ERRATUM: “SIMULATED PHOTOEVAPORATIVE MASS LOSS FROM HOT JUPITERS IN 3D” (2015, ApJ, 808, 173)

2015 ◽  
Vol 811 (2) ◽  
pp. 159
Author(s):  
Anjali Tripathi ◽  
Kaitlin M. Kratter ◽  
Ruth A. Murray-Clay ◽  
Mark R. Krumholz
Keyword(s):  
Mass Loss ◽  
Hot Jupiters

Exoplanet Upper Atmosphere Environment Characterization

2011 ◽  
Vol 7 (S282) ◽  
pp. 525-532 ◽  
Author(s):  
Helmut Lammer ◽  
Kristina G. Kislyakova ◽  
Petra Odert ◽  
Martin Leitzinger ◽  
Maxim L. Khodachenko ◽  
...  
Keyword(s):  
Magnetic Properties ◽  
Mass Loss ◽  
Radiation Exposure ◽  
High Temperatures ◽  
Stellar Wind ◽  
Numerical Models ◽  
Large Mass ◽  
Upper Atmosphere ◽  
Hot Jupiters ◽  
Atmosphere Environment

AbstractThe intense stellar SXR and EUV radiation exposure at “Hot Jupiters” causes profound responses to their upper atmosphere structures. Thermospheric temperatures can reach several thousands of Kelvins, which result in dissociation of H2 to H and ionization of H to H+. Depending on the density and orbit location of the exoplanet, as a result of these high temperatures the thermosphere expands dynamically up to the Roche lobe, so that geometric blow-off with large mass loss rates and intense interaction with the stellar wind plasma can occur. UV transit observations together with advanced numerical models can be used to gain knowledge on stellar plasma and the planet's magnetic properties, as well as the upper atmosphere.

scholarly journals Swift UVOT near-UV transit observations of WASP-121 b

2019 ◽  
Vol 623 ◽  
pp. A57 ◽  
Author(s):  
M. Salz ◽  
P. C. Schneider ◽  
L. Fossati ◽  
S. Czesla ◽  
K. France ◽  
...  
Keyword(s):  
Mass Loss ◽  
Spectral Range ◽  
Relative Accuracy ◽  
Uv Absorption ◽  
Absorption Lines ◽  
Optical Telescope ◽  
Hot Jupiters ◽  
Excess Absorption ◽  
Loss Rates ◽  
Gas Planets

Close-in gas planets are subject to continuous photoevaporation that can erode their volatile envelopes. Today, ongoing mass loss has been confirmed in a few individual systems via transit observations in the ultraviolet spectral range. We demonstrate that the Ultraviolet/Optical Telescope (UVOT) onboard the Neil Gehrels Swift Observatory enables photometry to a relative accuracy of about 0.5% and present the first near-UV (200–270 nm, NUV) transit observations of WASP-121 b, a hot Jupiter with one of the highest predicted mass-loss rates. The data cover the orbital phases 0.85–1.15 with three visits. We measure a broadband NUV transit depth of 2.10 ± 0.29%. While still consistent with the optical value of 1.55%, the NUV data indicate excess absorption of 0.55% at a 1.9σ level. Such excess absorption is known from the WASP-12 system, and both of these hot Jupiters are expected to undergo mass loss at extremely high rates. With a Cloudy simulation, we show that absorption lines of Fe II in a dense extended atmosphere can cause broadband near-UV absorption at the 0.5% level. Given the numerous lines of low-ionization metals, the NUV range is a promising tracer of photoevaporation in the hottest gas planets.

scholarly journals Measuring and modeling the Balmer series in hot gaseous giant exoplanets

2020 ◽  
Author(s):  
Aurélien Wyttenbach ◽  
Paul Mollière ◽  
David Ehrenreich ◽  
Heather Cegla ◽  
Vincent Bourrier ◽  
...  
Keyword(s):  
Mass Loss ◽  
Loss Rate ◽  
Mass Loss Rate ◽  
Atmospheric Model ◽  
Balmer Series ◽  
Hot Jupiters ◽  
Atmospheric Escape ◽  
Line Shapes ◽  
Early Type Star ◽  
Photo Ionization

<p>Atmospheric escape rate is a key parameter to measure in order to understand the evolution of exoplanets. In this presentation, we will show that the Balmer series, observed with high-resolution transmission spectroscopy, is a precise probe to measure exoplanet evaporation, especially for ultra hot Jupiters orbiting early-type star. These hot gaseous giant exoplanets (such as KELT-9 b) are presumed to have an atmosphere dominated by neutral and ionized atomic species. In particular, hydrogen Balmer lines have been detected in some of their upper atmospheres, suggesting that hydrogen is filling the planetary Roche lobe and escaping from these planets. Here, we will present new significant absorptions of the Balmer series in the KELT-9b atmosphere obtained with HARPS-N. The precise line shapes of the Hα, Hβ, and Hγ absorptions allow us to put constraints on the thermospheric temperature. Moreover, the mass loss rate, and the excited hydrogen population of KELT-9 b are also constrained, thanks to a retrieval analysis performed with a new atmospheric model (the PAWN model). We retrieved a thermospheric temperature of T = 13 200+800-720 K and a mass loss rate of log10(MLR) = 10^(12.8+-0.3) g/s when the atmosphere was assumed to be in hydrodynamical expansion and in local thermodynamic equilibrium (LTE). Since the thermospheres of hot Jupiters are not expected to be in LTE, we explored atmospheric structures with non-Boltzmann equilibrium for the population of the excited hydrogen. We do not find strong statistical evidence in favor of a departure from LTE. However, our non-LTE scenario suggests that a departure from the Boltzmann equilibrium may not be sufficient to explain the retrieved low number densities of the excited hydrogen. In non-LTE, Saha equilibrium departure via photo-ionization, is also likely to be necessary to explain the data.</p>

scholarly journals Five New Hot Jupiter Transits Investigated with Swift-UVOT

2021 ◽  
Vol 162 (6) ◽  
pp. 287
Author(s):  
Lia Corrales ◽  
Sasikrishna Ravi ◽  
George W. King ◽  
Erin May ◽  
Emily Rauscher ◽  
...  
Keyword(s):  
Mass Loss ◽  
Loss Rate ◽  
Mass Loss Rate ◽  
Equilibrium Temperature ◽  
Light Curves ◽  
X Ray ◽  
Hot Jupiters ◽  
Upper Limits ◽  
Marginal Detection ◽  
Optical Radius

Abstract Short-wavelength exoplanet transit measurements have been used to probe mass loss in exoplanet atmospheres. We present the Swift-UVOT transit light curves for five hot Jupiters orbiting UV-bright F-type stars: XO-3, KELT-3, WASP-3, WASP-62, and HAT-P-6. We report one positive transit detection of XO-3b and one marginal detection of KELT-3b. We place upper limits on the remaining three transit depths. The planetary radii derived from the NUV transit depths of both potential detections are 50%–100% larger than their optical radius measurements. We examine the ratio R NUV/R opt for trends as a function of estimated mass-loss rate, which we derive from X-ray luminosity obtained from the Swift-XRT or, in the case of WASP-62, XMM-Newton. We find no correlation between the energy-limited photoevaporative mass-loss rate and the R NUV/R opt ratio. We also search for trends based on the equilibrium temperature of the hot Jupiters. We find a possible indication of a transition in the R NUV/R opt ratio around T eq = 1700 K, analogous to the trends found for NIR water features in transmission spectra. This might be explained by the formation of extended cloud decks with silicate particles ≤1 μm. We demonstrate that the Swift-UVOT filters could be sensitive to absorption from aerosols in exoplanet atmospheres.

scholarly journals Comparative analysis of the influence of Sgr A* and nearby active galactic nuclei on the mass loss of known exoplanets

2019 ◽  
Vol 624 ◽  
pp. A71 ◽  
Author(s):  
A. M. Wisłocka ◽  
A. B. Kovačević ◽  
A. Balbi
Keyword(s):  
Mass Loss ◽  
Sloan Digital Sky Survey ◽  
Galactic Bulge ◽  
Incorrect Choice ◽  
Mars Atmosphere ◽  
Hot Jupiters ◽  
Sagittarius A ◽  
Exoplanetary Atmospheres ◽  
Sgr A ◽  
Atmospheric Mass

Context. The detailed evolution of exoplanetary atmospheres has been the subject of decade-long studies. Only recently, investigations began on the possible atmospheric mass loss caused by the activity of galactic central engines. This question has so far been explored without using available exoplanet data. Aims. The goal of this paper is to improve our knowledge of the erosion of exoplanetary atmospheres through radiation from supermassive black holes (SMBHs) undergoing an active galactic nucleus (AGN) phase. Methods. To this end, we extended the well-known energy-limited mass-loss model to include the case of radiation from AGNs. We set the fraction of incident power ɛ available to heat the atmosphere as either constant (ɛ = 0.1) or flux dependent (ɛ = ɛ(FXUV)). We calculated the possible atmospheric mass loss for 54 known exoplanets (of which 16 are hot Jupiters residing in the Galactic bulge and 38 are Earth-like planets, EPs) due to radiation from the Milky Way’s (MW) central SMBH, Sagittarius A* (Sgr A*), and from a set of 107 220 AGNs generated using the 33 350 AGNs at z < 0.5 of the Sloan Digital Sky Survey database. Results. We found that planets in the Galactic bulge might have lost up to several Earth atmospheres in mass during the AGN phase of Sgr A*, while the EPs are at a safe distance from Sgr A* (>7 kpc) and have not undergone any atmospheric erosion in their lifetimes. We also found that the MW EPs might experience a mass loss up to ~15 times the Mars atmosphere over a period of 50 Myr as the result of exposure to the cumulative extreme-UV flux FXUV from the AGNs up to z = 0.5. In both cases we found that an incorrect choice of ɛ can lead to significant mass loss overestimates.

scholarly journals High-energy irradiation and mass loss rates of hot Jupiters in the solar neighborhood

2015 ◽  
Vol 576 ◽  
pp. A42 ◽  
Author(s):  
M. Salz ◽  
P. C. Schneider ◽  
S. Czesla ◽  
J. H. M. M. Schmitt
Keyword(s):  
Mass Loss ◽  
High Energy ◽  
Solar Neighborhood ◽  
Hot Jupiters ◽  
Energy Irradiation ◽  
High Energy Irradiation ◽  
Loss Rates

scholarly journals Atmospheric Mass Loss from Hot Jupiters Irradiated by Stellar Superflares

2018 ◽  
Vol 869 (2) ◽  
pp. 108 ◽  
Author(s):  
D. V. Bisikalo ◽  
V. I. Shematovich ◽  
A. A. Cherenkov ◽  
L. Fossati ◽  
C. Möstl
Keyword(s):  
Mass Loss ◽  
Hot Jupiters ◽  
Atmospheric Mass

scholarly journals A data-driven approach to constraining the atmospheric temperature structure of the ultra-hot Jupiter KELT-9b

2020 ◽  
Vol 643 ◽  
pp. A131
Author(s):  
L. Fossati ◽  
D. Shulyak ◽  
A. G. Sreejith ◽  
T. Koskinen ◽  
M. E. Young ◽  
...  
Keyword(s):  
Mass Loss ◽  
Thermodynamic Equilibrium ◽  
Local Thermodynamic Equilibrium ◽  
Mass Loss Rate ◽  
Atmospheric Temperature ◽  
High Mass ◽  
Temperature Structure ◽  
Hot Jupiters ◽  
Data Driven Approach ◽  
Hot Jupiter

Context. Observationally constraining the atmospheric temperature-pressure (TP) profile of exoplanets is an important step forward for improving planetary atmosphere models, thus further enabling one to place the detection of spectral features and the measurement of atomic and molecular abundances through transmission and emission spectroscopy on solid ground. Aims. The aim is to constrain the TP profile of the ultra-hot Jupiter KELT-9b by fitting synthetic spectra to the observed Hα and Hβ lines and identify why self-consistent planetary TP models are unable to fit the observations. Methods. We constructed 126 one-dimensional TP profiles varying the lower and upper atmospheric temperatures, as well as the location and gradient of the temperature rise. For each TP profile, we computed the transmission spectra of the Hα and Hβ lines employing the Cloudy radiative transfer code, which self-consistently accounts for non-local thermodynamic equilibrium (NLTE) effects. Results. The TP profiles, leading to best fit the observations, are characterised by an upper atmospheric temperature of 10 000–11 000 K and by an inverted temperature profile at pressures higher than 10−4 bar. We find that the assumption of local thermodynamic equilibrium (LTE) leads one to overestimate the level population of excited hydrogen by several orders of magnitude and hence to significantly overestimate the strength of the Balmer lines. The chemical composition of the best fitting models indicate that the high upper atmospheric temperature is most likely driven by metal photoionisation and that FeII and FeIII have comparable abundances at pressures lower than 10−6 bar, possibly making the latter detectable. Conclusions. Modelling the atmospheres of ultra-hot Jupiters requires one to account for metal photoionisation. The high atmospheric mass-loss rate (>1011 g s−1), caused by the high temperature, may have consequences on the planetary atmospheric evolution. Other ultra-hot Jupiters orbiting early-type stars may be characterised by similarly high upper atmospheric temperatures and hence high mass-loss rates. This may have consequences on the basic properties of the observed planets orbiting hot stars.

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