The White Dwarf Mass versus X-Ray Temperature Relationship of Dwarf Novae, Revisited
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2022-03
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Mukai, Koji and Kristiina Byckling. The White Dwarf Mass versus X-Ray Temperature Relationship of Dwarf Novae, Revisited. Research Notes of the AAS 6 (Mar. 2022), no. 3. https://doi.org/10.3847/2515-5172/ac618b.
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Attribution 4.0 International (CC BY 4.0)
Attribution 4.0 International (CC BY 4.0)
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Abstract
While Keplerian orbits account for the majority of the astrometric motion of directly-imaged planets, perturbations due to N-body interactions allow us to directly constrain exoplanet masses in multiplanet systems. This has the potential to improve our understanding of massive directly-imaged planets, which nearly all currently have only model-dependent masses. The VLTI-GRAVITY instrument has demonstrated that interferometry can achieve 100x better astrometric precision than existing methods, a level of precision that makes detection of planet–planet interactions possible. In this study, we show that in the HR-8799 system, planet–planet deviations from currently used Keplerian approximations are expected to be up to one-quarter of a milliarcsecond within five years, which will make them detectable with VLTI-GRAVITY. Modeling of this system to directly constrain exoplanet masses will be crucial in order to make precise predictions.