosphere of rocky planets |
hot exoplnets are heated by intense radiation of the host star result in intensive thermal escape and mass loss of their hydrogen-dominated upper atmospheres. spectral absorptions of hot exoplanets passing through stellar disk plays in atmospheres investigations the role of rosetta stone, providing information on these... | interpretation of mysterious non-detection he, c and o components in the atmosphere of gj-436b |
far ultraviolet (fuv; 912-1700 å) spectroscopic observations of f, g, k, and m dwarf stars allow for the study of several chromospheric and transition region emission features. h i lyman-alpha (lyα, 1216 å) emission dominates the fuv spectrum, and is a critical driver of photochemistry in the atmospheres of exoplanets.... | far ultraviolet radiation environments of fgkm stars |
nitrogen is an essential building block of dna, rna, and proteins and, subsequently, it must have been bioavailable since the origin of life. on modern earth, biological sources are mostly responsible for making nitrogen bioavailable via n2 fixation with only a few percent coming from abiotic sources. on early earth, b... | nitrogen fixation by lightning and its role for early life on earth and exoplanets |
the atmospheres of exoplanets are being characterised in increasing detail by observational facilities and will be examined with even greater clarity with upcoming space based missions such as the james webb space telescope (jwst) and the wide field infrared survey telescope (wfirst). a major component of exoplanet atm... | glass rain: modelling the formation, dynamics and radiative-transport of cloud particles in hot jupiter exoplanet atmospheres |
planetary formation models predict that giant planets should not form around stars with masses less than 0.5 m_sun. this is due to two fundamental factors: (1) slow accretion due to long orbital timescales, and (2) low protoplanetary disk masses, limiting the available planetary building material. nature has proven thi... | problem planets: understanding the formation of giant planets around low mass stars |
for an assessment of the detectability of molecular concentrations from transit spectra of earth-like exoplanets, occultation spectra observed by an operational earth observation satellite mission have been modeled with a line-by-line infrared radiative transfer code. retrieval of atmospheric composition utilizing a no... | atmospheric composition retrieval from transit spectra of terrestrial exoplanets: a feasibility study using earth observations |
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