Atmospheric Mass Loss from Hot Jupiters Irradiated by Stellar Superflares

Bisikalo, D. V.; Shematovich, V. I.; Черенков, А. А.; Fossati, L.; Möstl, Christian

doi:10.3847/1538-4357/aaed21

Cited by 27 publications

(15 citation statements)

References 20 publications

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“…Regardless of whether exoplanets lie along CME trajectories, they can nevertheless be affected by the almost-instantaneous increase in irradiation caused by an eventual CME-associated flare, since this emission covers a wider solid angle. An increase in irradiation input caused by a flare can lead to increase in evaporation in close-in gas giants (Cherenkov et al 2017;Bisikalo et al 2018;Hazra et al 2020). Transit observations of the hot Jupiter HD189733b showed an enhancement of atmospheric evaporation that took place 8h after the host star flared.…”

Section: Implication For Exoplanets and New Lessons For The Solar Systemmentioning

confidence: 99%

The evolution of the solar wind

Vidotto

2021

Living Rev Sol Phys

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How has the solar wind evolved to reach what it is today? In this review, I discuss the long-term evolution of the solar wind, including the evolution of observed properties that are intimately linked to the solar wind: rotation, magnetism and activity. Given that we cannot access data from the solar wind 4 billion years ago, this review relies on stellar data, in an effort to better place the Sun and the solar wind in a stellar context. I overview some clever detection methods of winds of solar-like stars, and derive from these an observed evolutionary sequence of solar wind mass-loss rates. I then link these observational properties (including, rotation, magnetism and activity) with stellar wind models. I conclude this review then by discussing implications of the evolution of the solar wind on the evolving Earth and other solar system planets. I argue that studying exoplanetary systems could open up new avenues for progress to be made in our understanding of the evolution of the solar wind.

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Section: Implication For Exoplanets and New Lessons For The Solar Systemmentioning

confidence: 99%

The evolution of the solar wind

Vidotto

2021

Living Rev Sol Phys

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“…Notable amongst the former is the 1-D code developed by Erkaev et al (2016); similar to ATES in its hydrodynamics, energy and ionization balance treatment (unlike ATES, it includes thermal conduction, but neglects He ), this code has been extensively used (by the many contributing authors) to estimate the atmospheric profiles and mass outflow rates for several, wellknown, highly irradiated exoplanets (e.g., Erkaev et al 2017;Fossati et al 2017;Kubyshkina et al 2018a;Odert et al 2020, to name a few). More recently developed (proprietary) 1-D hydrodynamics codes include Vidotto & Cleary (2020) (following Allan & Vidotto 2019), which computes the effects of the stellar wind ram pressure on the atmospheric outflow, and Bisikalo et al (2018), which adapts the code by (Ionov et al 2017) to account for the role of supra-thermal photo-electrons during stellar flares. Somewhat separately, Chen & Rogers (2016) developed a prescription to adapt the capabilities of the Modules for Experiments in Stellar Astrophysics (MESA) to model sub-Neptunesized planets with H -He envelopes.…”

Section: Comparison To Other Existing Codesmentioning

confidence: 99%

“…As a result, in the last two decades much effort has gone into the development of more realistic, numerical models of atmospheric escape (Lammer et al 2003;Yelle 2004;Tian et al 2005;García Muñoz 2007;Murray-Clay et al 2009;Owen & Jackson 2012;Erkaev et al 2013;Erkaev et al 2015Erkaev et al , 2016Salz et al 2015;Debrecht et al 2019;McCann et al 2019;Esquivel et al 2019;Vidotto & Cleary 2020). Specific exoplanet targets have been modeled with a great deal of sophistication, also accounting for 2D and/or 3D effects and complex chemistry (see, e.g, Ehrenreich et al 2015b andKhodachenko et al 2019 for GJ 436 b, Koskinen et al 2013, Khodachenko et al 2017, Bisikalo et al 2018and Debrecht et al 2020 for HD 209458 b, Odert et al 2020 for HD 189733 b). Typically, these models aim to reproduce the results of time-intensive transit spectroscopy campaigns, and are extremely computationally expensive; as a corollary, the associated numerical solvers are seldom publicly available.…”

Section: Introductionmentioning

confidence: 99%

Irradiation-driven escape of primordial planetary atmospheres

Caldiroli

Haardt

Gallo

et al. 2021

A&A

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Intense X-ray and ultraviolet stellar irradiation can heat and inflate the atmospheres of closely orbiting exoplanets, driving mass outflows that may be significant enough to evaporate a sizable fraction of the planet atmosphere over the system lifetime. The recent surge in the number of known exoplanets, together with the imminent deployment of new ground and space-based facilities for exoplanet discovery and characterization, requires a prompt and efficient assessment of the most promising targets for intensive spectroscopic follow-ups. For this purpose, we developed ATmospheric EScape (ATES), a new hydrodynamics code that is specifically designed to compute the temperature, density, velocity, and ionization fraction profiles of highly irradiated planetary atmospheres, along with the current, steady-state mass loss rate. ATES solves the one-dimensional Euler, mass, and energy conservation equations in radial coordinates through a finite-volume scheme. The hydrodynamics module is paired with a photoionization equilibrium solver that includes cooling via bremsstrahlung, recombination, and collisional excitation and ionization for the case of a primordial atmosphere entirely composed of atomic hydrogen and helium, whilst also accounting for advection of the different ion species. Compared against the results of 14 moderately to highly irradiated planets simulated with The PLUTO-CLOUDY Interface (TPCI), which couples two sophisticated and computationally expensive hydrodynamics and radiation codes of much broader astrophysical applicability, ATES yields remarkably good agreement at a significantly smaller fraction of the time. A convergence study shows that ATES recovers stable, steady-state hydrodynamic solutions for systems with log(−Φp)≲12.9 + 0.17 log FXUV, where Φp and FXUV are the planet gravitational potential and stellar flux (in cgs units). Incidentally, atmospheres of systems above this threshold are generally thought to be undergoing Jeans escape. The code, which also features a user-friendly graphic interface, is available publicly as an online repository.

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“…Vidotto et al 2011bVidotto et al , 2014. Additionally, short-term events such as coronal mass ejections and flares can also affect planetary escape (Cherenkov et al 2017;Bisikalo et al 2018). Therefore, it is possible that the variation in stellar outflow of WASP-12b, its orbital distance is smaller than the minimum orbital distance considered here.…”

Section: Inhomogeneities In the Stellar Wind And The Stability Of Escmentioning

confidence: 99%

Stellar wind effects on the atmospheres of close-in giants: a possible reduction in escape instead of increased erosion

Vidotto

Cleary

2020

Monthly Notices of the Royal Astronomical Society

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The atmospheres of highly irradiated exoplanets are observed to undergo hydrodynamic escape. However, due to strong pressures, stellar winds can confine planetary atmospheres, reducing their escape. Here, we investigate under which conditions atmospheric escape of close-in giants could be confined by the large pressure of their host star's winds. For that, we simulate escape in planets at a range of orbital distances ([0.04, 0.14] au), planetary gravities ([36%, 87%] of Jupiter's gravity), and ages ([1, 6.9] Gyr). For each of these simulations, we calculate the ram pressure of these escaping atmospheres and compare them to the expected stellar wind external pressure to determine whether a given atmosphere is confined or not. We show that, although younger close-in giants should experience higher levels of atmospheric escape, due to higher stellar irradiation, stellar winds are also stronger at young ages, potentially reducing escape of young exoplanets. Regardless of the age, we also find that there is always a region in our parameter space where atmospheric escape is confined, preferably occurring at higher planetary gravities and orbital distances. We investigate confinement of some known exoplanets and find that the atmosphere of several of them, including π Men c, should be confined by the winds of their host stars, thus potentially preventing escape in highly irradiated planets. Thus, the lack of hydrogen escape recently reported for π Men c could be caused by the stellar wind.

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Atmospheric Mass Loss from Hot Jupiters Irradiated by Stellar Superflares

Cited by 27 publications

References 20 publications

The evolution of the solar wind

The evolution of the solar wind

Irradiation-driven escape of primordial planetary atmospheres

Stellar wind effects on the atmospheres of close-in giants: a possible reduction in escape instead of increased erosion

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