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a debate has arisen in the magnetospheres community in recent years about whether planetary magnetic fields actually inhibit atmospheric loss from planets. on one hand, atmospheric escape rates are driven in part by the strength of the stellar wind, and unmagnetized venus and mars both have atmospheric isotope ratios t... | progress on understanding the influence of planetary magnetic fields on atmospheric escape rates |
the origin of the radius distribution gap for short-period kepler planets has become a priority investigation in exoplanet science. the current leading explanation is the photoevaporation of h/he envelopes during the first 100 million years of a planet's lifetime, where the gap is created when planets below some initia... | planetary mass loss and the high-energy spectrum of v1298 tau |
a debate has arisen in the magnetospheres community in recent years about whether planetary magnetic fields actually inhibit atmospheric loss from planets. on one hand, atmospheric escape rates are driven in part by the strength of the stellar wind, and unmagnetized venus and mars both have atmospheric isotope ratios t... | progress on understanding the influence of planetary magnetic fields on atmospheric escape rates |
the hd 97658b super-earth was recently detected in transit across one of the brightest star (v=7.7) known to host a transiting planet. the density of the planet suggests it must contain a large mass fraction of water. although the water vapor has not been detected in the lower atmosphere by hst/wfc3 due to the small at... | search for an evaporating ocean on the super-earth hd 97658b |
the helium (he) 1083 nm line offers insight into the atmospheric mass loss of close-in exoplanets, which is likely to be significant in sculpting their population. most studies of atmospheric escape have been done at uv wavelengths using the hydrogen lyman-alpha line, but in the last few years the metastable he 1083 nm... | metastable helium reveals ongoing mass loss for the gas giant hat-p-18b |
in the past months we have obtained evidence that an unusual phenomenon is happening in the atmosphere of one of the hot jupiters with shortest period. high-resolution spectroscopy from the ground reveals a transit spectrum where the sodium absorption signal from the planet peaks at 2-3%, which is larger than the plane... | is the atmosphere of the extremely irradiated exoplanet wasp-43b in a blow-off state? |
exoplanets in short-period orbits provide a unique opportunity to observe phenomena critical to the development and evolution of our own solar system, including atmospheric escape, interaction with the host star, and the potential to study exoplanetary magnetism. at present, the theories explaining upper atmosphere obs... | cute: the colorado ultraviolet transit experiment |
progress on addressing two important exoplanet science topics can be made in the near-uv, where transit spectroscopy can measure aerosol scattering from the lower atmosphere, while large atmospheric escape signatures can be detectable in narrow-bands centred around strong mg and fe lines. wfc3/uvis has never been used ... | how small and how high? enabling uv exoplanet cloud and exosphere science with wfc3/uvis |
studying the magnetic fields of exoplanets will allow for the investigation of their formation history, evolution, interior structure, rotation period, atmospheric dynamics, moons, and potential habitability. we previously observed the transits of 16 exoplanets as they crossed the face of their host-star in the near-uv... | the robustness of using near-uv observations to detect and study exoplanet magnetic fields |
the 2006 guinsaugon landslide in st. bernard, southern leyte is one of the largest known landslides in the philippines in recent history. it consists of a 15-20 million m3 rockslide-debris avalanche from an approximately 675 m high mountain weakened by continuous movement of the philippine fault. the catastrophic guins... | structurally controlled hazard mapping of southern leyte, philippines |
in this work, we present preliminary results of the simulation of the atmospheric escape in a hot-jupiter like exoplanet using the radiative- hydrodynamic code 3d guacho. our model is able to reproduce, in a self-consistent way, the formation of a planetary wind generated by the absortion of extreme ultraviolet (euv) p... | simulación numérica 3d del escape atmosférico de un hot-júpiter |
the hydrogen exosphere constitutes the uppermost atmospheric layer of the earth, and its shape may reflect the last stage of the atmospheric escape process. the distribution of hydrogen in the outer exosphere remains unobserved because outer geocoronal emissions are difficult to observe from within the exosphere. in th... | hydrogen lyman alpha imaging camera onboard procyon |
in the present chapter we present the results of evolutionary studies of exoplanetary atmospheres. we mostly focus on the sub- to super-earth domain, although these methods are applicable to all types of exoplanets. we consider both thermal and nonthermal loss processes. the type of thermal loss mechanism depends on so... | stellar driven evolution of hydrogen-dominated atmospheres from earth-like to super-earth-type exoplanets |
how many rocky planets in the galaxy have an atmosphere? the answer to this question is urgent: models suggest that many exoplanets suffer prolonged atmospheric escape, implying that most rocky planets could actually have little chance of sustaining a surface biosphere. the james webb space telescope (jwst) might be ab... | how to quickly search rocky exoplanets for signs of atmospheres |
super-earth characterization continues to be a particular focus of the field given that it is the interface between terrestrial planets and gas-dominated planets. the implications of this division reverberate in planet formation, planetary interiors, and the origins and evolution of planetary atmospheres. a recently di... | atmospheric evolution and loss of a recently discovered low-density ultra-short period super-earth |
as we are on the verge of receiving high quality spectra of many exoplanetary atmospheres, the next major challenge is discerning the underlying atmospheric characteristics, such as the surface pressure and temperature profile. forward modeling of rocky exoplanet atmospheres shows that many different states can produce... | plasma-neutral interactions as a method of constraining stable rocky exoplanet atmospheres |
luvoir is a powerful and flexible observatory designed to revolutionize our view of the universe. in addition to searching for signs of life on habitable worlds, luvoir will be capable of detecting and characterizing hundreds of non-habitable exoplanets orbiting nearby stars dramatically advancing the field of "compara... | diversity of exoplanets with luvoir ii: the uv |
with the continually increasing number of newly discovered exoplanets, the quest to characterize the high energy radiation environment of each individual system becomes a larger and more arduous task. stellar euv flux contributes to atmospheric escape and water loss on close-in planets, therefore having a reliable cata... | pegasus: phoenix euv grid and stellar uv spectra |
atmospheric escape has traditionally been observed using hydrogen lyman-α transits, but more recent detections utilise the metastable helium triplet lines at 1083nm. capable of being observed from the ground, this helium signature offers new possibilities for studying atmospheric escape. such detections are dependent h... | the evolution of atmospheric escape of highly irradiated gassy exoplanets |
stellar extreme ultraviolet (euv, 100-1000 å) radiation can influence factors for habitability of planets in k dwarf systems, including driving atmospheric escape and water loss from close-in exoplanets. this wavelength range is currently unobservable due to interstellar contamination and a lack of operational instrume... | the great escape! extreme-uv spectra grids for k-type stars |
although exomoons, natural satellites beyond our solar system, are still undetectable in direct searches with state-of-the-art instruments, their existence has been hypothesized to explain various inconsistencies in exoplanetary spectra. exogenic sources of sodium and potassium have been considered at multiple exoplane... | exo-io simulations of toroidal exospheres |
ariel [1] is the m4 mission of the esa's cosmic vision program 2015-2025, whose aim is to characterize by lowresolution transit spectroscopy the atmospheres of over one thousand warm and hot exoplanets orbiting nearby stars. the operational orbit of the spacecraft is baselined as a large amplitude halo orbit around the... | preliminary surface charging analysis of ariel payload dielectrics in early transfer orbit and l2-relevant space environment |
intense, high-energy stellar irradiation is believed to control the atmospheric chemistry and mass loss of short-period planets. these effects are most dramatic in the early stages of planetary evolution, when young stars produce higher levels of x-ray and ultraviolet (uv) radiation, and experience extreme stellar acti... | a multi-wavelength investigation of young stellar and planetary systems |
the k2-33 b is a planet of 5 earth radii orbiting the young m-type host star, recently emerged from the interplanetary disc. the extreme youth of the system (<20 myr) gives the unprecedented opportunity to study the earliest phases of planetary evolution, at a stage when the planet is exposed to an extremely high le... | young planets under extreme uv irradiation: upper atmosphere modelling of the young exoplanet k2-33b |
high-energy stellar irradiation can photoevaporate planetary atmospheres, which can be observed in spectroscopic transits of hydrogen lines. for the close-in giant exoplanet hd189733b, multiple observations in the ly-alpha line have shown that atmospheric evaporation is variable, going from undetected to enhanced evapo... | the impact of cmes and flares on the atmospherere of close-in exoplanets: comparison with observations |
atmospheric escape from exoplanets is a topic of great interest for the exoplanet community since atmospheric retention is an important component of surface habitability. while atmospheric escape has been detected from large exoplanets, it remains difficult to measure for smaller (rocky) planets. indeed, for rocky plan... | atmospheric lifetime from a hypothetical mars-sized planet orbiting barnard's star |
we have studied the input of the exothermic photochemistry into the formation of the non-thermal escape flux in the transition h 2 − h region of the extended upper atmosphere of the hot exoplanet - the sub-neptune π men c. the formation rate and the energy spectrum of hydrogen atoms formed with an excess of kinetic ene... | study of the non-thermal atmospheric loss for exoplanet π men c |
with jwst up and running, astronomers are getting a first look at the quirks of individual exoplanets. features never before examined are coming into view: for instance, a recent study has revealed that while hat-p-18b may not have much methane, it does have a tiny tail.jwst shows off, finds a corginow more than a year... | the corgi of exoplanets: methane mystery on hat-p-18b |
the terrestrial planets of the solar system are rocky worlds that did not accrete envelopes of hydrogen and helium, but instead possess thin secondary atmospheres, or no atmosphere at all. until recently, most exoplanet atmospheric studies have centered around hot jupiters, for which high planet-to-star radius ratios a... | exploring an earth-sized neighbor: ground-based transmission spectroscopy of gj1132b, a rocky planet transiting a small nearby m-dwarf |
we present the colorado ultraviolet transit experiment (cute), a 6u cubesat mission that will perform exoplanet transmission spectroscopy to study the physics of atmospheric escape and possibly detect the presence of magnetic fields on exoplanets. | cute: a small nuv satellite mission to study exoplanet atmospheres |
atmospheres of the early earth with the young sun or close-in exoplanets around k and m dwarfs are subject to large fluxes of solar/stellar radiation from the hosts stars. the solar/stellar radiative flux in the x-ray and extreme ultraviolet ray (xuv) are the key elements for heating the upper atmosphere such as the io... | xuv and joule heating driven atmospheric escape from the early earth and earth-sized exoplanets around active stars |
the absence of global dipole magnetic fields at terrestrial planets is widely perceived as a major impediment in protecting planetary atmospheres from being eroded by stellar winds. in this work, we re-examine this idea by focusing on the rate of atmospheric ion escape from mars for nominal solar wind parameters and an... | global dipole magnetic field: boon or bane for the martian atmospheric retention? |
luvoir is powerful and flexible observatory designed to revolutionize our view of the universe. in addition to searching for signs of life on habitable worlds, luvoir will be capable of detecting and characterizing hundreds of non-habitable exoplanets orbiting nearby stars dramatically advancing the field of "comparati... | studying the diversity of exoplanets with luvoir |
stellar flares are considered an impediment to habitability, especially in the case of close-in exoplanets around m-dwarfs since these stars are highly active. in recent times, there has been a growing awareness that coronal mass ejections (cmes) - sometimes termed as stellar storms or superstorms, depending on the fla... | how flares regulate atmospheric losses from the trappist-1 planets |
in this investigation, we present 3-d simulations of the upper thermosphere and ionosphere of the hot jupiter hd 209458 b (nicknamed osiris). we examine the 3-d neutral and ion dynamics under the influence of jovian-type magnetic fields and compare these with a non-magnetic case. our initial results suggest that the jo... | simulating the three-dimensional upper atmospheres of close-in exoplanets with strong magnetic fields |
i will address two questions: (1) do tess/kepler super-earths have atmospheres? (2) for sub-neptunes, how does magma-atmosphere exchange set the composition of the atmosphere? both involve coupling between magma oceans and h2-rich atmospheres. (1) after stellar xuv flux declines, super-earth volcanism continues for gyr... | the transition from primary to secondary atmospheres |
so far, atmospheric evaporation has been detected in exoplanets with direct and indirect methods. from these observations, it was found that close-in exoplanets show very high escape rates that are on the order of 1e9 -- 1e10 g/s and even higher. there is a number of reasons of why these rates are so high, including th... | an exoplanetary view on atmospheric evaporation |
the helium line triplet at 1083 nm has recently been established as a powerful new diagnostic of upper atmospheres of exoplanets. these observations opened a new wavelength window into the extended atmospheres of exoplanets, which can ultimately improve our understanding of the physical processes that drive atmospheric... | a new method for detecting magnetic fields in exoplanets |
mars has always represented an important target from the standpoint of planetary science, especially on account of its long-term climate evolution. one of the most striking differences between ancient and current mars is that the former had a thicker atmosphere compared to the present-day value, thereby making noachian... | modeling martian atmospheric losses over time: implications for (exo)planetary climate evolution and habitability |
transmission spectroscopy is one of our most powerful tools for characterizing exoplanet atmospheres and hanks to the recent launch of nasa's tess mission we will soon have a large sample of planets around bright stars, ideally suited to this technique. with it's unique combination of uv to nir wavelength coverage and ... | transmission spectroscopy of exoplanets with luvoir |
high euv irradiation near the parent star significantly heats and ionizes hydrogen-rich exoplanet upper atmospheres. the resulting weakly-bound gas, and frozen-in magnetic fields, can escape the planet in a gas pressure-driven outflow, aided by stellar tidal forces. this upper atmosphere of atomic hydrogen has been det... | exoplanetary mhd outflows driven by euv heating, lyman alpha radiation forces and stellar tides |
we study the atmospheric escape from m-dwarf exoplanets (including proxima b and seven earth-sized planets in the trappist-1 system) and its implications for long-term climate evolution and habitability by using the state-of-the-art numerical tools. | atmospheric escape from m-dwarf exoplanets and implications for long-term climate evolution and habitability |
we present a uniform analysis of the atmospheric escape rate of neptune-like planets with known radius and mass. we find that nearly 15% of neptunes exhibit extremely high mass-loss rates, that defy evolution and composition models of their atmospheres. we conclude that at least one of the established techniques to con... | mass-loss rate constraints on the observed distribution of exoplanets |
planetary oxidation is critical to the evolution of terrestrial-type atmospheres and consequently to astrobiology and the search for biosignatures. the atmospheres and surfaces of all rocky planets oxidize to some degree due to gravitational differentiation: hydrogen is lost to space and iron moves to the core, leaving... | planetary oxidation and abiotic o2 atmospheres |
the work presents the multi-fluid numerical modeling to interpret the observed absorption in mg resonance lines during the transit of wasp-12b and to quantify the crucial mechanisms responsible for the exoplanetary upper atmosphere mass loss. the model simulates the expansion of upper atmosphere due to stellar xuv radi... | multi-fluid modeling of upper atmosphere mass loss and absorption line for wasp-12b |
exoplanetary environments are made of an intricate mixture of plasmas, radiation, energetic particles, winds, and magnetic fields; these all play crucial roles for the structure and evolution of planetary atmospheres and the formation and possibly protection of planetary habitable environments. interactions between pla... | exoplanetary habitability: radiation, particles, plasmas, and magnetic fields |
we will present the results of magma ocean models incorporating ferrous iron disproportionation [1] in the silicate melt [2], combined with ferrous/ferric iron fractionation during crystallization of the magma ocean. the magma ocean model is coupled to a steam atmosphere model [3], which controls the rate of cooling. e... | combined redox evolution of magma oceans due to disproportionation, ferric iron partitioning, and atmospheric oxidation |
the uppermost layer of the atmosphere, the exosphere,is not well-known in its global structure since the densities are very low compared to instrument detection capabilities. because of rare collisions and high knudsen numbers, the motion of light species (h,h2, ...)in the corona is essentially determined by the extern... | influence of the radiation pressure on the planetary exospheres: density profiles, escape flux and atmospheric stability |
short-period sub-neptunes with substantial volatile envelopes are among the most common type of known exoplanets. however, these planets are typically on highly-irradiated orbits where they are vulnerable to atmospheric photoevaporation. in particular, recent studies of the kepler planet population have suggested a dea... | investigation of the sub-neptune photoevaporation desert for m-dwarfs to sun-like stars |
we aim at investigating the possible internal structures of the exoplanet gj 1132 b whose physical properties have been recently refined from multi-wavelength observations of a series of transits. because this planet potentially harbors an atmosphere, we also discuss the influence of hydrodynamic escape on its internal... | the atmosphere and internal structure of gj 1132 b |
ongoing and future space missions aim to identify potentially habitable planets in our solar system and beyond. planetary habitability is determined not only by a planet's current stellar insolation and atmospheric properties, but also by the evolutionary history of its climate. it has been suggested that icy planets a... | abrupt climate transition of icy worlds from snowball to moist or runaway greenhouse |
exoplanets orbiting at close distances from their stars could lose some fraction of their atmospheres because of the extreme stellar irradiation. hot rocky planets might have lost all of their atmospheres through this process, having evolved from larger progenitors with gas envelopes, possibly neptune-mass exoplanets. ... | full hst coverage of a comet-like exoplanet in transit |
young planetary systems offer the opportunity to study the early stages of planetary and atmospheric evolution. exoplanets in young stellar clusters, which have known ages, provide a valuable benchmark for models of these processes. k2-25b is a neptune-sized exoplanet recently found to transit a mid m dwarf member of t... | the evaporating exosphere of a young planet |
with stis/uv observations we detected magnesium atoms at high altitude in the atmosphere of the hot-jupiter hd209458b, probing lower regions in the atmosphere than previously done with lyman-alpha observations (vidal-madjar et al. 2013). with the present program, we will search for magnesium and other heavy species in ... | metals from deep atmosphere to exosphere in hot-jupiters |
observations of exoplanets during the transit of their host star allow probing the structure and composition of their atmosphere. the intense stellar energy input into exoplanets orbiting close to their star can lead to a dramatic expansion of their upper atmosphere, and the 'evaporation' of large amounts of gas into s... | the most extreme case of atmospheric escape detected on the warm neptune gj 3470b with hst |
we present new quasi-global 3-d radiative-hydrodynamic simulations of close-in exoplanets undergoing atmospheric escape. by tracking the ionization state of outflows driven by ionization heating, we produce self-consistent synthetic observations. the resulting synthetic lyman-α observations find several distinct large-... | atmospheric escape: new windows, longer baselines and demographic influences |
exoplanets in short-period orbits provide a unique opportunity to observe phenomena critical to the development and evolution of our own solar system, including atmospheric escape, interaction with the host star, and the potential to study exoplanetary magnetism. i will present the colorado ultraviolet transit experime... | the cute small satellite mission |
the most widely-studied mechanism of mass loss from irradiated exoplanets is photoevaporation via xuv ionization. however, lower-energy fuv dissociation of hydrogen molecules can also theoretically drive atmospheric evaporation on low-mass planets because the dissociation energy of hydrogen is an order of magnitude gre... | photodissociation-driven mass loss from young and highly-irradiated exoplanets |
one of the great strengths of the proposed luvoir space observatory is that in addition to searching for potentially habitable terrestrial planets, it will find and characterize hundreds of other types of planets as well. this large population of planets will offer unparalleled opportunities for comparative planetary s... | the capabilities of luvoir for studies of exoplanet diversity |
transmission spectroscopy is one of our most powerful tools for characterizing exoplanet atmospheres and thanks to the recent launch of nasa's tess mission we will soon have a large sample of planets around bright stars, ideally suited to this technique. with it's unique combination of uv to nir wavelength coverage and... | transmission spectroscopy of exoplanets with luvoir |
the atmospheres of highly irradiated exoplanets are observed to undergo hydrodynamic escape, resulting in planetary mass loss. however, stellar winds can shape and even prevent atmospheric escape, affecting observable signatures of escape such as lyman-alpha and h-alpha line profiles. in this work, we simulate atmosphe... | how stellar winds can affect atmospheric escape in close-in exoplanets |
we use maven data and models to assess how crustal magnetic fields modify the escape rates of atmospheric ions. this has applicability to a big picture question for mars, planetary, and exoplanetary science: do magnetic fields influence habitability? | do magnetic fields matter? |
with a simple transmission code, we compute high-resolution transit spectra of the sodium/potassium doublet with arbitrary number density profiles as input (in particular non-hydrostatic ones). while hydrostatic atmospheres absorb mostly in an optically thick regime, we find that non-hydrostatic atmospheres (such as es... | nonhydrostatic density profiles of sodium & potassium at close-in gas giant exoplanets |
host stars create environments that shape the atmospheric structure and composition of their exoplanets, the effects of which we observe today. the stellar wind and high energy radiation present within astrospheres can erode planetary atmospheres, leading to the detections of atmospheric evaporation for short-period pl... | the evaporating atmosphere of the young exoplanet k2-25b |
most planets in the solar system have or previously had a global magnetic field, yet not much is known about magnetic fields in exoplanets. information about the presence of a magnetic field and its strength could give us valuable insights into the interior structure and thermal evolution of an exoplanet. furthermore, ... | detecting magnetic fields in exoplanets with spectropolarimetry in the helium line at 1083 nm |
we present 3d mhd simulations of the wind-wind interactions that occur between a solar-type star and a short period hot jupiter exoplanet. a planetary outflow results from atmospheric escape induced by the host stars incident radiation. circumstellar and circumplanetary material which accretes onto the stellar surface ... | it's raining hot jupiters: 3d mhd simulations of planetary atmospheric escape |
observational breakthroughs in the exoplanet field of the last decade motivated the development of numerous theoretical models describing atmospheres and mass loss, which is believed to be one of the main drivers of planetary evolution. we aim to outline for which types of close-in planets in the neptune-mass range the... | precise photoionisation treatment and hydrodynamic effects in atmospheric modelling of warm and hot neptunes |
a large fraction of known exoplanets orbit their host stars at very short periods. due to such close proximity to the parent star, their atmospheres are exposed to high levels of stellar radiation and stellar wind, as well as strong tidal interactions, which can lead to atmospheric escape operating in a regime much mor... | heavy metals escaping from a hot neptune |
intuition for the various regimes of atmospheric escape driven by stellar interactions will be given through order of magnitude sketches. consideration will be given to both planetary parameters and the stellar environment in which the planet resides. thereafter, detailed models will be presented focusing on the most d... | atmospheric escape for close-in exoplanets |
both rocky super-earths and volatile-rich sub-neptunes have been found simultaneously in multi-planetary systems, suggesting that these systems are appropriate to study different composition and formation pathways within the same environment. to estimate their composition, we present an interior structure model that in... | water content trends in low-mass multiplanetary systems |
ultra-hot jupiter is a new class of exoplanets emerging in the recent years. their extremely hot temperatures cause thermal dissociation of molecules and even ionisation of atoms. we have detected an extended hot hydrogen atmosphere around kelt-9b — the hottest exoplanet discovered so far. the detection was achieved by... | high resolution transmission spectrum of ultra-hot jupiters |
in this white paper we focus on the science case for exoplanet observations at near-uv/blue optical wavelengths. scattering information encoded in at these wavelengths can distinguish the cause of muted spectral features. these wavelengths also capture atmospheric escape processes, and help characterize mass loss from ... | understanding exoplanet atmospheres with uv observations i: nuv and blue/optical |
of the three terrestrial worlds that have significant atmospheres (venus, earth, and mars), only earth also possesses a global dynamo magnetic field. this magnetic field is often thought to have shielded the planet from the impinging solar wind, preventing the atmosphere from being stripped away to space. the atmospher... | do habitable worlds require magnetic fields? |
in this white paper we focus on the science case for exoplanet observations in the far-uv (fuv); an accompanying white paper led by jessie christiansen will focus on the science case in the nuv and blue/optical. | understanding exoplanet atmospheres with uv observations ii: the far uv and atmospheric escape |
atmospheric escape is the prevailing evolutionary theory that explains current exoplanet demographics - pertaining to the most common exoplanet types, short-period sub-neptunes and super-earths, in particular. two planets have been detected around the 23 myr pre-main sequence m dwarf au mic; their known age makes them ... | a young burping planet: characterizing the variable atmospheric escape of the exciting au mic b |
atmospheres of exoplanets are our main observing window into the physical and chemical properties of these remote worlds. spectacular progress has already been made on the atmospheric characterisation of exoplanets, highlighting a huge diversity compared to our solar system planets. in particular, hot exoplanets found ... | toward the characterization of upper atmospheres with a 3d coupled thermosphere-exosphere model |
spectroscopy of transiting exoplanets has revealed a wealth of information about their atmospheric compositions and thermal structures. in particular, studies of highly irradiated exoplanets at temperatures much higher than those found in our solar system have provided detailed information on planetary chemistry and ph... | revealing the atmospheres of highly irradiated exoplanets: from ultra-hot jupiters to rocky worlds |
we present a simple analytic description of atmospheric mass loss by aerial bursts and demonstrate that mass loss from aerial bursts becomes significant when the maximum impactor size that leads to an aerial burst rather than a ground explosion, ro, is larger than the minimum impactor size needed to achieve atmospheric... | atmosphere loss by aerial bursts |
ultra-hot jupiters (uhjs) provide a natural laboratory of rapid atmospheric escape that can be used to test models of this process. uhjs have dayside temperatures in excess of 2200 k, which means that metals and heavy elements are not likely to condense on the dayside. metals like fe and mg can often escape their atmos... | atmospheric escape and near-uv signatures of ultra-hot jupiters |
as the exoplanet wasp-107b orbits its host star, its atmosphere escapes to form a comet-like tail. helium atoms detected in the escaping gases give astronomers a powerful tool for investigating exoplanetary atmospheres. | helium discovered in the tail of an exoplanet |
exoplanet radii show a bimodal distribution, with two peaks corresponding to smaller planets (likely rocky) and larger intermediate-size planets, respectively. we apply interior structure model, growth model, as well as atmospheric escape model, and conduct monte carlo simulations, to demonstrate that many intermediate... | iceland, iceline, iceplanets |
this work shows results from magma ocean outgassing and hydrodynamic escape processes on the mass and longevity of secondary atmospheres on rocky exoplanets. | the transition from primary to secondary atmospheres on rocky exoplanets |
the atmospheres of close-in, low-mass exoplanets are extremely vulnerable to the effects of stellar uv to x-ray radiation. photoevaporation can significantly ablate planetary atmospheres or even strip them entirely, potentially rendering a planet uninhabitable. existing hydrodynamical studies of this important atmosphe... | photoevaporation of water dominated exoplanet atmospheres |
the observed exoplanet population unveiled by recent detection programs is billions of years old, distinctly separated in time from the planet formation process that only lasted ~10-100 myr. i will argue that photo evaporation driven atmospheric escape has been one of the key evolutionary drivers shaping the exoplanet ... | the evaporation driven evolution of close-in exoplanets |
exoplanet research has become a major focus due to advancements like the transit method, which allows us to observe the features of exoplanet atmospheres. shared features between exoplanetary atmospheres and their host stars limit confidence on any atmospheric interpretation. our ability to characterize the variability... | characterizing variability for solar he i 1083 nm |
the photoionization-driven evaporation of planetary atmospheres appears to be a fundamental process for exoplanets on short period orbits. given its importance, it is vital that photoevaporation be explored as a fully 3-d multi-physics process facilitating detailed comparison with existing observations. using astrobear... | exoplanet photoevaporation and mass loss: why don't theory and observation match? |
the extreme ultraviolet (euv) emission from stars is the dominant source of heating to the upper atmospheres of planets and drives atmospheric escape, but this wavelength regime is unobserved for most exoplanet host stars. the differential emission measure technique is a method to infer the euv emission of stars using ... | a library of extreme ultraviolet spectra for 115 main-sequence stars to enable comparative exoplanet studies |
the recent observations on wasp-39 b by jwst have revealed hints of high metallicity within the atmosphere compared to its host star. there are various theories on how these high metallic atmospheres emerge. in this study, we closely investigate the impact of extreme escape in the form of hydrodynamic escape to see its... | metallicity and spectral evolution of wasp 39b: the limited role of hydrodynamic escape |
kepler's observations show most of the exoplanets are super-earths. the formation of a super-earth is generally related to the atmospheric mass loss that is crucial in the planetary structure and evolution. the shock driven by the giant impact will heat the planet, resulting in the atmosphere escape. we focus on whethe... | effects of self-gravity on mass-loss of the post-impact super-earths |
characterizing rocky exoplanet atmospheres is a key goal of exoplanet science, but interpreting such observations will require understanding the stellar ultraviolet (uv) irradiation incident on the planet from its host star. stellar uv mediates atmospheric escape, photochemistry, and planetary habitability, and observa... | uv spectral characterization of low-mass stars with astrosat uvit for exoplanet applications: the case study of hip 23309 |
x-ray observations of star-planet systems are important to grow our understanding of exoplanets; these observation allow for studies of photoevaporation of the exoplanetary atmosphere, and in some cases even estimations of the size of the outer planetary atmosphere. the german-russian erosita instrument onboard the srg... | identifying interesting planetary systems for future x-ray observations |
the atmosphere of a terrestrial planet that is replenished with secondary gases should have accumulated hydrogen-rich gas from its protoplanetary disk. although a giant impact blows off a large fraction of the primordial atmosphere of a terrestrial planet in the late formation stage, the remaining atmosphere can become... | evolution of a water-rich atmosphere formed by a giant impact on an earth-sized planet |
the absorption signals of metastable he in hd 209458b and several other exoplanets can be explained via an escaping atmosphere model with a subsolar he/h ratio. the low abundance of helium can be a result of planet formation if there is a small amount of helium in their primordial atmosphere. however, another possibili... | the mass fractionation of helium in the escaping atmosphere of hd 209458b |
spectral observations in the ly-α line have shown that atmospheric escape is variable and for the exoplanet hd189733b, the atmospheric evaporation goes from undetected to enhanced evaporation in a 1.5 years interval. to understand the temporal variation in the atmospheric escape, we investigate the effect of flares, wi... | effect of stellar flares and coronal mass ejections on the atmospheric escape from hot jupiters |
the lyα emission line is the brightest uv emission line in m and k dwarf spectra and serves as an important tool for studies of stellar chromospheres, the interstellar medium, and exoplanet atmospheres. however, lyα observations have proven difficult due to the strong absorption by the interstellar medium, necessitatin... | new and improved lyα reconstructions for m and k dwarfs |
in this presentation, we make use of sophisticated 3d numerical simulations to assess the extent of atmospheric ion (e.g., o+, o2+ and co2+) losses from venus over time. a sophisticated upper atmospheric model (venus thermospheric general circulation model - vtgcm) is coupled with a magnetohydrodynamic (mhd) code, bats... | modeling venusian atmospheric losses over time |
multi-planet systems offer insight into a host star's influence on its planets' atmospheres. k2-3 is an m0 star (effective temperature of 3880 k) orbited by three small transiting planets, k2-3b, c, and d (2.0, 1.6, and 1.4 earth radii, respectively). we combine stellar spectral information with self-consistently deriv... | a visit to the k2-3 system: models of three planetary atmospheres spanning the radius valley informed by a high energy stellar spectrum and updated system properties |
dust clouds are ubiquitous in the atmospheres of hot jupiters and affect their observable properties. the alignment of dust grains in the clouds and resulting dust polarization is a promising method to study magnetic fields of exoplanets. moreover, the grain size distribution plays an important role in physical and che... | grain alignment and rotational disruption by radiative torques in exoplanet atmospheres |
we present two novel additions to the semianalytic solution of lyα radiative transfer in spherical geometry: (1) implementation of the correct boundary condition for a steady source, and (2) solution of the time-dependent problem for an impulsive source. for the steady-state problem, the solution can be represented as ... | a novel solution for resonant scattering using self-consistent boundary conditions |
one of jwst's four pillars of science points to finding the building blocks of life elsewhere in the universe. planets orbiting m-dwarf stars represent our best (and only) opportunity to measure the spectrum of a potentially-habitable planet in the next decade. the quest towards habitability begins with a simple questi... | tell me how i?m supposed to breathe with no air: measuring the prevalence and diversity of m-dwarf planet atmospheres |
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