Magnetospheres of hot Jupiters: hydrodynamic models and ultraviolet absorption

Alexander, R. D.; Wynn, G. A.; Mohammed, Hastyar Omar; Nichols, J. D.; Ercolano, Barbara

doi:10.1093/mnras/stv2867

Cited by 39 publications

(45 citation statements)

References 37 publications

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“…Theory predicts that several mechanisms can generate (pre-)transitional disk SEDs, all of which are important for disk evolution. Table 2 summarizes the generic properties expected for (pre-)transitional disks produced by different mechanisms, as previously described in § 3 and the literature (e.g., Najita et al 2007a;Alexander and Armitage 2007). Which of these occur commonly (or efficiently) and on what timescale(s)?…”

Section: Demographicsmentioning

confidence: 93%

“…Another mechanism for sculpting (pre-)transitional disk structures relies on the complementary interactions of viscous evolution, dust migration, and disk dispersal via photoevaporative winds (Hollenbach et al 1994;Clarke et al 2001;Alexander et al 2006;Alexander and Armitage 2007;Gorti and Hollenbach 2009;Gorti et al 2009;Owen et al 2010Owen et al , 2011Rosotti et al 2013). Here, the basic idea is that the high-energy irradiation of the disk surface by the central star can drive mass-loss in a wind that will eventually limit the re-supply of inner disk material from accretion flows.…”

Section: Photoevaporationmentioning

confidence: 99%

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An Observational Perspective of Transitional Disks

Espaillat¹,

Muzerolle²,

Najita³

et al. 2014

Protostars and Planets VI

198

204

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Transitional disks are objects whose inner disk regions have undergone substantial clearing. The Spitzer Space Telescope produced detailed spectral energy distributions (SEDs) of transitional disks that allowed us to infer their radial dust disk structure in some detail, revealing the diversity of this class of disks. The growing sample of transitional disks also opened up the possibility of demographic studies, which provided unique insights. There now exist (sub)millimeter and infrared images that confirm the presence of large clearings of dust in transitional disks. In addition, protoplanet candidates have been detected within some of these clearings. Transitional disks are thought to be a strong link to planet formation around young stars and are a key area to study if further progress is to be made on understanding the initial stages of planet formation. Here we provide a review and synthesis of transitional disk observations to date with the aim of providing timely direction to the field, which is about to undergo its next burst of growth as ALMA reaches its full potential. We discuss what we have learned about transitional disks from SEDs, color-color diagrams, and imaging in the (sub)mm and infrared. We note the limitations of these techniques, particularly with respect to the sizes of the clearings currently detectable, and highlight the need for pairing broad-band SEDs with multi-wavelength images to paint a more detailed picture of transitional disk structure. We review the gas in transitional disks, keeping in mind that future observations with ALMA will give us unprecedented access to gas in disks, and also observed infrared variability pointing to variable transitional disk structure, which may have implications for disks in general. We then distill the observations into constraints for the main disk clearing mechanisms proposed to date (i.e., photoevaporation, grain growth, and companions) and explore how the expected observational signatures from these mechanisms, particularly planet-induced disk clearing, compare to actual observations. Lastly, we discuss future avenues of inquiry to be pursued with ALMA, JWST, and next generation of ground-based telescopes.

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Section: Demographicsmentioning

confidence: 93%

Section: Photoevaporationmentioning

confidence: 99%

An Observational Perspective of Transitional Disks

Espaillat¹,

Muzerolle²,

Najita³

et al. 2014

Protostars and Planets VI

198

204

View full text Add to dashboard Cite

show abstract

“…Like the pure hydrodynamic calculations, work has also been done on the interaction of the flow with the broader interplanetary environment, where the interaction between any planetary magnetic field, the outflow and the stellar magnetic field ultimately controls what happens to the gas that has escaped the planet (Matsakos et al 2015;Alexander et al 2016;Daley-Yates & Stevens 2017;Villarreal D'Angelo et al 2018).…”

Section: The Role Of Magnetic Fieldsmentioning

confidence: 99%

Atmospheric Escape and the Evolution of Close-In Exoplanets

Owen

2019

Annu. Rev. Earth Planet. Sci.

249

165

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Exoplanets with substantial Hydrogen/Helium atmospheres have been discovered in abundance, many residing extremely close to their parent stars. The extreme irradiation levels these atmospheres experience causes them to undergo hydrodynamic atmospheric escape. Ongoing atmospheric escape has been observed to be occurring in a few nearby exoplanet systems through transit spectroscopy both for hot Jupiters and lower-mass super-Earths/mini-Neptunes. Detailed hydrodynamic calculations that incorporate radiative transfer and ionization chemistry are now common in one-dimensional models, and multi-dimensional calculations that incorporate magnetic-fields and interactions with the interstellar environment are cutting edge. However, there remains very limited comparison between simulations and observations. While hot Jupiters experience atmospheric escape, the mass-loss rates are not high enough to affect their evolution. However, for lower mass planets atmospheric escape drives and controls their evolution, sculpting the exoplanet population we observe today.

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“…The behaviour of the EUV wind changes significantly in the case of a disk with an optically thin inner hole, as the heating is dominated by direct irradiation from the central star. Alexander et al (2006a) studied this problem using both analytic arguments and 2-D numerical hydrodynamics. As the direct field dominates they were able to compute the location of the ionization front "on-the-fly" in their hydrodynamic calculations, and find a self-consistent flow solution.…”

Section: Euv Heatingmentioning

confidence: 99%

The Dispersal of Protoplanetary Disks

Alexander¹,

Pascucci²,

Andrews³

et al. 2014

Protostars and Planets VI

226

266

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Protoplanetary disks are the sites of planet formation, and the evolution and eventual dispersal of these disks strongly influences the formation of planetary systems. Disk evolution during the planet-forming epoch is driven by accretion and mass-loss due to winds, and in typical environments photoevaporation by high-energy radiation from the central star is likely to dominate final gas disk dispersal. We present a critical review of current theoretical models, and discuss the observations that are used to test these models and inform our understanding of the underlying physics. We also discuss the role disk dispersal plays in shaping planetary systems, considering its influence on both the process(es) of planet formation and the architectures of planetary systems. We conclude by presenting a schematic picture of protoplanetary disk evolution and dispersal, and discussing prospects for future work.Comment: 23 pages, 6 figures. Refereed review chapter, accepted for publication in Protostars & Planets VI, University of Arizona Press (2014), eds. H.Beuther, C.Dullemond, Th.Henning, R.Klesse

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Magnetospheres of hot Jupiters: hydrodynamic models and ultraviolet absorption

Cited by 39 publications

References 37 publications

An Observational Perspective of Transitional Disks

An Observational Perspective of Transitional Disks

Atmospheric Escape and the Evolution of Close-In Exoplanets

The Dispersal of Protoplanetary Disks

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