The impact of pre-main sequence stellar evolution on mid-plane snowline locations and C/O in planet forming discs

Miley, James; Panić, Olja; Booth, Richard A; Ilee, John D.; Ida, Shigeru; Kunitomo, Masanobu

doi:10.1093/mnras/staa3517

Cited by 14 publications

(12 citation statements)

References 99 publications

(133 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It is generally expected that the C/O ratios of exoplanetary atmospheres are linked to the compositions of protoplanetary disks (e.g., Öberg et al 2011;Madhusudhan et al 2014;Mordasini et al 2016;Booth et al 2017;Cridland et al 2020;Notsu et al 2020;Miley et al 2021). In shadowed disks, the solid C/O ratio reaches the solar value in shadowed regions, similar to the outer disk (Fig.…”

Section: Diagnostic Ratios For Exoplanet Observationsmentioning

confidence: 95%

Jupiter’s “cold” formation in the protosolar disk shadow

Ohno

Ueda

2021

A&A

View full text Add to dashboard Cite

Context. Atmospheric compositions offer valuable clues to planetary formation and evolution. Jupiter has been the most well-studied giant planet in terms of its atmosphere; however, the origin of the Jovian atmospheric composition remains a puzzle as the abundances of nitrogen and noble gases as high as those of other elements could only originate from extremely cold environments. Aims. We propose a novel idea for explaining the Jovian atmospheric composition: dust pileup at the H2O snow line casts a shadow and cools the Jupiter orbit so that N2 and noble gases can freeze. Planetesimals or a core formed in the shadowed region can enrich nitrogen and noble gases as much as other elements through their dissolution in the envelope. Methods. We compute the temperature structure of a shadowed protosolar disk with radiative transfer calculations. Then, we investigate the radial volatile distributions and predict the atmospheric composition of Jupiter with condensation calculations. Results. We find that the vicinity of the current Jupiter orbit, approximately 3 − 7 AU, could be as cold as ≲30 K if the small-dust surface density varies by a factor of ≳30 across the H2O snow line. According to previous grain growth simulations, this condition could be achieved by weak disk turbulence if silicate grains are more fragile than icy grains. The shadow can cause the condensation of most volatile substances, namely N2 and Ar. We demonstrate that the dissolution of shadowed solids can explain the elemental abundance patterns of the Jovian atmosphere even if proto-Jupiter was formed near Jupiter’s current orbit. Conclusions. The disk shadow may play a vital role in controlling atmospheric compositions. The effect of the shadow also impacts the interpretation of upcoming observations of exoplanetary atmospheres by JWST.

show abstract

Section: Diagnostic Ratios For Exoplanet Observationsmentioning

confidence: 95%

Jupiter’s “cold” formation in the protosolar disk shadow

Ohno

Ueda

2021

A&A

View full text Add to dashboard Cite

show abstract

“…Radial velocity surveys have revealed that the occurrence rate of detected giant planets depends upon M (e.g., Johnson et al 2010;Reffert et al 2015). The mass fraction and/or composition of planet atmospheres can give an indication as to when or where the planet was formed in a disk (Guillot & Hueso 2006;Ogihara et al 2020;Miley et al 2021). We expect that our disk evolution models also lead to the understanding of planet formation processes around IM stars.…”

Section: Implications For Planet Formationmentioning

confidence: 87%

Photoevaporative Dispersal of Protoplanetary Disks around Evolving Intermediate-mass Stars

Kunitomo,

Ida,

Takeuchi

et al. 2021

Preprint

Self Cite

View full text Add to dashboard Cite

We aim to understand the effect of stellar evolution on the evolution of protoplanetary disks. We focus in particular on the disk evolution around intermediate-mass (IM) stars, which evolve more rapidly than low-mass ones. We numerically solve the long-term evolution of disks around 0.5-5 M stars considering viscous accretion and photoevaporation (PE) driven by stellar far-ultraviolet (FUV), extreme-ultraviolet (EUV), and X-ray emission. We also take stellar evolution into account and consider the time evolution of the PE rate. We find that the FUV, EUV, and X-ray luminosities of IM stars evolve by orders of magnitude within a few Myr along with the time evolution of stellar structure, stellar effective temperature, or accretion rate. Therefore, the PE rate also evolves with time by orders of magnitude, and we conclude that stellar evolution is crucial for the disk evolution around IM stars.

show abstract

“…as illustrated in a single value of the external UV field in Walsh et al 2013). The idea that planetary composition could link to formation locations in the disc through snow lines (Öberg et al 2011) 2020) and the time evolution of the host star luminosity (Miley et al 2021). External irradiation adds yet another factor.…”

Section: Comments On the Effect Of External Irradiation Upon Snow Linesmentioning

confidence: 99%

“…Here we do not study the time evolution of snow lines like e.g. Booth & Ilee (2019) and Miley et al (2021), but in Figure 8 we show the radius in a 100 au, 10 M ⊕ disc around a 1 M star at which the temperature drops below certain values as a function of distance from the external radiation source. The rightmost set of points represent the thermal structure of an isolated disc (placed at 100 pc in Figure 8).…”

Section: Comments On the Effect Of External Irradiation Upon Snow Linesmentioning

confidence: 99%

Warm millimetre dust in protoplanetary discs near massive stars

Haworth

2021

Preprint

View full text Add to dashboard Cite

Dust plays a key role in the formation of planets and its emission also provides one of our most accessible views of protoplanetary discs. If set by radiative equilibrium with the central star, the temperature of dust in the disc plateaus at around 10 − 20 K in the outer regions. However sufficiently nearby massive stars can heat the outer disc to substantially higher temperatures.In this paper we study the radiative equilibrium temperature of discs in the presence of massive external sources and gauge the effect that it has on millimetre dust mass estimates. Since millimetre grains are not entrained in any wind we focus on geometrically simple 2Daxisymmetric disc models using radiative transfer calculations with both the host star and an external source. Recent surveys have searched for evidence of massive stars influencing disc evolution using disc properties as a function of projected separation. In assuming a disc temperature of 20 K for a disc a distance 𝐷 from a strong radiation source, disc masses are overestimated by a factor that scales with 𝐷 −1/2 interior to the separation that external heating becomes important. This could significantly alter dust mass estimates of discs in close proximity to 𝜃 1 C in the Orion Nebular Cluster. We also make an initial assessment of the effect upon snow lines. Within a parsec of an O star like 𝜃 1 C a CO snow line no longer exists, though the water snow line is virtually unaffected except for very close separations of ≤ 0.01 pc.

show abstract

The impact of pre-main sequence stellar evolution on mid-plane snowline locations and C/O in planet forming discs

Cited by 14 publications

References 99 publications

Jupiter’s “cold” formation in the protosolar disk shadow

Jupiter’s “cold” formation in the protosolar disk shadow

Photoevaporative Dispersal of Protoplanetary Disks around Evolving Intermediate-mass Stars

Warm millimetre dust in protoplanetary discs near massive stars

Contact Info

Product

Resources

About