Chondrule formation during planetesimal accretion

Asphaug, Erik; Jutzi, Martin; Movshovitz, N.

doi:10.1016/j.epsl.2011.06.007

Cited by 138 publications

(160 citation statements)

References 65 publications

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“…This mechanism is not local since the shock waves induced by the companion star covers the whole disk, since the spiral wave extends from inside to the outer borders. As a consequence, it would not be necessary to invoke additional heating mechanisms or local shock fronts of different origins (Urey & Craig 1953;Urey 1967;Sanders & Taylor 2005;Asphaug et al 2011;Levy & Araki 1989;Joung et al 2004;Morfill et al 1993;Pilipp et al 1998;Desch & Cuzzi 2000;Nakamoto et al 2005;Boss & Graham 1993;Ruzmaikina & Ip 1994;Hood et al 2009;Hood 1998;Weidenschilling et al 1998;Ciesla et al 2004;Morris et al 2012;Wood 1996;Desch & Connolly 2002;Boss & Durisen 2005;Boley & Durisen 2008). In this picture, the strong shock waves generated by binary interaction during pericenter passages might be an additional and very efficient mechanism for chondrule formation over the whole disk.…”

Section: Temperature Profile: Chondrule Formation At Shocks?mentioning

confidence: 99%

Three-dimensional modeling of radiative disks in binaries

Picogna¹,

Marzari²

2013

A&A

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Context. Circumstellar disks in binaries are perturbed by the companion gravity causing significant alterations of the disk morphology. Spiral waves due to the companion tidal force also develop in the vertical direction and affect the disk temperature profile. These effects may significantly influence the process of planet formation. Aims. We perform 3D numerical simulations of disks in binaries with different initial dynamical configurations and physical parameters. Our goal is to investigate their evolution and their propensity to grow planets. Methods. We use an improved version of the SPH code VINE modified to better account for momentum and energy conservation via variable smoothing and softening length. The energy equation includes a flux-limited radiative transfer algorithm. The disk cooling is obtained with the use of "boundary particles" populating the outer surfaces of the disk and radiating to infinity. We model a system made of star/disk + star/disk where the secondary star (and relative disk) is less massive than the primary. Results. The numerical simulations performed for different values of binary separation and disk density show that trailing spiral shock waves develop when the stars approach their pericenter. Strong hydraulic jumps occur at the shock front, in particular for small separation binaries, creating breaking waves, and a consistent mass stream between the two disks. Both shock waves and mass transfer cause significant heating of the disk. At apocenter these perturbations are reduced and the disks are cooled down and less eccentric. Conclusions. The disk morphology is substantially affected by the companion perturbations, in particular in the vertical direction. The hydraulic jumps may slow down or even halt the dust coagulation process. The disk is significantly heated up by spiral waves and mass transfer, and the high gas temperature may prevent the ice condensation by moving the "snow line" outward. The disordered motion triggered by the spiral waves may, on the other hand, favor direct formation of large planetesimals from pebbles. The strength of the hydraulic jumps, disk heating, and mass exchange depends on the binary separation, and for larger semi-major axes, the tidal spiral pattern is substantially reduced. The environment then appears less hostile to planet formation.

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Section: Temperature Profile: Chondrule Formation At Shocks?mentioning

confidence: 99%

Three-dimensional modeling of radiative disks in binaries

Picogna¹,

Marzari²

2013

A&A

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“…Chondrules are mainly composed of olivine ((Fe,Mg) 2 SiO 4 ) and pyroxene ((Fe,Mg)SiO 3 ) minerals, which crystallised within minutes to days between 1800 and 1300 K (Scott 2007). Several heat sources have been proposed for the thermal processing of chondrule precursors, including shock waves (Boss and Graham 1993;Connolly and Love 1998;Hood 1998;Connolly et al 2006), current sheets (Joung et al 2004), x-winds (Shu et al 1997), magnetised disk wind (Salmeron and Ireland 2012), and colliding planetesimals (Asphaug et al 2011;Sanders and Scott 2012). A longstanding paradigm used to constrain chondrule-formation models is the so-called chemical complementarity that apparently exists between chondrules and matrix in individual chondrite groups (Hezel and Palme 2010;Palme et al 2015;Ebel et al 2016).…”

Section: Fig 62mentioning

confidence: 99%

“…Among the proposed mechanisms of chondrule formation are shock waves related to disk gravitational instability, eccentric planetesimals, and X-ray flares (Desch et al 2005;Morris et al 2012), magnetised turbulence in the disk (McNally et al 2013), collisions between chondritic or differentiated planetesimals (Asphaug et al 2011;Johnson et al 2015), and splashing of differentiated planetesimals (Asphaug et al 2011). Although none of the proposed mechanisms can be completely ruled out, the common presence of relict grains and Fe,Ni-metal in porphyritic chondrules as well as the large age range of chondrules from individual chondrites, including ages indistinguishable from CAIs (Connelly et al 2012;Bollard et al 2017), are inconsistent with formation of the majority of porphyritic chondrules by splashing of differentiated bodies.…”

Section: Multiplicity Of Chondrule-forming Mechanismsmentioning

confidence: 99%

Chondrules: Ubiquitous Chondritic Solids Tracking the Evolution of the Solar Protoplanetary Disk

Bizzarro

Connelly

Krot

2017

Formation, Evolution, and Dynamics of Young Solar Systems

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Chondrite meteorites are samples of primitive asteroidal bodies that have escaped melting and differentiation. The only record of our Solar System's formative stages comes from the earliest solids preserved in chondrites, namely millimetre-to centimetre-sized calcium-aluminium-rich inclusions (CAIs) and chondrules. These solids formed by transient heating events during the lifetime of the solar protoplanetary disk. Collectively, CAIs and chondrules provide timesequenced samples allowing us to probe the composition of the disk material that accreted to form planetesimals and planets. Here, we showcase the current stateof-the-art data with respect to the chronology and stable isotopic compositions of individual chondrules from various chondrite groups and discuss how these data can be used to provide novel insights into the thermal and chemical evolution of the solar protoplanetary disk, including mass transport processes.

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“…As an alternative, a model of impacts on planetesimals causing rapid melting and vaporization is gaining ground since this provides the very high density and highly volatile-enriched environments required to form chondrules (Asphaug et al, 2011;Alexander and Ebel, 2012;Sanders and Scott, 2012;Fedkin et al, 2012;Morris et al, 2012;Fedkin and Grossman, 2013;Johnson et al, 39 2015).…”

Section: Redox Conditions During Chondrule Formationmentioning

confidence: 99%

Relationships between type I and type II chondrules: Implications on chondrule formation processes

Villeneuve

Libourel

Soulié

2015

Geochimica et Cosmochimica Acta

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Please cite this article as: Villeneuve, J., Libourel, G., Soulié, C., Relationships between type I and type II chondrules: Implications on chondrule formation processes, Geochimica et Cosmochimica Acta (2015), doi: http://dx.doi.org/ 10.1016/j.gca. 2015.03.033 This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain.

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Chondrule formation during planetesimal accretion

Cited by 138 publications

References 65 publications

Three-dimensional modeling of radiative disks in binaries

Three-dimensional modeling of radiative disks in binaries

Chondrules: Ubiquitous Chondritic Solids Tracking the Evolution of the Solar Protoplanetary Disk

Relationships between type I and type II chondrules: Implications on chondrule formation processes

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