TY - JOUR
T1 - On Trapped Modes in Variable White Dwarfs as Probes of the 12C(α, γ)16O Reaction Rate
AU - Chidester, Morgan T.
AU - Farag, Ebraheem
AU - Timmes, F. X.
N1 - Funding Information:
We thank James Deboer for sharing the C probability distribution function, Josiah Schwab for sharing wd _ builder , and Pablo Marchant for sharing mkipp . This research is supported by NASA under the Astrophysics Theory Program grant NNH21ZDA001N-ATP, by the NSF under grant PHY-1430152 for the “Joint Institute for Nuclear Astrophysics—Center for the Evolution of the Elements,” and by the NSF under the Software Infrastructure for Sustained Innovation grants ACI-1663684, ACI-1663688, and ACI-1663696 for the MESA Project. This research made extensive use of the SAO/NASA Astrophysics Data System (ADS). 12
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/8/1
Y1 - 2022/8/1
N2 - We seek signatures of the current experimental 12C α , γ 16 O reaction rate probability distribution function in the pulsation periods of carbon-oxygen white dwarf (WD) models. We find that adiabatic g-modes trapped by the interior carbon-rich layer offer potentially useful signatures of this reaction rate probability distribution function. Probing the carbon-rich region is relevant because it forms during the evolution of low-mass stars under radiative helium-burning conditions, mitigating the impact of convective mixing processes. We make direct quantitative connections between the pulsation periods of the identified trapped g-modes in variable WD models and the current experimental 12C α , γ 16 O reaction rate probability distribution function. We find an average spread in relative period shifts of ΔP/P ≃ ±2% for the identified trapped g-modes over the ±3σ uncertainty in the 12C α , γ 16 O reaction rate probability distribution function—across the effective temperature range of observed DAV and DBV WDs and for different WD masses, helium shell masses, and hydrogen shell masses. The g-mode pulsation periods of observed WDs are typically given to six to seven significant figures of precision. This suggests that an astrophysical constraint on the 12C α , γ 16 O reaction rate could, in principle, be extractable from the period spectrum of observed variable WDs.
AB - We seek signatures of the current experimental 12C α , γ 16 O reaction rate probability distribution function in the pulsation periods of carbon-oxygen white dwarf (WD) models. We find that adiabatic g-modes trapped by the interior carbon-rich layer offer potentially useful signatures of this reaction rate probability distribution function. Probing the carbon-rich region is relevant because it forms during the evolution of low-mass stars under radiative helium-burning conditions, mitigating the impact of convective mixing processes. We make direct quantitative connections between the pulsation periods of the identified trapped g-modes in variable WD models and the current experimental 12C α , γ 16 O reaction rate probability distribution function. We find an average spread in relative period shifts of ΔP/P ≃ ±2% for the identified trapped g-modes over the ±3σ uncertainty in the 12C α , γ 16 O reaction rate probability distribution function—across the effective temperature range of observed DAV and DBV WDs and for different WD masses, helium shell masses, and hydrogen shell masses. The g-mode pulsation periods of observed WDs are typically given to six to seven significant figures of precision. This suggests that an astrophysical constraint on the 12C α , γ 16 O reaction rate could, in principle, be extractable from the period spectrum of observed variable WDs.
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U2 - 10.3847/1538-4357/ac7ec3
DO - 10.3847/1538-4357/ac7ec3
M3 - Article
AN - SCOPUS:85136130649
SN - 0004-637X
VL - 935
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 21
ER -