The Eroding Disk of AU Mic

Grady, C. A.; Wisniewski, John P.; Schneider, Glenn; Boccaletti, A.; Gáspár, András; Debes, John H.; Hines, Dean C.; Stark, Christopher C.; Thalmann, Christian; Lagrange, Anne-Marie; Augereau, J.-C.; Sezestre, Élie; Milli, J.; Henning, Thomas; Kuchner, Marc J.

doi:10.3847/2041-8213/ab65bb

Cited by 18 publications

(12 citation statements)

References 27 publications

(52 reference statements)

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“…Sample return from Mars is a long-term goal of the planetary science community (Muirhead et al, 2020), and the first concrete step will be taken with sample caching by the Perseverance (Mars 2020) mission to Jezero Crater (Grady et al, 2020). Although the goals of the mission are to search for evidence of past life in the sedimentary deposits around the landing site, any returned samples would ultimately provide counterparts to the Martian meteorites (SNCs) and/or indirect evidence for or constraints on any past magma ocean (e.g., the composition of the mantle).…”

Section: Future Solar System Missionsmentioning

confidence: 99%

Lava Worlds: From Early Earth to Exoplanets

Chao,

deGraffenried,

Lach

et al. 2020

Preprint

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The magma ocean concept was first conceived to explain the geology of the Moon, but hemispherical or global oceans of silicate melt could be a widespread "lava world" phase of rocky planet accretion, and could persist on planets on short-period orbits around other stars. The formation and crystallization of magma oceans could be a defining stage in the assembly of a core, origin of a crust, initiation of tectonics, and formation of an atmosphere. The last decade has seen significant advances in our understanding of this phenomenon through analysis of terrestrial and extraterrestrial samples, planetary missions, and astronomical observations of exoplanets. This review describes the energetic basis of magma oceans and lava worlds and the lava lake analogs available for study on Earth and Io. It provides an overview of evidence for magma oceans throughout the Solar System and considers the factors that control the rocks these magma oceans leave behind. It describes research on theoretical and observed exoplanets that could host extant magma oceans and summarizes efforts to detect and characterize them. It reviews modeling of the evolution of magma oceans as a result of crystallization and evaporation, the interaction with the underlying solid mantle, and the effects of planetary rotation. The review also considers theoretical investigations on the formation of an atmosphere in concert with the magma ocean and in response to irradiation from the host star, and possible end-states. Finally, it describes needs and gaps in our knowledge and points to future opportunities with new planetary missions and space telescopes to identify and better characterize lava worlds around nearby stars.

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Section: Future Solar System Missionsmentioning

confidence: 99%

Lava Worlds: From Early Earth to Exoplanets

Chao,

deGraffenried,

Lach

et al. 2020

Preprint

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“…Due to its proximity (d = 9.72 ± 0.04 pc, Gaia Collaboration et al 2018), the circumstellar environment of AU Mic can be spatially resolved with various high-contrast imaging methods. These observations reveal an edge-on debris disk (Kalas et al 2004;Strubbe & Chiang 2006;Grady et al 2020) with a complex and dynamic clump structure (Boccaletti et al 2015(Boccaletti et al , 2018. The transiting planet, AU Mic b, was reported by Plavchan et al (2020).…”

Section: Introductionmentioning

confidence: 55%

Magnetic Field of the Active Planet-hosting M Dwarf AU Mic

Kochukhov,

Reiners

2020

Preprint

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AU Mic is a young, very active M dwarf star with a debris disk and at least one transiting Neptune-size planet. Here we present detailed analysis of the magnetic field of AU Mic based on previously unpublished high-resolution optical and near-infrared spectropolarimetric observations. We report a systematic detection of circular and linear polarization signatures in the stellar photospheric lines. Tentative Zeeman Doppler imaging modeling of the former data suggests a non-axisymmetric global field with a surface-averaged strength of about 90 G. At the same time, linear polarization observations indicate the presence of a much stronger ≈ 2 kG axisymmetric dipolar field, which contributes no circular polarization signal due to the equator-on orientation of AU Mic. A separate Zeeman broadening and intensification analysis allowed us to determine a mean field modulus of 2.3 and 2.1 kG from the Y-and K-band atomic lines respectively. These magnetic field measurements are essential for understanding environmental conditions within the AU Mic planetary system.

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“…For example, Strubbe & Chiang (2006) devise a 'birth ring' model for AU Mic where a parent population of planetesimals at 43 au produces micrometer size dust grains that are then transported inwards by stellar wind drag and Poynting-Robertson drag, and outwards by radiation pressure and stellar wind ram pressure. Boccaletti et al (2015Boccaletti et al ( , 2018; Grady et al (2020) observe fast moving dust features in scattered light travelling outwards along the disc, possibly dust 'avalanches' originating from the point of intersection of the birth ring and a second, inclined ring leftover from the catastrophic disruption of a large planetesimal (Chiang & Fung 2017) or material released from a parent body on a Keplerian orbit closer to the star (Sezestre et al 2017). Daley et al (2019) were able to estimate the sizes and masses of bodies within the disc through resolving its vertical structure.…”

Section: Introductionmentioning

confidence: 99%

ALMA's view of the M-dwarf GSC 07396-00759's edge-on debris disc: AU Mic's coeval twin

Cronin-Coltsmann,

Kennedy,

Adam

et al. 2022

Preprint

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We present new ALMA Band 7 observations of the edge-on debris disc around the M1V star GSC 07396-00759. At ∼ 20 Myr old and in the 𝛽 Pictoris Moving Group along with AU Mic, GSC 07396-00759 joins it in the handful of low mass M-dwarf discs to be resolved in the sub-mm. With previous VLT/SPHERE scattered light observations we present a multi-wavelength view of the dust distribution within the system under the effects of stellar wind forces. We find the mm dust grains to be well described by a Gaussian torus at 70 au with a FWHM of 48 au and we do not detect the presence of CO in the system. Our ALMA model radius is significantly smaller than the radius derived from polarimetric scattered light observations, implying complex behaviour in the scattering phase function. The brightness asymmetry in the disc observed in scattered light is not recovered in the ALMA observations, implying that the physical mechanism only affects smaller grain sizes. High resolution follow-up observations of the system would allow investigation into its unique dust features as well as provide a true coeval comparison for its smaller sibling AU Mic, singularly well observed amongst M-dwarfs systems.

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The Eroding Disk of AU Mic

Cited by 18 publications

References 27 publications

Lava Worlds: From Early Earth to Exoplanets

Lava Worlds: From Early Earth to Exoplanets

Magnetic Field of the Active Planet-hosting M Dwarf AU Mic

ALMA's view of the M-dwarf GSC 07396-00759's edge-on debris disc: AU Mic's coeval twin

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