Structural and core parameters of the hot B subdwarf KPD 0629-0016 from CoRoT g-mode asteroseismology

Context. The asteroseismic exploitation of long period, g-mode hot B subdwarf pulsators (sdBVs), undermined so far by limitations associated with ground-based observations, has now become possible, thanks to high quality data obtained from space such as those recently gathered with the CoRoT (COnvection, ROtation, and planetary Transits) satellite. Aims. We propose a detailed seismic analysis of the sdBVs star KPD 0629-0016, the first compact pulsator monitored with CoRoT, using the g-mode pulsations recently uncovered by that space-borne observatory during short run SRa03. Methods. We use a forward modeling approach on the basis of our latest sdB models, which are now suitable for the accurate com- putation of the g-mode pulsation properties. The simultaneous match of the independent periods observed in KPD 0629-0016 with those of the models leads objectively to the identification of the pulsation modes and, more importantly, to the determination of the structural and core parameters of the star. Results. The optimal model we found closely reproduces the 18 observed periods retained in our analysis at a 0.23% level on av- erage. These are identified as low-degree (l = 1 and 2), intermediate-order (k = −9 through −74) g-modes. The structural and core parameters for KPD 0629-0016 are the following (formal fitting errors only): Teff = 26 290 ± 530 K, log g = 5.450 ± 0.034, M∗ = 0.471 ± 0.002 M⊙, log (Menv/M∗) = −2.42 ± 0.07, log (1 − Mcore/M∗) = −0.27 ± 0.01, and Xcore(C+O) = 0.41 ± 0.01. We addition- ally derive an age of 42.6 ± 1.0 Myr after the zero-age extreme horizontal branch, the radius R = 0.214 ± 0.009 R⊙, the luminosity L = 19.7 ± 3.2 L⊙, the absolute magnitude MV = 4.23 ± 0.13, the reddening index E(B − V) = 0.128 ± 0.023, and the distance d = 1190 ± 115 pc. Conclusions. The advent of high-precision time-series photometry from space with instruments like CoRoT now allows as demon- strated with KPD 0629-0016 the full exploitation of g-modes as deep probes of the internal structure of these stars, in particular for determining the mass of the convective core and its chemical composition.Peer reviewe

Tidally Tilted Pulsations in HD 265435, a Subdwarf B Star with a Close White Dwarf Companion

Abstract: Tidally tilted pulsators (TTPs) are an intriguing new class of oscillating stars in binary systems; in such stars, the pulsation axis coincides with the line of apsides, or tidal axis, of the binary. All three TTPs discovered so far have been δ Scuti stars. In this Letter, we report the first conclusive discovery of tidally tilted pulsations in a subdwarf B (sdB) star. HD 265435 is an sdB–white dwarf binary with a 1.65 hr period that has been identified and characterized as the nearest potential Type Ia supernova progenitor. Using TESS 20 s cadence data from Sectors 44 and 45, we show that the pulsation axis of the sdB star has been tidally tilted into the orbital plane and aligned with the tidal axis of the binary. We identify 31 independent pulsation frequencies, 27 of which have between 1 and 7 sidebands separated by the orbital frequency (ν orb) or multiples thereof. Using the observed amplitude and phase variability due to tidal tilting, we assign ℓ and m values to most of the observed oscillation modes and use these mode identifications to generate preliminary asteroseismic constraints. Our work significantly expands our understanding of TTPs, as we now know that (i) they can be found in stars other than δ Scuti pulsators, especially highly evolved stars that have lost their H-rich envelopes, and (ii) tidally tilted pulsations can be used to probe the interiors of stars in very tight binaries

Deep asteroseismic sounding of the compact hot B subdwarf pulsator KIC02697388 from Kepler time series photometry

peer reviewedContext. Contemporary high precision photometry from space provided by the Kepler and CoRoT satellites generates significant breakthroughs in terms of exploiting the long-period, g-mode pulsating hot B subdwarf (sdBVs) stars with asteroseismology. Aims: We present a detailed asteroseismic study of the sdBVs star KIC02697388 monitored with Kepler, using the rich pulsation spectrum uncovered during the ~27-day-long exploratory run Q2.3. Methods: We analyse new high-S/N spectroscopy of KIC02697388 using appropriate NLTE model atmospheres to provide accurate atmospheric parameters for this star. We also reanalyse the Kepler light curve using standard prewhitening techniques. On this basis, we apply a forward modelling technique using our latest generation of sdB models. The simultaneous match of the independent periods observed in KIC02697388 with those of models leads objectively to the identification of the pulsation modes and, more importantly, to the determination of some of the parameters of the star. Results: The light curve analysis reveals 43 independent frequencies that can be associated with oscillation modes. All the modulations observed in this star correspond to g-mode pulsations except one high-frequency signal, which is typical of a p-mode oscillation. Although the presence of this p-mode is surprising considering the atmospheric parameters that we derive for this cool sdB star (Teff = 25 395 ± 227 K, log g = 5.500 ± 0.031 (cgs), and log N(He) /N(H) = -2.767 ± 0.122), we show that this mode can be accounted for particularly well by our optimal seismic models, both in terms of frequency match and nonadiabatic properties. The seismic analysis leads us to identify two model solutions that can both account for the observed pulsation properties of KIC02697388. Despite this remaining ambiguity, several key parameters of the star can be derived with stringent constraints, such as its mass, its H-rich envelope mass, its radius, and its luminosity. We derive the properties of the core proposing that it is a relatively young sdB star that has burnt less than ~34% (in mass) of its central helium and has a relatively large mixed He/C/O core. This latter measurement is in line with the trend already uncovered for two other g-mode sdB pulsators analysed with asteroseismology and suggests that extra mixing is occurring quite early in the evolution of He cores on the horizontal branch. Conclusions: Additional monitoring with Kepler of this particularly interesting sdB star should reveal the inner properties of KIC02697388 and provide important information about the mode driving mechanism and the helium core properties

Discovery of 74 new bright ZZ Ceti stars in the first three years of TESS

We report the discovery of 74 new pulsating DA white dwarf stars, or ZZ Cetis, from the data obtained by the Transiting Exoplanet Survey Satellite mission, from Sectors 1 to 39, corresponding to the first 3 cycles. This includes objects from the Southern hemisphere (Sectors 1–13 and 27–39) and the Northern hemisphere (Sectors 14–26), observed with 120 s- and 20 s-cadence. Our sample likely includes 13 low-mass and one extremely low-mass white dwarf candidate, considering the mass determinations from fitting Gaia magnitudes and parallax. In addition, we present follow-up time series photometry from ground-based telescopes for 11 objects, which allowed us to detect a larger number of periods. For each object, we analysed the period spectra and performed an asteroseismological analysis, and we estimate the structure parameters of the sample, i.e. stellar mass, effective temperature, and hydrogen envelope mass. We estimate a mean asteroseismological mass of 〈Msis〉 = 0.635 ± 0.015 M⊙, excluding the candidate low or extremely low-mass objects. This value is in agreement with the mean mass using estimates from Gaia data, which is 〈Mphot〉 = 0.631 ± 0.040 M⊙, and with the mean mass of previously known ZZ Cetis of 〈M*〉 = 0.644 ± 0.034 M⊙. Our sample of 74 new bright ZZ Cetis increases the number of known ZZ Cetis by ∼20 per cent

TESS first look at evolved compact pulsators : Asteroseismology of the pulsating helium-atmosphere white dwarf TIC 257459955

Context. Pulsation frequencies reveal the interior structures of white dwarf stars, shedding light on the properties of these compact objects that represent the final evolutionary stage of most stars. Two-minute cadence photometry from the Transiting Exoplanet Survey Satellite (TESS) records pulsation signatures from bright white dwarfs over the entire sky. Aims. As part of a series of first-light papers from TESS Asteroseismic Science Consortium Working Group 8, we aim to demonstrate the sensitivity of TESS data, by measuring pulsations of helium-atmosphere white dwarfs in the DBV instability strip, and what asteroseismic analysis of these measurements can reveal about their stellar structures. We present a case study of the pulsating DBV WD 0158−160 that was observed as TIC 257459955 with the two-minute cadence for 20.3 days in TESS Sector 3. Methods. We measured the frequencies of variability of TIC 257459955 with an iterative periodogram and prewhitening procedure. The measured frequencies were compared to calculations from two sets of white dwarf models to constrain the stellar parameters: the fully evolutionary models from LPCODE and the structural models from WDEC. Results. We detected and measured the frequencies of nine pulsation modes and eleven combination frequencies of WD 0158−160 to ∼0.01 µHz precision. Most, if not all, of the observed pulsations belong to an incomplete sequence of dipole (` = 1) modes with a mean period spacing of 38.1 ± 1.0 s. The global best-fit seismic models from both LPCODE and WDEC have effective temperatures that are &3000 K hotter than archival spectroscopic values of 24 100–25 500 K; however, cooler secondary solutions are found that are consistent with both the spectroscopic effective temperature and distance constraints from Gaia astrometry. Conclusions. Our results demonstrate the value of the TESS data for DBV white dwarf asteroseismology. The extent of the shortcadence photometry enables reliably accurate and extremely precise pulsation frequency measurements. Similar subsets of both the LPCODE and WDEC models show good agreement with these measurements, supporting that the asteroseismic interpretation of DBV observations from TESS is not dominated by the set of models used. However, given the sensitivity of the observed set of pulsation modes to the stellar structure, external constraints from spectroscopy and/or astrometry are needed to identify the best seismic solutions.Facultad de Ciencias Astronómicas y Geofísica

Le potentiel de l'astéroséismologie pour les étoiles sous-naines de type B

N/AL'objectif principal de cette thèse consiste à évaluer les possibilités que les étoiles sous naines de type B, aussi appelées sdB, puissent développer des variations de luminosité engendrées par des phénomènes de pulsations. Dans la mesure où, au commencement de cette étude, les sdB ne sont pas connues pour montrer ce type de comportement, notre approche s'effectue exclusivement sur des bases théoriques visant à déterminer, par le calcul, si ces étoiles ont le potentiel pour devenir instables. Le cas échéant, il s'agira d'évaluer quels sont les résultats susceptibles d'émerger d'un sondage de la structure interne de ces étoiles avec les méthodes de l'astéroséismologie.Après avoir introduit le contexte et les outils théoriques nécessaires à ce projet (théorie des pulsations stellaires et modèles d'étoiles sous-naines de type B), la démarche passe obligatoirement par une étude exhaustive des propriétés des modes de pulsation dans ces étoiles. Nous l'avons entreprise de manière systématique afin d'évaluer et de comprendre les comportements des oscillations en fonction des différents paramètresphysiques qui caractérisent une sdB. Par souci de complétude, nous étudions également les rapports qu'entretiennent évolution et périodes de pulsation au cours de la phase sdB. Par la suite, fort des connaissances nouvellement acquises, nous nous lançons dans l'étude de la stabilité des modes d'oscillation, l'objectif étant d'identifier, le cas échéant, un mécanisme capable de déstabiliser, dans certaines conditions, une fraction de ces étoiles. Par cette approche, nous déterminons qu'un mécanisme kappa associé à une région d'ionisation partielle de l'élément fer agit efficacement dans l'enveloppe des sdB si, toutefois, le fer y est présent en quantités extra-solaires. Nous montrons alors que des processus de diffusion,déjà fortement suspectés d'exister dans ces étoiles, sont en mesure d'accumuler des quantités de fer largement suffisantes pour engendrerdes pulsations, nous conduisant ainsi à avancer la prédiction que des sdB pulsantes doivent exister.L'annonce, indépendante et pratiquement simultanée, de la découverte de véritables sdB pulsantes ainsi que les premières comparaisonsentre théorie et observations nous poussent alors à construire des modèles plus sophistiqués $-$ incluant les effets de la diffusion sur le fer $-$, mieux adaptés pour décrire le mécanisme de déstabilisation proposé. Nous constatons alors un très bon accord quantitatif entre les propriétés sismiques déduites des modèles théoriques et celles effectivement observées dans les sdB pulsantes, confirmant dès lors le rôle joué par le mécanisme en question.Nous discutons également des aspects reliés à l'étude astéroséismologique de ces étoiles dont l'objectif, ultimement, est d'en sonder l'intérieur. Bien qu'il soit encore prématuré d'appliquer une telle méthode sur les sdB, nous explorons rapidement les moyens pour y parvenir et nous tentons de préciser quels sont les éléments de la structure des sdB que nous pouvons espérer mesurer avec cette technique.Finalement, suite aux résultats satisfaisants obtenus pour les sdB, nous entreprenons de poursuivre l'étude de stabilité sur les modèles évolutifs en phase post-EHB. Nous constatons alors l'existence de modèles instables, identifiables aux étoiles naines blanches de type DAO, pour lesquels des modes g de faible ordre radial sont excités par un mécanisme epsilon associé à la région de brûlage en couche résiduel de l'hydrogène située à la base de l'enveloppe des modèles. Ce résultat nous conduit ainsi à proposer l'existence d'une autre classe d'étoiles pulsantes parmi les DAO. Contrairement aux sdB, cette prédiction reste toutefois à confirmer par l'observation