Triggered Star Formation inside the Shell of a Wolf-Rayet Bubble as the Origin of the Solar System

Dwarkadas, Vikram V.; Dauphas, N.; Meyer, B. S.; Boyajian, P. H.; Bojazi, M. J.

doi:10.1017/s1743921319002850

Cited by 9 publications

(15 citation statements)

References 121 publications

(268 reference statements)

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“…Finally, the environment may affect disc and planet properties through chemical enrichment. Recent work has highlighted that protoplanets may be heated by short-lived radionuclides (SLRs), which likely originate in mas-sive Wolf-Rayet stars and must be deposited quickly into nascent planetary systems due to their short half-lives 105 . This heating process sets the bulk water content and influences the formation of terrestrial planets 106 .…”

Section: Bimodal Exoplanet Propertiesmentioning

confidence: 99%

Stellar clustering shapes the architecture of planetary systems

Winter

Kruijssen

Longmore

et al. 2020

Nature

109

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Planet formation is generally described in terms of a system containing the host star and a protoplanetary disk 1 – 3 , of which the internal properties (for example, mass and metallicity) determine the properties of the resulting planetary system 4 . However, (proto)planetary systems are predicted 5 , 6 and observed 7 , 8 to be affected by the spatially clustered stellar formation environment, through either dynamical star–star interactions or external photoevaporation by nearby massive stars 9 . It is challenging to quantify how the architecture of planetary sysems is affected by these environmental processes, because stellar groups spatially disperse within less than a billion years 10 , well below the ages of most known exoplanets. Here we identify old, co-moving stellar groups around exoplanet host stars in the astrometric data from the Gaia satellite 11 , 12 and demonstrate that the architecture of planetary systems exhibits a strong dependence on local stellar clustering in position-velocity phase space. After controlling for host stellar age, mass, metallicity and distance from the star, we obtain highly significant differences (with p values of 10 −5 to 10 −2 ) in planetary system properties between phase space overdensities (composed of a greater number of co-moving stars than unstructured space) and the field. The median semi-major axis and orbital period of planets in phase space overdensities are 0.087 astronomical units and 9.6 days, respectively, compared to 0.81 astronomical units and 154 days, respectively, for planets around field stars. ‘Hot Jupiters’ (massive, short-period exoplanets) predominantly exist in stellar phase space overdensities, strongly suggesting that their extreme orbits originate from environmental perturbations rather than internal migration 13 , 14 or planet–planet scattering 15 , 16 . Our findings reveal that stellar clustering is a key factor setting the architectures of planetary systems.

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Section: Bimodal Exoplanet Propertiesmentioning

confidence: 99%

Stellar clustering shapes the architecture of planetary systems

Winter

Kruijssen

Longmore

et al. 2020

Nature

109

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“…Moreover, supernova sources would likely provide abundant 26 Al and 60 Fe, whereas the early solar system content of 60 Fe is equivalent to the measly ambient galactic supply (Trappitsch et al., 2018). More recent suggestions envisage stellar winds from a massive Wolf‐Rayet star injecting 26 Al to complement the local inventory of ambient galactic sources (Dwarkadas et al., 2017; Gounelle & Meynet, 2012; Young, 2014). At the same time, the enhanced abundance of 53 Mn and the presence of very short half‐life isotopes (e.g., 41 Ca t 1/2 =0.1 Ma) present challenges to be explained by models invoking Wolf‐Rayet stars (Vescovi et al., 2018).…”

Section: Radiogenic Heat and Geoneutrino Luminosity Of The Earthmentioning

confidence: 99%

Radiogenic Power and Geoneutrino Luminosity of the Earth and Other Terrestrial Bodies Through Time

McDonough

Šrámek

Wipperfurth

2020

Geochem Geophys Geosyst

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We report the Earth's rate of radiogenic heat production and (anti)neutrino luminosity from geologically relevant short‐lived radionuclides (SLR) and long‐lived radionuclides (LLR) using decay constants from the geological community, updated nuclear physics parameters, and calculations of the β spectra. We track the time evolution of the radiogenic power and luminosity of the Earth over the last 4.57 billion years, assuming an absolute abundance for the refractory elements in the silicate Earth and key volatile/refractory element ratios (e.g., Fe/Al, K/U, and Rb/Sr) to set the abundance levels for the moderately volatile elements. The relevant decays for the present‐day heat production in the Earth (19.9 ± 3.0 TW) are from 40K, 87Rb, 147Sm, 232Th, 235U, and 238U. Given element concentrations in kg‐element/kg‐rock and density ρ in kg/m3, a simplified equation to calculate the present‐day heat production in a rock is h[μW m−3]=ρ3.387×10−3K+0.01139Rb+0.04595Sm+26.18Th+98.29U The radiogenic heating rate of Earth‐like material at solar system formation was some 103 to 104 times greater than present‐day values, largely due to decay of 26Al in the silicate fraction, which was the dominant radiogenic heat source for the first ∼10 Ma. Assuming instantaneous Earth formation, the upper bound on radiogenic energy supplied by the most powerful short‐lived radionuclide 26Al (t1/2 = 0.7 Ma) is 5.5×1031 J, which is comparable (within a factor of a few) to the planet's gravitational binding energy.

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“…In addition to 26 Al, type II supernova is expected to produce shortlived radionuclide 60 Fe that decays to 60 Ni with half-life of 2.6 Ma. The recently estimated low initial abundance of 60 Fe in the SS (Tang and Dauphas 2012;Trappitsch et al 2018) precludes a supernova origin of 26 Al and favors injection of 26 Al by a stellar wind from a nearby Wolf-Rayet star (e.g., Gaidos et al 2009;Dwarkadas et al 2018).…”

Section: Internal 26 Al-26 Mg Isochronsmentioning

confidence: 99%

Refractory inclusions in carbonaceous chondrites: Records of early solar system processes

Krot

2019

Meteorit & Planetary Scien

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Chondrites consist of three major components: refractory inclusions (Ca,Al‐rich inclusions [CAIs] and amoeboid olivine aggregates), chondrules, and matrix. Here, I summarize recent results on the mineralogy, petrology, oxygen, and aluminum‐magnesium isotope systematics of the chondritic components (mainly CAIs in carbonaceous chondrites) and their significance for understanding processes in the protoplanetary disk (PPD) and on chondrite parent asteroids. CAIs are the oldest solids originated in the solar system: their U‐corrected Pb‐Pb absolute age of 4567.3 ± 0.16 Ma is considered to represent time 0 of its evolution. CAIs formed by evaporation, condensation, and aggregation in a gas of approximately solar composition in a hot (ambient temperature >1300 K) disk region exposed to irradiation by solar energetic particles, probably near the protoSun; subsequently, some CAIs were melted in and outside their formation region during transient heating events of still unknown nature. In unmetamorphosed, type 2–3.0 chondrites, CAIs show large variations in the initial 26Al/27Al ratios, from <5 × 10–6 to ~5.25 × 10–5. These variations and the inferred low initial abundance of 60Fe in the PPD suggest late injection of 26Al by a wind from a nearby Wolf–Rayet star into the protosolar molecular cloud core prior to or during its collapse. Although there are multiple generations of CAIs characterized by distinct mineralogies, textures, and isotopic (O, Mg, Ca, Ti, Mo, etc.) compositions, the 26Al heterogeneity in the CAI‐forming region(s) precludes determining the duration of CAIs formation using 26Al‐26Mg systematics. The existence of multiple generations of CAIs and the observed differences in CAI abundances in carbonaceous and noncarbonaceous chondrites may indicate that CAIs were episodically formed and ejected by a disk wind from near the Sun to the outer solar system and then spiraled inward due to gas drag. In type 2–3.0 chondrites, most CAIs surrounded by Wark–Lovering rims have uniform Δ17O (= δ17O−0.52 × δ18O) of ~ −24‰; however, there is a large range of Δ17O (from ~−40 to ~ −5‰) among them, suggesting the coexistence of 16O‐rich (low Δ17O) and 16O‐poor (high Δ17O) gaseous reservoirs at the earliest stages of the PPD evolution. The observed variations in Δ17O of CAIs may be explained if three major O‐bearing species in the solar system (CO, H2O, and silicate dust) had different O‐isotope compositions, with H2O and possibly silicate dust being 16O‐depleted relative to both the Genesis solar wind Δ17O of −28.4 ± 3.6‰ and even more 16O‐enriched CO. Oxygen isotopic compositions of CO and H2O could have resulted from CO self‐shielding in the protosolar molecular cloud (PMC) and the outer PPD. The nature of 16O‐depleted dust at the earliest stages of PPD evolution remains unclear: it could have either been inherited from the PMC or the initially 16O‐rich (solar‐like) MC dust experienced O‐isotope exchange during thermal processing in the PPD. To understand the chemical and isotopic composition of the protosolar MC...

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Triggered Star Formation inside the Shell of a Wolf-Rayet Bubble as the Origin of the Solar System

Cited by 9 publications

References 121 publications

Stellar clustering shapes the architecture of planetary systems

Stellar clustering shapes the architecture of planetary systems

Radiogenic Power and Geoneutrino Luminosity of the Earth and Other Terrestrial Bodies Through Time

Refractory inclusions in carbonaceous chondrites: Records of early solar system processes

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