TESS data show stochastic low-frequency variability dominates in most extreme helium stars, with characteristic timescales of 0.5-10 days correlating to stellar parameters and matching subsurface convection predictions.
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Binary population synthesis predicts several thousand intermediate-mass helium stars in the Milky Way, mostly in binaries, with metallicity and common-envelope ejection efficiency as the dominant shaping factors.
Simulations overpredict hot subdwarf and RR Lyrae binaries with Gaia astrometric solutions but match red clump stars with high mass functions as potential black hole impostors, implying fewer au-scale RR Lyrae binaries than expected.
A homogeneous search of TESS Cycle 7 20-second cadence light curves identifies 73 rapid oscillators (24 white dwarfs, 31 hot subdwarfs, 18 A-F stars) with measured frequencies and amplitudes after vetting.
citing papers explorer
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TESS Observations of Stochastic Low-frequency Variability in Extreme Helium Stars
TESS data show stochastic low-frequency variability dominates in most extreme helium stars, with characteristic timescales of 0.5-10 days correlating to stellar parameters and matching subsurface convection predictions.
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A Rare Population of Intermediate-mass Helium Stars Between Hot Subdwarfs and Wolf-Rayet Stars
Binary population synthesis predicts several thousand intermediate-mass helium stars in the Milky Way, mostly in binaries, with metallicity and common-envelope ejection efficiency as the dominant shaping factors.
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Testing models for fully and partially stripped low-mass stars with Gaia: Implications for hot subdwarfs, binary RR Lyrae, and black hole impostors
Simulations overpredict hot subdwarf and RR Lyrae binaries with Gaia astrometric solutions but match red clump stars with high mass functions as potential black hole impostors, implying fewer au-scale RR Lyrae binaries than expected.
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A Search for High Frequency Oscillations in TESS Cycle 7
A homogeneous search of TESS Cycle 7 20-second cadence light curves identifies 73 rapid oscillators (24 white dwarfs, 31 hot subdwarfs, 18 A-F stars) with measured frequencies and amplitudes after vetting.