On Stellar Evolution in a Neutrino Hertzsprung–Russell Diagram

Farag, Ebraheem; Timmes, F. X.; Taylor, Morgan; Patton, Kelly M.; Farmer, Robert

doi:10.3847/1538-4357/ab7f2c

Cited by 22 publications

(25 citation statements)

References 137 publications

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“…Farag et al (2020, see their Tables 1 and 2) showed that, if the above three input and target quantities are used, then the optimized solutions using the MESA code are similar to those in Vinyoles et al (2017). We confirmed that, using these three target quantities, we could reproduce exactly the results of Farag et al (2020). However, we found that in some cases this can result in values of Y surf outside the range of observed values (see, e.g., Table 4 of Vinyoles et al 2017).…”

Section: Chi-squared Testssupporting

confidence: 72%

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Imprint of planet formation in the deep interior of the Sun

Kunitomo,

Guillot

2021

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In protoplanetary disks, the growth and inward drift of dust lead to the generation of a temporal "pebble wave" of increased metallicity. This phase must be followed by a phase in which the exhaustion of the pebbles in the disk and the formation of planets lead to the accretion of metal-poor gas. At the same time, disk winds may lead to the selective removal of hydrogen and helium from the disk. Hence, stars grow by accreting gas that has an evolving composition. In this work, we investigated how the formation of the Solar System may have affected the composition and structure of the Sun, and whether it plays any role in solving the so-called solar abundance problem, that is, the fact that standard models with up-to-date lower-metallicity abundances reproduce helioseismic constraints significantly more poorly than those with old higher-metallicity abundances. We simulated the evolution of the Sun from the protostellar phase to the present age and attempted to reproduce spectroscopic and helioseismic constraints. We performed chisquared tests to optimize our input parameters, which we extended by adding secondary parameters. These additional parameters accounted for the variations in the composition of the accreted material and an increase in the opacities. We confirmed that, for realistic models, planet formation occurs when the solar convective zone is still massive; thus, the overall changes due to planet formation are too small to significantly improve the chi-square fits. We found that solar models with up-to-date abundances require an opacity increase of 12% to 18% centered at T = 10 6.4 K to reproduce the available observational constraints. This is slightly higher than, but is qualitatively in good agreement with, recent measurements of higher iron opacities. These models result in better fits to the observations than those using old abundances; therefore, they are a promising solution to the solar abundance problem. Using these improved models, we found that planet formation processes leave a small imprint in the solar core, whose metallicity is enhanced by up to 5%. This result can be tested by accurately measuring the solar neutrino flux. In the improved models, the protosolar molecular cloud core is characterized by a primordial metallicity in the range Z proto = 0.0127-0.0157 and a helium mass fraction in the range Y proto = 0.268-0.274.

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Section: Chi-squared Testssupporting

confidence: 72%

“…In the csv file, we list the values of M XY,lost [M ], assuming M Z,planet = 150 M ⊕ , and M Z,planet [M ⊕ ], assuming M XY,lost = 0, for the models with planet formation. Neutrino fluxes, calculated using the subroutine provided in Farag et al (2020), are also included in the csv file.…”

Section: Appendix A: Details Of Simulation Resultsmentioning

confidence: 99%

Imprint of planet formation in the deep interior of the Sun

Kunitomo,

Guillot

2021

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“…We take the NFW profile. ii ) The ν flux varies with the type and age of stars [27]. iii ) The star distribution in the Milky Way.…”

Section: < L a T E X I T S H A 1 _ B A S E 6 4 = " N P / R V H H E J ...mentioning

confidence: 99%

Cosmic-Neutrino-Boosted Dark Matter ($ν$BDM)

Jho¹,

Park²,

Park³

et al. 2021

Preprint

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A novel mechanism of boosting dark matter by cosmic neutrinos is proposed. The new mechanism is so significant that the arriving flux of dark matter in the mass window 1 keV mDM 1 MeV on Earth can be enhanced by two to four orders of magnitude compared to one only by cosmic electrons. Thereby we firstly derive conservative but still stringent bounds and future sensitivity limits for such cosmic-neutrino-boosted dark matter (νBDM) from advanced underground experiments such as Borexino, PandaX, XENON1T, and JUNO.

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“…The abundance of 22 Ne when He-burning is completed is thus proportional to the initial CNO abundance of the progenitor main-sequence star. The weak reaction in this sequence powers the neutrino luminosity during He-burning (e.g., Serenelli & Fukugita 2005;Farag et al 2020) and marks the first time in a star's life that the core becomes neutron rich. For zero-age main sequence (ZAMS) masses between ;0.5 M e (Demarque & Mengel 1971;Prada Moroni & Straniero 2009;Gautschy 2012) and ;7 M e (Becker & Iben 1979, 1980García-Berro et al 1997), depending on the treatment of convective boundary mixing (Weidemann 2000;Denissenkov et al 2013;Jones et al 2013;Farmer et al 2015; Lecoanet et al 2016;Constantino et al 2015Constantino et al , 2016Constantino et al , 2017, the 14 N(α,γ) 18 F(,e + ν e ) 18 O(α,γ) 22 Ne reaction sequence determines the 22 Ne content of a resulting carbon-oxygen white dwarf (CO WD).…”

Section: Introductionmentioning

confidence: 99%

On the Impact of ²²Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres

Chidester

Timmes

Schwab

et al. 2021

ApJ

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We explore changes in the adiabatic low-order g-mode pulsation periods of 0.526, 0.560, and 0.729 M ⊙ carbon–oxygen white dwarf models with helium-dominated envelopes due to the presence, absence, and enhancement of 22Ne in the interior. The observed g-mode pulsation periods of such white dwarfs are typically given to 6−7 significant figures of precision. Usually white dwarf models without 22Ne are fit to the observed periods and other properties. The rms residuals to the ≃150−400 s low-order g-mode periods are typically in the range of σ rms ≲ 0.3 s, for a fit precision of σ rms/P ≲ 0.3%. We find average relative period shifts of ΔP/P ≃ ±0.5% for the low-order dipole and quadrupole g-mode pulsations within the observed effective temperature window, with the range of ΔP/P depending on the specific g-mode, abundance of 22Ne, effective temperature, and the mass of the white dwarf model. This finding suggests a systematic offset may be present in the fitting process of specific white dwarfs when 22Ne is absent. As part of the fitting processes involves adjusting the composition profiles of a white dwarf model, our study on the impact of 22Ne can provide new inferences on the derived interior mass fraction profiles. We encourage routinely including 22Ne mass fraction profiles, informed by stellar evolution models, to future generations of white dwarf model-fitting processes.

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On Stellar Evolution in a Neutrino Hertzsprung–Russell Diagram

Cited by 22 publications

References 137 publications

Imprint of planet formation in the deep interior of the Sun

Imprint of planet formation in the deep interior of the Sun

Cosmic-Neutrino-Boosted Dark Matter ($ν$BDM)

On the Impact of ²²Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres

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On Stellar Evolution in a Neutrino Hertzsprung–Russell Diagram

Cited by 22 publications

References 137 publications

Imprint of planet formation in the deep interior of the Sun

Imprint of planet formation in the deep interior of the Sun

Cosmic-Neutrino-Boosted Dark Matter ($ν$BDM)

On the Impact of 22Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres

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Product

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On the Impact of ²²Ne on the Pulsation Periods of Carbon–Oxygen White Dwarfs with Helium-dominated Atmospheres