ANGULAR MOMENTUM TRANSPORT WITHIN EVOLVED LOW-MASS STARS

By Matteo Cantiello, C. Mankovich, L. Bildsten, J. Christensen-Dalsgaard, B. Paxton. 2014

168 citations recorded by the source corpus.

Asteroseismology of 1.0–2.0 M☉ red giants by the Kepler satellite has enabled the first definitive measurements of interior rotation in both first ascent red giant branch (RGB) stars and those on the helium burning clump. The inferred rotation rates are 10–30 days for the ≈0.2 M☉ He degenerate cores on the RGB and 30–100 days for the He burning core in a clump star. Using the Modules for Experiments in Stellar Evolution code, we calculate state-of-the-art stellar evolution models of low mass rotating stars from the zero-age main sequence to the cooling white dwarf (WD) stage. We include transport of angular momentum due to rotationally induced instabilities and circulations, as well as magnetic fields in radiative zones (generated by the Tayler–Spruit dynamo). We find that all models fail to predict core rotation as slow as observed on the RGB and during core He burning, implying that an unmodeled angular momentum transport process must be operating on the early RGB of low mass stars. Later evolution of the star from the He burning clump to the cooling WD phase appears to be at nearly constant core angular momentum. We also incorporate the adiabatic pulsation code, ADIPLS, to explicitly highlight this shortfall when applied to a specific Kepler asteroseismic target, KIC8366239.

View Paper: https://www.semanticscholar.org/paper/604677916558b8a9f5778719f9c74bf6a3429969

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Citations in the corpus

Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, result): “…we note that our main conclusion, which states that angular momentum transport needs to be more effective than predicted by shellular model for massive stars, lends support to a similar conclusion that was reached for low-mass stars based on Kepler asteroseismology data (Cantiello et al. 2014).”
Supernova simulations from a 3D progenitor model - Impact of perturbations and evolution of explosion properties (2017, background): “This is especially interesting considering that asteroseismic measurements of core rotation in evolved low-mass stars (Cantiello et al. 2014) suggest that current stellar evolution models still underestimate the efficiency of angular momentum transport in stellar interiors, which implies that…”
Most Black Holes Are Born Very Slowly Rotating (2019, result): “…2018), unambiguously demonstrating that the internal rotation rates of low-mass stars (and their white dwarf descendants) are slower than predicted by essentially all previous models (e.g., Meynet & Maeder 2005; Heger et al. 2005; Woosley & Heger 2006; Cantiello et al. 2014; Wheeler et al. 2015).”
The Status of Multi-Dimensional Core-Collapse Supernova Models (2016, background): “…(Heger et al. 2005) that include angular momentum transport by magnetic fields generated by the Tayler-Spruit dynamo (Spruit 2002), and asteroseismic measurements of core rotation in evolved low-mass stars suggest that the spin-down of the cores may be even more efficient (Cantiello et al. 2014).”
Gravitational wave signals from 3D neutrino hydrodynamics simulations of core-collapse supernovae (2016, result): “Furthermore, the angular momentum loss due to the stellar winds seems to be underestimated by the stellar evolution models, compared to results from asteroseismology (Cantiello et al. 2014).”
Mixed modes in red giants: a window on stellar evolution (2014, background): “…ΔΠ1 allows us to probe the core, to monitor its rotation (Beck et al. 2012; Mosser et al. 2012a; Deheuvels et al. 2012, 2014), and to investigate how angular Article published by EDP Sciences L5, page 1 of 5 momentum is transferred between the stellar core and the envelope (Cantiello et al. 2014).”
White Dwarf Rotation as a Function of Mass and a Dichotomy of Mode Line Widths: Kepler Observations of 27 Pulsating DA White Dwarfs through K2 Campaign 8 (2017, background): “Still, this is an order of magnitude slower than expected after accounting for all hypothesized angular momentum transport processes (e.g., Marques et al. 2013; Cantiello et al. 2014).”
The origin of spin in binary black holes (2019, background): “From observations of astro-seismology (Fuller et al. 2014; Cantiello et al. 2014), as well as neutron star and white dwarf spins (Heger et al. 2005; Suijs et al. 2008), it is known that this mechanism must be efficient (Spruit 1999, 2002; Fuller et al. 2019).”
Angular momentum transport by heat-driven g-modes in slowly pulsating B stars (2017, background): “It also remains possible that an as-yetunknown angular momentum transport process (as for example invoked by Cantiello et al. 2014, to explain the slow core rotation of red giant stars) may play a role in determining whether g modes can establish a differential rotation profile.”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “…1997; Heger et al. 2000; Maeder & Meynet 2000; Palacios et al. 2003; Talon & Charbonnel 2005; Denissenkov & Pinsonneault 2007; Hunter et al. 2007; Chieffi & Limongi 2013; Cantiello et al. 2014), but it remains as one of the most challenging and uncertain problems in stellar astrophysics.”
Slowing the spins of stellar cores (2019, background): “…2002) can provide more efficient AM transport than most other mechanisms, but prior implementations still predict spin rates roughly an order of magnitude too large because they struggle to overcome the steep composition gradient in red giants that suppress AM mixing (Cantiello et al. 2014).”