The possibility of forming an inhomogeneous Sun and the solar neutrino effect

Levy, E. H.; Ruzmaǐkina, T. V.

doi:10.1086/174539

Cited by 6 publications

(3 citation statements)

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“…The implication is that the radiative interior of the Sun might have a metallicity slightly lower than the photosphere. A number of authors (Joss 1974 ;Christensen-Dalsgaard et al 1979 ;Levy & Ruzmaikina 1994 ;Je †ery, Bailey, & Chambers 1997) suggested this possibility two decades ago as a way out of the solar neutrino problem ; lowering the metallicity of the solar interior reduces the radiative gradient, which, in turn, would lower the inferred temperature in the core. Finally, a lower core temperature would predict that fewer neutrinos would be emitted compared with that of the standard solar model.…”

Section: Solar Pollutionmentioning

confidence: 99%

Stellar Pollution in the Solar Neighborhood

Murray

Chaboyer

Arras

et al. 2001

ApJ

106

127

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We study spectroscopically determined iron abundances of 640 solar-type stars to search for the signature of accreted iron-rich material. We Ðnd that the metallicity [Fe/H] of a subset of 466 main-sequence stars, when plotted as a function of stellar mass, mimics the pattern seen in lithium abundances in open clusters. Using Monte Carlo models, we Ðnd that, on average, these stars appear to have accreted D0.5 of iron while on the main-sequence. A consistency check is provided by a much smaller sample of M1 9 stars in the Hertzsprung gap, which are slightly evolved and the convection zones of which are signiÐ-cantly more massive ; they have lower average [Fe/H], and their metallicity shows no clear variation with stellar mass. We argue that our Sun is likely to have accreted a similar amount of iron ; in this respect, most systems resemble ours rather than the currently known extrasolar planetary systems. These Ðndings suggest that terrestrial-type material is common around solar-type stars.

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Section: Solar Pollutionmentioning

confidence: 99%

Stellar Pollution in the Solar Neighborhood

Murray

Chaboyer

Arras

et al. 2001

ApJ

106

127

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“…This has important implications for the interpretation of solar abundances, since the outer layers of the sun must have been contaminated by the accretion of a large mass of comets or planetesimals during the early evolution of the solar system, leading to systematic differences between the composition of the solar core and its convective envelope. As discussed by Joss (1974), and more recently by Levy & Ruzmaikina (1994), h c emically inhomogeneous solar models provide a possible solution to the solar neutrino problem, while the accretion of comets and planetesimals (e.g. during and after the late heavy bombardment of the inner planets) due to the evolution of objects on to sun-colliding orbits provides a mechanism to contaminate the outer envelope.…”

Section: Dynamicsmentioning

confidence: 98%

The provenance and evolution of comets

Bailey

1996

Earth Moon Planet

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The process of comet formation through the hierarchical aggregation of originally submicron-sized interstellar grains to form micron-sized particles and then larger bodies in the protoplanetary disc, culminating in the formation of planetesimals in the disc extending from Jupiter to beyond Neptune, is briefly reviewed. The 'planetesimal' theory for the origin of comets implies the existence of distinct cometary reservoirs, with implications for the immediate provenance of observed comets (both long-period and shortperiod) and their evolution as a result of planetary perturbations and physicd decay, for example splitting and sublimation. The principal mode of cometary decay and collisional interaction with the terrestrial planets is through the formation and evolution of streams of cometary debris and hitherto undiscovered 'families' of cometary asteroids. Recent dynamical results, in particular the sungrazing and sun-colliding end-state for short-period comet and asteroid orbits, are briefly discussed.

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“…Joss (1974) suggested that stellar surfaces may be continuously enriched with heavy elements by infalling comets. Levy & Ruzmaikina (1994) investigated the effects of dust-gas separation during the star formation Send offprint requests to: J. Y. Yang process. As they pointed out, dust grains that aggregate by turbulence to large sizes will settle from the upper layers toward the center of the molecular cloud and merge into the proto-planetary nebula disk, and finally fall onto the star by means of disk accretion.…”

Section: Introductionmentioning

confidence: 99%

Solar model: Element diffusion or metal-enhanced envelope?

Yang

2001

A&A

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Abstract. Solar models with moderate enrichment of heavy elements in the convective envelope (CSM) and with element diffusion (DSM) are investigated using updated input physics. It is found that both CSM and DSM can result in adequate depth of the convection zone and appropriate surface helium abundance, and the agreement between the calculated and observed p-mode frequencies are also improved. The sound speed of DSM is better than CSM and the standard solar model (SSM) in the deep interior, which means that element diffusion helps improve the sound speed profile in the solar interior. In the area just below the base of the convection zone, CSM is the best of the three models.

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The possibility of forming an inhomogeneous Sun and the solar neutrino effect

Cited by 6 publications

References 0 publications

Stellar Pollution in the Solar Neighborhood

Stellar Pollution in the Solar Neighborhood

The provenance and evolution of comets

Solar model: Element diffusion or metal-enhanced envelope?

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