Publications
Check out my five most recent publications
- Van Beeck J., Van Hoolst T., Aerts C., Fuller J., Non-linear three-mode coupling of gravity modes in rotating slowly pulsating B stars. Stationary solutions and modeling potential, July 2024, A&A, 687, A265 (Nr. of citations: 5)
DOI: 10.1051/0004-6361/202348369, NASA ADS: 2024A&A…687A.265V, arXiv: 2311.02972
- Fritzewski D. J., Van Reeth T., Aerts C., Van Beeck J., Gossage S., Li G., Age-dating the young open cluster UBC 1 with g-mode asteroseismology, gyrochronology, and isochrone fitting, January 2024, A&A, 681, A13 (Nr. of citations: 8)
DOI: 10.1051/0004-6361/202347618, NASA ADS: 2024A&A…681A..13F, arXiv: 2310.18426
- Van Reeth T., Johnston C., Southworth J., Fuller J., Bowman D. M., Poniatowski L., Van Beeck J., Tidally perturbed gravity-mode pulsations in a sample of close eclipsing binaries, March 2023, A&A, 671, A121 (Nr. of citations: 7)
DOI: 10.1051/0004-6361/202245460, NASA ADS: 2023A&A…671A.121V, arXiv: 2301.08816
- Van Reeth T., De Cat P., Van Beeck J., et al., The near-core rotation of HD 112429. A γ Doradus star with TESS photometry and legacy spectroscopy, June 2022, A&A, 662, A58 (Nr. of citations: 6)
DOI: 10.1051/0004-6361/202142921, NASA ADS: 2022A&A…662A..58V, arXiv: 2203.11071
- Van Reeth T., Southworth J., Van Beeck J., Bowman D. M., V456 Cyg: An eclipsing binary with tidally perturbed g-mode pulsations, March 2022, A&A, 659, A177 (Nr. of citations: 10)
DOI: 10.1051/0004-6361/202142833, NASA ADS: 2022A&A…659A.177V, arXiv: 2201.05359
(Last update: 21 October 2024)
Check out my key works (view the full publication list in my ADS library)
Results from five iterative pre-whitening strategies
Example of a photometric light curve of a slowly pulsating B star, as measured by the NASA Kepler space telescope.
Variable stars exhibit (periodic) variations in their brightness, which can be tracked with long-term observations by telescopes (photometry), resulting in so-called photometric light curves. Harmonic analysis of these light curves is an established technique to retrieve the variable star’s (intrinsic) oscillation mode frequencies. To characterize the energy exchange among these oscillation modes, which is important in unraveling the internal structure and the intrinsically linked evolution of stars, one should however also characterize their amplitudes (and phases).
In this work we created a framework that uses 5 different strategies to perform harmonic analysis, in order to track any systematics that occur when using a single (specific) strategy. Combining the outcomes of the different analyses led to a robust list of amplitudes, frequencies and phases of stellar oscillation modes for a sample of slowly pulsating B (SPB) stars. Within that list several resonant triads were identified, which indicates that SPB stars are inherently non-linear oscillators (see Van Beeck et al. 2024 for additional information).
J Van Beeck, D.M. Bowman, M.G. Pedersen, T. Van Reeth, T. Van Hoolst, C. Aerts
A&A Vol. 655, A59 (November 2021)
You may also want to check out the NTSA computational framework, which was used in this work. A succinct description of its capabilities is discussed on this page.
Stationary solutions and modeling potential
Schematic overview of triads of interacting oscillation modes. Orange circles indicate oscillation modes that naturally occur (i.e., are linearly driven) within the star (model). Purple squares indicate oscillation modes that would not be sustained (i.e., linearly damped) within the star without non-linear energy exchange among the modes in the triad.
Asteroseismology, the study of stellar oscillation modes to improve our understanding of stellar evolution and structure, commonly relies on the measurement of precise oscillation mode frequencies. These frequencies are typically obtained by applying harmonic analysis techniques to observed photometric light curves, which are for example observed by space telescopes such as the NASA Kepler space telescope. Such harmonic analyses not only characterize parameters additional to the mode frequency (i.e., the mode amplitude and phase) but in some cases distinct signs of non-linear energy exchange among oscillations can also be detected based on their parameter values (see e.g., Van Beeck et al. 2021).
In this work we therefore developed a theoretical and computational framework that simulates the (non-linear) energy exchange among three modes that (resonantly) interact (i.e., resonant triads). We found that utilizing oscillation mode amplitude ratio information (of modes in resonant triads) may offer additional constraints when modeling stellar interiors.
J. Van Beeck, T. Van Hoolst, C. Aerts, J. Fuller
A&A Vol. 687, A265 (July 2024)
You may also want to check out the AESolver computational framework, which was used in this work. A succinct description of its capabilities is discussed on this page.