J/A+A/706/A200ivo://CDS.VizieR/J/A+A/706/A200CDSChecha V.A.Aret A.Kolka I.Liimets T.Araya I.Christen A.,Avila Marin G.F.Levenhagen R.S.Cidale L.Eenmaee T.Hajiyeva G.,Kivila Ue.Mitrokhina V.Ramler H.Verro T.2026-03-02T06:25:50Z2026-02-10T10:30:45ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frvariable-starssupergiant-starsphotometryvisible-astronomyThe post-main-sequence evolution of massive stars remains poorly understood, particularly in the case of blue supergiants. As key drivers of the dynamical and chemical evolution of galaxies, massive stars warrant detailed investigation during this complex evolutionary stage. Hot supergiants exhibit pronounced photometric and spectroscopic variability, typically in the form of quasi-periodic rather than strictly periodic variations. We investigate the variability patterns of the evolved B-type star rho Leo to determine its properties, identify the underlying physical processes, and constrain its evolutionary stage. We have combined extensive, long-term datasets of spectroscopic and photometric observations from various sources. These include data from the TESS and Kepler space telescopes, as well as observations from the 1.5m telescope in Estonia. We analysed the data using the Generalized Lomb-Scargle periodogram, Lomb-Scargle periodogram with pre-whitening, and the Weighted Wavelet Z-Transform. To determine the fundamental parameters of rho Leo, we fitted synthetic line profiles computed with FastWind code to the HARPS spectrum. We used the zpektr code to infer the stellar rotation inclination angle. The HeI 6678.151{AA} line profile exhibits significant changes in radial velocity and, consequently, in its moment values. We identify a set of periods and harmonics ranging from ~0.8 to ~35 days. Some periods remain nearly constant, while others appear and disappear from one observing season to another. A comparison of spectroscopic and photometric data, along with the shape of the phase curves, helps to constrain the nature of several periods. In particular, the ~11-day period is attributed to stellar rotation, while the ~17-day period is associated with radial pulsations.2026A&A...706A.200Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/706/A200CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/706/A200https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/706/A200http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/706/A200https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/706/A200https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/706/A200http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/706/A200GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/A+A/706/A200/tessTESS data (table A2)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDBarycentric Julian datedtime.epochdoubledmagDifferential magnitudemagphot.mag;arith.diffdoubleJ/A+A/706/A200/m1-2017First normalized moment data, 2017 (table A3)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHJDHeliocentric Julian datedtime.epochdoubleM1The first normalized moment (centroid)km/sspect.line.widthfloatJ/A+A/706/A200/m1-2022First normalized moment data, 2022 (table A4)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHJDHeliocentric Julian datedtime.epochdoubleM1The first normalized moment (centroid)km/sspect.line.widthfloat