Examinando por Autor "Kervella, Pierre"

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    The Orbit and Dynamical Mass of Polaris: Observations with the CHARA Array
    (Institute of Physics, 2024-08) Evans, Nancy Remage; Schaefer, Gail H.; Gallenne, Alexandre; Torres, Guillermo; Horch, Elliott P.; Anderson, Richard I.; Monnier, John D.; Roettenbacher, Rachael M.; Baron, Fabien; Anugu, Narsireddy; Davidson, James W.; Kervella, Pierre; Bras, Garance; Proffitt, Charles; Mérand, Antoine; Karovska, Margarita; Jones, Jeremy; Lanthermann, Cyprien; Kraus, Stefan; Codron, Isabelle; Bond, Howard E.; Viviani, Giordano
    The 30 yr orbit of the Cepheid Polaris has been followed with observations by the Center for High Angular Resolution Astronomy (CHARA) Array from 2016 through 2021. An additional measurement has been made with speckle interferometry at the Apache Point Observatory. Detection of the companion is complicated by its comparative faintness—an extreme flux ratio. Angular diameter measurements appear to show some variation with pulsation phase. Astrometric positions of the companion were measured with a custom grid-based model-fitting procedure and confirmed with the CANDID software. These positions were combined with the extensive radial velocities (RVs) discussed by Torres to fit an orbit. Because of the imbalance of the sizes of the astrometry and RV data sets, several methods of weighting are discussed. The resulting mass of the Cepheid is 5.13 ± 0.28 M ⊙. Because of the comparatively large eccentricity of the orbit (0.63), the mass derived is sensitive to the value found for the eccentricity. The mass combined with the distance shows that the Cepheid is more luminous than predicted for this mass from evolutionary tracks. The identification of surface spots is discussed. This would give credence to the identification of a radial velocity variation with a period of approximately 120 days as a rotation period. Polaris has some unusual properties (rapid period change, a phase jump, variable amplitude, and unusual polarization). However, a pulsation scenario involving pulsation mode, orbital periastron passage, and low pulsation amplitude can explain these characteristics within the framework of pulsation seen in Cepheids.
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    The Orbit and Mass of the Cepheid AW Per
    (Institute of Physics, 2024-09) Evans, Nancy Remage; Gallenne, Alexandre; Kervella, Pierre; Mérand, Antoine; Monnier, John; Anderson, Richard I; Günther, H. Moritz; Proffitt, Charles; Winston, Elaine M.; Pietrzynski, Grzegorz; Gieren, Wolfgang; Kuraszkiewicz, Joanna; Anugu, Narsireddy; Roettenbacher, Rachael M.; Lanthermann, Cyprien; Gutierrez, Mayra; Schaefer, Gail; Setterholm, Benjamin R.; Ibrahim, Noura; Kraus, Stefan
    The Cepheid AW Per is a component in a multiple system with a long-period orbit. The radial velocities of Griffin cover the 38 yr orbit well. An extensive program of interferometry with the Center for High Angular Resolution Astronomy array is reported here, from which the long-period orbit is determined. In addition, a Hubble Space Telescope high-resolution spectrum in the ultraviolet demonstrates that the companion is itself a binary with nearly equal-mass components. These data combined with a distance from Gaia provide a mass of the Cepheid (primary) of M 1 = 6.79 ± 0.85 M ⊙. The combined mass of the secondary is M S = 8.79 ± 0.50 M ⊙. The accuracy of the mass will be improved after the fourth Gaia data release, expected in approximately two years.