Water formation in early solar nebula: I. Quasi-stationary cloud core

Tornow, Carmen; Gast, Philipp; Pelivan, Ivanka; Kupper, Stefan; Kührt, Ekkehard; Motschmann, U.

doi:10.1016/j.pss.2013.12.010

“…It is allowed to evolve for between 1 and 6 Myrs (Tornow et al 2014a). Both the gas phase 2 and grain 3 chemistry is followed.…”

Section: A Model Of the Deuteration Of Water In The Early Stages Of Tmentioning

confidence: 99%

The Composition of the Protosolar Disk and the Formation Conditions for Comets

Willacy¹,

Alexander²,

Ali-Dib³

et al. 2017

Comets as Tracers of Solar System Formation and Evolution

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Conditions in the protosolar nebula have left their mark in the composition of cometary volatiles, thought to be some of the most pristine material in the solar system. Cometary compositions represent the end point of processing that began in the parent molecular cloud core and continued through the collapse of that core to form the protosun and the solar nebula, and finally during the evolution of the solar nebula itself as the cometary bodies were accreting. Disentangling the effects of the various epochs on the final composition of a comet is complicated. But comets are not the only source of information about the solar nebula. Protostellar disks around young stars similar to the protosun provide a way of investigating the evolution of disks similar to the solar nebula while they are in the process of evolving to form their own solar systems. In this way we can learn about the physical and chemical conditions under which comets formed, and about the types of dynamical processing that shaped the solar system we see today.This paper summarizes some recent contributions to our understanding of both cometary volatiles and the composition, structure and evolution of protostellar disks.

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“…In these models the cloud core is initially described as a Bonner-Ebert sphere which is embedded in a constant density gas-shell wiht a visual extinction of up to 4 magnitudes (Wakelam et al 2014), and irradiated by an external UV field. It is allowed to evolve for between 1 and 6 Myrs (Tornow et al 2014a). Both the gas phase 2 and grain 3 chemistry is followed.…”

Section: A Model Of the Deuteration Of Water In The Early Stages Of Tmentioning

confidence: 99%

“…The cosmic ray ionization rate is taken to be 10 −17 s −1 . The related gas and grain chemistry is modeled using a combined code (Tornow et al 2014a).…”

Section: A Model Of the Deuteration Of Water In The Early Stages Of Tmentioning

confidence: 99%

The Composition of the Protosolar Disk and the Formation Conditions for Comets

Willacy

¹

,

Alexander

²

,

Ali-Dib

³

et al. 2015

Self Cite

View full text Add to dashboard Cite

Conditions in the protosolar nebula have left their mark in the composition of cometary volatiles, thought to be some of the most pristine material in the solar system. Cometary compositions represent the end point of processing that began in the parent molecular cloud core and continued through the collapse of that core to form the protosun and the solar nebula, and finally during the evolution of the solar nebula itself as the cometary bodies were accreting. Disentangling the effects of the various epochs on the final composition of a comet is complicated. But comets are not the only source of information about the solar nebula. Protostellar disks around young stars similar to the protosun provide a way of investigating the evolution of disks similar to the solar nebula while they are in the process of evolving to form their own solar systems. In this way we can learn about the physical and chemical conditions under which comets formed, and about the types of dynamical processing that shaped the solar system we see today.This paper summarizes some recent contributions to our understanding of both cometary volatiles and the composition, structure and evolution of protostellar disks.

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“…Equations (4) and (5) depend also on the dust density, ρ d , and are valid at each radial grid point of the core and the shell. The meaning of the various parameters in the balance equations, explained in Table 1, are explicitly given in Tornow et al (2014a). To calculate the difference Γ dust -Λ dust in Eq.…”

Section: Model Descriptionmentioning

confidence: 99%

“…In order to provide a relatively self-contained presentation of our SNmodel, in the next section we expound briefly the main aspects of the evolving cloud core without going into too much mathematical detail. These details are explained in Tornow et al (2014a) for the quasi-stationary core, while for the collapsing core, they can be found in Tornow et al (2014b). The third section presents and explains the simulated water abundances and deuterium fractionation.…”

Section: Introductionmentioning

confidence: 99%

Simulating the D/H ratio of water formed in the early solar nebula

Tornow

¹

,

Gast

²

,

Pelivan

³

et al. 2014

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assumption that starless cores can be in a collapsing prestellar or in an unbounded stage while protostellar cores contain relatively hot hydrostatic gas-dust spheresthe precursors of T-Tauri stars-and outflows (Belloche et al., 2011a, b). After a time between 10 5 and 10 6 years the gaseous envelope disappears and a T-Tauri star surrounded by a turbulent disk becomes observable. Our SN-model is based on these three stages of lowmass star formation (Fig. 1). Its early part simulates the starless stage as a quasi-stationary cloud core and the protostellar stage as a collapsing cloud core. The material in each stage consists of the gas phase with about 99% of the total core mass and the dust phase. Both phases interact with each other thermally and chemically. The energetic equilibrium of the first stage corresponds to a spherical core constructed by Bonnor (1956) and Ebert (1957). Since a number of these cores are characterized by oscillations (Keto et al., 2006), which are mathematically similar to stellar pulsations, relatively long lifetimes

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Water formation in early solar nebula: I. Quasi-stationary cloud core

Cited by 5 publications

References 103 publications

The Composition of the Protosolar Disk and the Formation Conditions for Comets

The Composition of the Protosolar Disk and the Formation Conditions for Comets

The Composition of the Protosolar Disk and the Formation Conditions for Comets

Simulating the D/H ratio of water formed in the early solar nebula

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