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dc.rights.license© ESO 2021es
dc.contributor.authorMarcos Arenal, P.-
dc.contributor.authorMendigutía, I.-
dc.contributor.authorKoumpia, E.-
dc.contributor.authorOudmaijer, R. D.-
dc.contributor.authorVioque, M.-
dc.contributor.authorGuzmán Díaz, J.-
dc.contributor.authorWichittanakom, C.-
dc.contributor.authorDe Wit, W. J.-
dc.contributor.authorMontesinos, B.-
dc.contributor.authorIlee, J. D.-
dc.identifier.citationAstronomy and Astrophysics 652: A68(2021)es
dc.description.abstractContext. It has been hypothesized that the location of Herbig Ae/Be stars (HAeBes) within the empirical relation between the inner disk radius (rin), inferred from K-band interferometry, and the stellar luminosity (L*), is related to the presence of the innermost gas, the disk-to-star accretion mechanism, the dust disk properties inferred from the spectral energy distributions (SEDs), or a combination of these effects. However, no general observational confirmation has been provided to date. Aims. This work aims to test whether the previously proposed hypotheses do, in fact, serve as a general explanation for the distribution of HAeBes in the size–luminosity diagram. Methods. GRAVITY/VLTI spectro-interferometric observations at ~2.2 μm have been obtained for five HBes representing two extreme cases concerning the presence of innermost gas and accretion modes. V590 Mon, PDS 281, and HD 94509 show no excess in the near-ultraviolet, Balmer region of the spectra (ΔDB), indicative of a negligible amount of inner gas and disk-to-star accretion, whereas DG Cir and HD 141926 show such strong ΔDB values that cannot be reproduced from magnetospheric accretion, but probably come from the alternative boundary layer mechanism. In turn, the sample includes three Group I and two Group II stars based on the Meeus et al. SED classification scheme. Additional data for these and all HAeBes resolved through K-band interferometry have been compiled from the literature and updated using Gaia EDR3 distances, almost doubling previous samples used to analyze the size–luminosity relation. Results. We find no general trend linking the presence of gas inside the dust destruction radius or the accretion mechanism with the location of HAeBes in the size–luminosity diagram. Similarly, our data do not support the more recent hypothesis linking such a location and the SED groups. Underlying trends are present and must be taken into account when interpreting the size–luminosity correlation. In particular, it cannot be statistically ruled out that this correlation is affected by dependencies of both L* and rin on the wide range of distances to the sources. Still, it is argued that the size–luminosity correlation is most likely to be physically relevant in spite of the previous statistical warning concerning dependencies on distance. Conclusions. Different observational approaches have been used to test the main scenarios proposed to explain the scatter of locations of HAeBes in the size–luminosity diagram. However, none of these scenarios have been confirmed as a fitting general explanation and this issue remains an open
dc.description.sponsorshipBased on observations collected at the European Southern Observatory under ESO programme 0102.C-0576. The authors acknowledge the anonymous referee for the useful comments, which have served to improve the manuscript. PMA, IM, and JGD acknowledge the Government of Comunidad Autónoma de Madrid (Spain) for funding this research through a ‘Talento’ Fellowship (2016-T1/TIC-1890, PI I. Mendigutía). The research of IM, JGD, and BM is also partially funded by the Spanish “Ministerio de Ciencia, Innovación y Universidades” through the national project “On the Rocks II” (PGC2018-101950-B-100; PI E. Villaver). EK is funded by the STFC (ST/P00041X/1). MV acknowledges the STARRY project, which has received funding from the European Union’s Horizon 2020 research and innovation programme under MSCA ITN-EID grant agreement No 676036. The research leading to these results has received funding from the European Union’s Horizon 2020 research and innovation programme under Grant Agreement 730890 (OPTICON). This research has made use of the Jean-Marie Mariotti Center LITpro4 service co-developed by CRAL, IPAG and LAGRANGE. PMA acknowledges M. Tallon in particular for his support on LITpro, and A.C. Carciofi and R.G. Vieira for their contribution to the observing proposal leading to these
dc.publisherEDP Scienceses
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-101950-B-I00/ES/ON THE ROCKS II/-
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.subjectStars: variable T Tauri, Herbig Ae/Bees
dc.subjectProtoplanetary diskses
dc.subjectStars: pre-main sequencees
dc.subjectAccretion diskses
dc.subjectInstrumentation: interferometerses
dc.titleK-band GRAVITY/VLTI interferometry of “extreme” Herbig Be stars. The size–luminosity relation revisitedes
dc.contributor.orcidMarcos Arenal, P. [0000-0003-1549-9396]-
dc.contributor.funderAgencia Estatal de Investigación (AEI), European Research Council-
dc.contributor.funderComunidad de Madrid-
dc.contributor.funderScience and Technology Facilities Council (STFC)-
dc.contributor.funderEuropean Research Council (ERC)-
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