Proyecto de Investigación: RYC-2012-09913
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RYC-2012-09913
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Unveiling the power spectra of delta Scuti stars with TESS The temperature, gravity, and frequency scaling relation
(EDP Sciences, 2020-06-11) Barceló Forteza, S.; Moya, A.; Barrado, D.; Martín Ruiz, S.; Suárez, J. C.; García Hernández, A.; Solano, Enrique; National Aeronautics and Space Administration (NASA); Ministerio de Economía y Competitividad (MINECO); European Research Council (ERC); Agencia Estatal de Investigación (AEI); Universidad de Granada (UGR); Junta de Andalucía; 0000-0001-9281-2919; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709
Thanks to high-precision photometric data legacy from space telescopes like CoRoT andKepler, the scientific community could detect and characterize the power spectra of hundreds of thousands of stars. Using the scaling relations, it is possible to estimate masses and radii for solar-type pulsators. However, these stars are not the only kind of stellar objects that follow these rules:delta Scuti stars seem to be characterized with seismic indexes such as the large separation (Delta nu). Thanks to long-duration high-cadence TESS light curves, we analysed more than two thousand of this kind of classical pulsators. In that way, we propose the frequency at maximum power (nu(max)) as a proper seismic index since it is directly related with the intrinsic temperature, mass and radius of the star. This parameter seems not to be affected by rotation, inclination, extinction or resonances, with the exception of the evolution of the stellar parameters. Furthermore, we can constrain rotation and inclination using the departure of temperature produced by the gravity-darkening effect. This is especially feasible for fast rotators as most of delta Scuti stars seem to be. © ESO 2020.
The first view of δ Scuti and γ Doradus stars with the TESS mission
(Oxford Academics: Oxford University Press, 2019-10-07) Antoci, V.; Cunha, M. S.; Bowman, D. M.; Murphy, S. J.; Kurtz, D. W.; Bedding, T. R.; Borre, C. C.; Christophe, S.; Daszyńska-Daszkiewicz, J.; Fox Machado, L.; García Hernández, A.; Ghasemi, H.; Handberg, R.; Hansen, H.; Hasanzadeh, A.; Houdek, G.; Johnston, C.; Justesen, A. B.; Kahraman Alicavus, F.; Kotysz, K.; Latham, D.; Matthews, J. M.; Monster, J.; Niemczura, E.; Paunzen, E.; Sánchez Arias, J. P.; Pigulski, A.; Pepper, J.; Richey Yowell, T.; Safari, H.; Seager, S.; Smalley, B.; Shutt, T.; Sódor, A.; Suárez, J. C.; Tkachenko, A.; Wu, T.; Zwintz, K.; Barceló Forteza, S.; Brunsden, E.; Bognár, Z.; Buzasi, D. L.; Chowdhury, S.; De Cat, P.; Evans, J. A.; Guo, Z.; Guzik, J. A.; Jetvic, N.; Lampens, P.; Lares Martiz, M.; Lovekin, C.; Li, G.; Mirouh, G. M.; Mkrtichian, D.; Monteiro, M. J. P. F. G.; Nemec, J. M.; Ouazzani, R. M.; Pascual Granado, J.; Reese, D. R.; Rieutord, M.; Rodon, J. R.; Skarka, M.; Sowicka, P.; Stateva, I.; Szabó, R.; Weiss, W. W.; Universidad Nacional Autónoma de México (UNAM); Agence Nationale de la Recherche (ANR); National Natural Science Foundation of China (NSFC); Danish National Research Foundation (DNRF); National Aeronautics and Space Administration (NASA); Fundacao para a Ciencia e a Tecnologia (FCT); National Science Centre, Poland (NCN); Hungarian Academy of Sciences (MTA); European Research Council (ERC); Ministerio de Economía y Competitividad (MINECO); Research Foundation Flanders (FWO); BELgian federal Science Policy Office (BELSPO); Science and Technology Facilities Council (STFC); Johnston, C. [0000-0002-3054-4135]; Granado, J. P. [0000-0003-0139-6951]; Monteiro, M. J. P. F. G. [0000-0003-0513-8116]; Szabo, R. [0000-0002-3258-1909]; Browman, D. [0000-0001-7402-3852]; Safari, H. [0000-0003-2326-3201]; Simon, M. [0000-0002-5648-3107]; Houdek, G. [0000-0003-1819-810X]; Ghasemi, H. [0000-0001-9534-9763]; Handerberg, R. [0000-0001-8725-4502]; Borre, C. C. [0000-0003-1286-8512]; Cunha, M. [0000-0001-8237-7343]; Justensen, A. B. [0000-0002-0174-2466]; Antoci, V. [0000-0002-0865-3650]; Christophe, S. [0000-0002-4153-870X]; Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFISICA DE ANDALUCIA (IAA), SEV-2017-0709; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
We present the first asteroseismic results for δ Scuti and γ Doradus stars observed in Sectors 1 and 2 of the TESS mission. We utilize the 2-min cadence TESS data for a sample of 117 stars to classify their behaviour regarding variability and place them in the Hertzsprung–Russell diagram using Gaia DR2 data. Included within our sample are the eponymous members of two pulsator classes, γ Doradus and SX Phoenicis. Our sample of pulsating intermediate-mass stars observed by TESS also allows us to confront theoretical models of pulsation driving in the classical instability strip for the first time and show that mixing processes in the outer envelope play an important role. We derive an empirical estimate of 74 per cent for the relative amplitude suppression factor as a result of the redder TESS passband compared to the Kepler mission using a pulsating eclipsing binary system. Furthermore, our sample contains many high-frequency pulsators, allowing us to probe the frequency variability of hot young δ Scuti stars, which were lacking in the Kepler mission data set, and identify promising targets for future asteroseismic modelling. The TESS data also allow us to refine the stellar parameters of SX Phoenicis, which is believed to be a blue straggler.
