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51. Cometary dust in the planetary belts of β Pictoris

Author

Vries, B. L., Acke, B., Waters, L. B. F. M., Blommaert, J. A. D. L., Bart Vandenbussche, Dominik, C., Waelkens, C., and Low Energy Astrophysics (API, FNWI)

Abstract

The discovery of more than 600 exo-planets in the past two decades has shown an amazing diversity in the properties of planetary systems. The origin of this diversity and the way the Solar Systemfits inmust be understood by studying young systems in which planet formation is ongoing, and by comparing the properties of these young systems with the historic records of the formation of the Solar System as recorded in e.g. asteroids and comets. Strong evidence that gas-phase condensation produces Mg2SiO4, comes from observations of crystalline olivine grains in evolved cool red giants. In another study we have detected the 69 μm crystalline olivine band in several red giants and the wavelength and band shape of the resonance are in agreement with pure Mg2SiO4. In contrast, Solar Systemcomets such as Wild 2 and chondritic meteorites show a small but significant fraction of Fe in the crystalline olivine of "1 per cent. β Pictoris is a young (12 Myr) main-sequence star surrounded by at least one planet at a distance of "10 AU, and a dusty debris disk created by catastrophic collisions of planetesimals. We have detected the 69 μm band in a HERSCHEL- PACS Range Scan of β Pictoris. Modeling this band gives an Fe/Mg ratio of 0.01 and constrains the location of the crystalline olivine to 8-16 AU. The crystalline olivine grains are probably produced by collisions between planetesimals in the known belts at 6 and 16 AU. The composition of the crystalline olivine is strikingly similar to that of Solar System bodies like comets, IDPs and meteorites. But an Fe/Mg ratio of 0.01 is not compatible with crystalline olivine grains produced through gas phase condensation, meaning that the crystalline olivine in β Pictoris must come from another source, similar to the one in our Solar System.

Published
2012

52. Uncovering the Pulsating Photospheres of Mira Stars through Near-IR Interferometry: A Case Study on R Vir

Author

Hillen, M., Verhoelst, T., Acke, B., Degroote, P., Kerschbaum, F, Lebzelter, T, Wing, RF, Kerschbaum, F., Lebzelter, T., and Wing, R. F.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We present the methodology and some preliminary results of our study of the relationship between a Mira's pulsating photosphere and its surrounding molecular layer(s) throughout several pulsation cycles, based on spatially resolved data. Our dataset consists of archival narrow-band observations in the near-infrared H and K bands obtained with the Palomar Testbed Interferometer between 1999 and 2006, extended with a few nights of VLTI AMBER low spectral resolution data and near-infrared SAAO photometry. The fitted model is the geometric star + layer model proposed by Perrin et al. (2004), in which the physical parameters (diameter and temperature of star and layer; wavelength dependent optical depth of the layer) are given a sinusoidal time dependence., Comment: 2 pages, to be published in ASP Conference Proceedings of the Vienna conference "Why Galaxies Care About AGB Stars II"

Published
2011

53. Detection of solar-like oscillations in the bright red giant stars γ Piscium and θ1 Tauri from a 190-day high-precision spectroscopic multi-site campaign⋆

Author

Beck, P.G., Kambe, E., Hillen, M., Corsaro, E., Winckel, H. van, Moravveji, E., Ridder, J. de, Bloemen, S., Saesen, S., Mathias, P., Degroote, P., Kallinger, T., Verhoelst, T., Ando, H., Carrier, F., Acke, B., Oreiro, R., Miglio, A., Eggenberger, P., Sato, B., Zwintz, K., Pápics, P.I., Marcos-Arenal, P., Fuentes, S.A. Sans, Schmid, V.S., Waelkens, C., Østensen, R.H., Matthews, J.M., Yoshida, M., Izumiura, H., Koyano, H., Nagayama, S., Shimizu, Y., Okada, N., Okita, K., Sakamoto, A., Yamamuro, T., Aerts, C., Beck, P.G., Kambe, E., Hillen, M., Corsaro, E., Winckel, H. van, Moravveji, E., Ridder, J. de, Bloemen, S., Saesen, S., Mathias, P., Degroote, P., Kallinger, T., Verhoelst, T., Ando, H., Carrier, F., Acke, B., Oreiro, R., Miglio, A., Eggenberger, P., Sato, B., Zwintz, K., Pápics, P.I., Marcos-Arenal, P., Fuentes, S.A. Sans, Schmid, V.S., Waelkens, C., Østensen, R.H., Matthews, J.M., Yoshida, M., Izumiura, H., Koyano, H., Nagayama, S., Shimizu, Y., Okada, N., Okita, K., Sakamoto, A., Yamamuro, T., and Aerts, C.

Abstract

Contains fulltext : 139608.pdf (preprint version ) (Open Access)

Published
2015

54. Towards ensemble asteroseismology of the young open clusters \u03c7 Persei and NGC 6910

Author

Saesen, S., Pigulski, A., Carrier, F., Michalska, G., Aerts, C., De Ridder, J., Briquet, M., Handler, G., Kołaczkowski, Z., Acke, B., Bauwens, E., Beck, P. G., Blom, Y., Blommaert, J., Broeders, E., Cherix, M., Davignon, G., Debosscher, J., Degroote, P., Decin, L., Dehaes, S., De Meester, W., Deroo, P., Desmet, M., Drummond, R., Eggen, J. R., Fu, J., Gazeas, K., Gelven, G. A., Gielen, C., Huygen, R., Jiang, X., Kalomeni, B., Kim, S.-L., Kim, D. H., Kopacki, G., Kwon, J.-H., Ladjal, D., Lee, C.-U., Lee, Y.-J, Saesen, Pigulski, Carrier, Michalska, Aerts, De Ridder, Briquet, Handler, Kołaczkowski, Acke, Bauwens, Beck, P. G., Blom, Blommaert, Broeders, Cherix, Davignon, Debosscher, Degroote, Decin, Dehaes, De Meester, Deroo, Desmet, Drummond, Eggen, J. R., Gazeas, Gelven, G. A., Gielen, Huygen, Jiang, Kalomeni, Kim, S.-L., D. H., Kopacki, Kwon, J.-H., Ladjal, Lee, C.-U., and Y.-J

Published
2010

55. The 2003–2004 multisite photometric campaign for the β Cephei and eclipsing star 16 (EN) Lacertae with an appendix on 2 Andromedae, the variable comparison star

Author

Jerzykiewicz, M., primary, Handler, G., additional, Daszyńska-Daszkiewicz, J., additional, Pigulski, A., additional, Poretti, E., additional, Rodríguez, E., additional, Amado, P. J., additional, Kołaczkowski, Z., additional, Uytterhoeven, K., additional, Dorokhova, T. N., additional, Dorokhov, N. I., additional, Lorenz, D., additional, Zsuffa, D., additional, Kim, S.-L., additional, Bourge, P.-O., additional, Acke, B., additional, De Ridder, J., additional, Verhoelst, T., additional, Drummond, R., additional, Movchan, A. I., additional, Lee, J.-A., additional, Stȩślicki, M., additional, Molenda-Żakowicz, J., additional, Garrido, R., additional, Kim, S.-H., additional, Michalska, G., additional, Paparó, M., additional, Antoci, V., additional, and Aerts, C., additional

Published
2015
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56. The β Pictoris disk imaged by Herschel PACS and SPIRE [Letter]

Author

Vandenbussche, B., Sibthorpe, B., Acke, B., Pantin, E., Olofsson, G., Waelkens, C., Dominik, C., Barlow, M. J., Blommaert, J. A. D. L., Bouwman, J., Brandeker, A., Cohen, M., De Meester, W., Dent, W. R. F., Exter, K., Di Francesco, J., Fridlund, M., Gear, Walter Kieran, Glauser, A. M., Gomez, Haley Louise, Greaves, J. S., Hargrave, Peter Charles, Harvey, P. M., Henning, Th., Heras, A. M., Hogerheijde, M. R., Holland, W. S., Huygen, R., Ivison, R. J., Jean, C., Leeks, S. J., Lim, T. L., Liseau, R., Matthews, B. C., Naylor, D. A., Pilbratt, G. L., Polehampton, E. T., Regibo, S., Royer, P., Sicilia-Aguilar, A., Swinyard, B. M., Walker, H. J., and Wesson, R.

Subjects
QB
Abstract

We obtained Herschel PACS and SPIRE images of the thermal emission of the debris disk around the A5V star β Pic. The disk is well resolved in the PACS filters at 70, 100, and 160 μm. The surface brightness profiles between 70 and 160 μm show no significant asymmetries along the disk, and are compatible with 90% of the emission between 70 and 160 μm originating in a region closer than 200 AU to the star. Although only marginally resolving the debris disk, the maps obtained in the SPIRE 250–500 μm filters provide full-disk photometry, completing the SED over a few octaves in wavelength that had been previously inaccessible. The small far-infrared spectral index (β = 0.34) indicates that the grain size distribution in the inner disk (

Published
2010

57. Towards ensemble asteroseismology of the young open clusters χ Persei and NGC 6910

Author

Saesen, S. Pigulski, A. Carrier, F. Michalska, G. Aerts, C. De Ridder, J. Briquet, M. Handler, G. Kołaczkowski, Z. Acke, B. Bauwens, E. Beck Blom, Y. Blommaert, J. Broeders, E. Cherix, M. Davignon, G. Debosscher, J. Degroote, P. Decin, L. Dehaes, S. De Meester, W. Deroo, P. Desmet, M. Drummond, R. Eggen, J.R. Fu, J. Gazeas, K. Gelven, G.A. Gielen, C. Huygen, R. Jiang, X. Kalomeni, B. Kim, S.-L. Kim, D.H. Kopacki, G. Kwon, J.-H. Ladjal, D. Lee, C.-U. Lee, Y.-J. Lefever, K. Leitner, A. Lenz, P. Liakos, A. Lorenz, D. Narwid, A. Niarchos, P. Østensen, R. Poretti, E. Prins, S. Provencal, J. Puga Antolin, E. Puschnig, J. Raskin, G. Reed, M.D. Reyniers, M. Schmidt, E. Schmitzberger, L. Spano, M. Steininger, B. SteeLicki, M. Uytterhoeven, K. Vanautgaerden, J. Vandenbussche, B. Van Helshoecht, V. Vanhollebeke, E. Van Winckel, H. Verhoelst, T. Vućković, M. Waelkens, C. Wolf, G. Yakut, K. Zhang, C. Zima, W.

Abstract

As a result of the variability survey in χ Persei and NGC 6910, the number of β Cep stars that are members of these two open clusters is increased to twenty stars, nine in NGC 6910 and eleven in χ Persei. We compare pulsational properties, in particular the frequency spectra, of β Cep stars in both clusters and explain the differences in terms of the global parameters of the clusters. We also indicate that the more complicated pattern of the variability among B-type stars in χ Persei is very likely caused by higher rotational velocities of stars in this cluster. We conclude that the sample of pulsating stars in the two open clusters constitutes a very good starting point for the ensemble asteroseismology of β Cep-type stars and maybe also for other B-type pulsators. © 2010 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.

Published
2010

58. The �� Pictoris disk imaged by Herschel PACS and SPIRE

Author

Vandenbussche, B., Sibthorpe, B., Acke, B., Pantin, E., Olofsson, G., Waelkens, C., Dominik, C., Barlow, M. J., Blommaert, J. A. D. L., Bouwman, J., Brandeker, A., Cohen, M., DeMeester, W., Dent, W. R. F., Exter, K., Di Francesco, J., Fridlund, M., Gear, W. K., Glauser, A. M., Gomez, H. L., Greaves, J. S., Hargrave, P. C., Harvey, P. M., Henning, Th., Heras, A. M., Hogerheijde, M. R., Holland, W. S., Huygen, R., Ivison, R. J., Jean, C., Leeks, S. J., Lim, T. L., Liseau, R., Matthews, B. C., Naylor, D. A., Pilbratt, G. L., Polehampton, E. T., Regibo, S., Royer, P., Sicilia-Aguilar, A., Swinyard, B. M., Walker, H. J., and Wesson, R.

Subjects
FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

We obtained Herschel PACS and SPIRE images of the thermal emission of the debris disk around the A5V star �� Pic. The disk is well resolved in the PACS filters at 70, 100, and 160 ��m. The surface brightness profiles between 70 and 160 ��m show no significant asymmetries along the disk, and are compatible with 90% of the emission between 70 and 160 ��m originating in a region closer than 200 AU to the star. Although only marginally resolving the debris disk, the maps obtained in the SPIRE 250 - 500 ��m filters provide full-disk photometry, completing the SED over a few octaves in wavelength that had been previously inaccessible. The small far-infrared spectral index (�� = 0.34) indicates that the grain size distribution in the inner disk (, Accepted for publication in Astronomy&Astrophysics, Herschel First Results special issue

Published
2010
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59. First results of the Herschel key program 'Dust, Ice and Gas In Time' (DIGIT): Dust and gas spectroscopy of HD 100546

Author

Sturm, B., Bouwman, J., Henning, Th., Evans, N. J., Acke, B., Mulders, G. D., Waters, L. B. F. M., Van Dishoeck, E. F., Meeus, G., Green, J. D., Augereau, J. C., Olofsson, J., Salyk, C., Najita, J., Herczeg, G. J., Van Kempen, T. A., Kristensen, L. E., Dominik, C., Carr, J. S., Waelkens, C., Bergin, E., Blake, G. A., Brown, J. M., Chen, J.-H., Cieza, L., Dunham, M. M., Glassgold, A., Güdel, M., Harvey, P. M., Hogerheijde, M. R., Jaffe, D., Jørgensen, J. K., Kim, H. J., Knez, C., Lacy, J. H., Lee, J.-E., Maret, S., Meijerink, R., Merín, B., Mundy, L., Pontoppidan, K. M., Visser, R., Yildiz, U. A., Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2010

60. Waters, dust evolution in protoplanetary disks around herbig ae/be stars—the spitzer view

Author

Juhász, A., Bouwman, J., Henning, Th., Acke, B., Van Den Ancker, M., Meeus, G., Dominik, C., Min, M., Tielens, A. G. G. M., Waters, L.B.F.M., Astrophysics, and Sub Experiment. Astrophysics begr 1/1/14

Abstract

In this paper, we present mid-infrared spectra of a comprehensive set of Herbig Ae/Be stars observed with the Spitzer Space Telescope. The signal-to-noise ratio of these spectra is very high, ranging between about a hundred and several hundreds. During the analysis of these data we tested the validity of standardized protoplanetary dust models and studied grain growth and crystal formation. On the basis of the analyzed spectra, the major constituents of protoplanetary dust around Herbig Ae/Be stars are amorphous silicates with olivine and pyroxene stoichiometry, crystalline forsterite, and enstatite and silica. No other solid-state features, indicating other abundant dust species, are present in the Spitzer spectra. Deviations of the synthetic spectra from the observations are most likely related to grain shape effects and uncertainties in the iron content of the dust grains. Our analysis revealed that larger grains are more abundant in the disk atmosphere of flatter disks than in that of flared disks, indicating that grain growth and sedimentation decrease the disk flaring. We did not find, however, correlations between the value of crystallinity and any of the investigated system parameters. Our analysis shows that enstatite is more concentrated toward the warm inner disk than forsterite, in contrast to predictions of equilibrium condensation models. None of the three crystal formation mechanisms proposed so far can alone explain all our findings. It is very likely that all three play at least some role in the formation of crystalline silicates.

Published
2010

61. Photometric multi-site campaign on the open cluster NGC 884 I. Detection of the variable stars

Author

Saesen, S. Carrier, F. Pigulski, A. Aerts, C. Handler, G. Narwid, A. Fu, J. N. Zhang, C. Jiang, X. J. and Vanautgaerden, J. Kopacki, G. Steslicki, M. Acke, B. and Poretti, E. Uytterhoeven, K. Gielen, C. Ostensen, R. De Meester, W. Reed, M. D. Kolaczkowski, Z. Michalska, G. and Schmidt, E. Yakut, K. Leitner, A. Kalomeni, B. Cherix, M. Spano, M. Prins, S. Van Helshoecht, V. Zima, W. and Huygen, R. Vandenbussche, B. Lenz, P. Ladjal, D. and Antolin, E. Puga Verhoelst, T. De Ridder, J. Niarchos, P. and Liakos, A. Lorenz, D. Dehaes, S. Reyniers, M. and Davignon, G. Kim, S. -L. Kim, D. H. Lee, Y. -J. Lee, C. -U. Kwon, J. -H. Broeders, E. Van Winckel, H. and Vanhollebeke, E. Waelkens, C. Raskin, G. Blom, Y. Eggen, J. R. Degroote, P. Beck, P. Puschnig, J. Schmitzberger, L. Gelven, G. A. Steininger, B. Blommaert, J. Drummond, R. Briquet, M. Debosscher, J.

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Context. Recent progress in the seismic interpretation of field beta Cep stars has resulted in improvements of the physics in the stellar structure and evolution models of massive stars. Further asteroseismic constraints can be obtained from studying ensembles of stars in a young open cluster, which all have similar age, distance and chemical composition. Aims. To improve our comprehension of the beta Cep stars, we studied the young open cluster NGC 884 to discover new B- type pulsators, besides the two known beta Cep stars, and other variable stars. Methods. An extensive multi-site campaign was set up to gather accurate CCD photometry time series in four filters (U, B, V, I) of a field of NGC 884. Fifteen different instruments collected almost 77 500 CCD images in 1286 h. The images were calibrated and reduced to transform the CCD frames into interpretable differential light curves. Various variability indicators and frequency analyses were applied to detect variable stars in the field. Absolute photometry was taken to deduce some general cluster and stellar properties. Results. We achieved an accuracy for the brightest stars of 5.7 mmag in V, 6.9 mmag in B, 5.0 mmag in I and 5.3 mmag in U. The noise level in the amplitude spectra is 50 mu mag in the V band. Our campaign confirms the previously known pulsators, and we report more than one hundred new multi- and mono- periodic B-, A- and F-type stars. Their interpretation in terms of classical instability domains is not straightforward, pointing to imperfections in theoretical instability computations. In addition, we have discovered six new eclipsing binaries and four candidates as well as other irregular variable stars in the observed field.

Published
2010

62. Asteroseismology of massive stars in the young open cluster NGC 884: a status report

Author

Saesen, S., Carrier, F., Pigulski, A., Aerts, C., Handler, G., Narwid, A., Fu, J. N., Zhang, C., Jiang, X. J., Kopacki, G., Vanautgaerden, J., Steślicki, M., Acke, B., Poretti, E., Uytterhoeven, K., De Meester, W., Reed, M. D., Kołaczkowski, Z., Michalska, G., Schmidt, E., xd6stensen, R., Gielen, C., Yakut, K., Leitner, A., Kalomeni, B., Prins, S., van Helshoecht, V., Zima, W., Huygen, R., Vandenbussche, B., Lenz, P., Ladjal, E., Puga Antolxedn, E., Verhoelst, T., De Ridder, J., Niarchos, P., Liakos, A., Lorenz, Saesen, Carrier, Pigulski, Aerts, Handler, Narwid, J. N., Zhang, Jiang, X. J., Kopacki, Vanautgaerden, Steślicki, Acke, Poretti, Uytterhoeven, De Meester, Reed, M. D., Kołaczkowski, Michalska, Schmidt, xd6stensen, Gielen, Yakut, Leitner, Kalomeni, Prins, van Helshoecht, Zima, Huygen, Vandenbussche, Lenz, Ladjal, Puga Antolxedn, Verhoelst, De Ridder, Niarchos, and Liakos

Published
2009

63. Photometric multi-site campaign on massive B stars in the open cluster chi Persei (NGC 884)

Author

Saesen, S. Pigulski, A. Carrier, F. De Ridder, J. Aerts, C. Handler, G. Narwid, A. Fu, J. N. Zhang, C. Jiang, X. J. Kopacki, G. Vanautgaerden, J. Steslicki, M. Acke, B. Poretti, E. Uytterhoeven, K. De Meester, W. Reed, M. D. Kolaczkowski, Z. Michalska, G. Schmidt, E. Ostensen, R. Gielen, C. Yakut, K. Leitner, A. Kalomeni, B. and Prins, S. Van Helshoecht, V. Zima, W. Huygen, R. and Vandenbussche, B. Lenz, P. Ladjal, D. Antolin, E. Puga and Verhoelst, T. Niarchos, P. Liakos, A. Lorenz, D. Dehaes, S. Reyniers, M. Davignon, G. Kim, S-L Kim, D. H. and Lee, Y-J Lee, C-U Kwon, J-H Broeders, E. Van Winckel, H. and Vanhollebeke, E. Raskin, G. Blom, Y. Eggen, J. R. and Beck, P. Puschnig, J. Schmitt, L. Gelven, G. A. and Steiniger, B. Drummond, R.

Abstract

In 2005 a photometric observation campaign started on the open cluster chi Persei, involving 13 telescopes spread over the whole northern hemisphere. After two years we gathered almost 1200 hours of data. We present here preliminary results on the variability search, especially from the 60-cm telescope in Bialkow (Poland), which show seven confirmed beta Cephei stars, four candidate B-type pulsators and other interesting variable stars.

Published
2008

64. Structure and composition of disks surrounding Herbig Be stars

Author

Ancker, M. van den, Acke, B., Bik, A., Bouwman, J., Dominik, C., Dullemond, K., Henning, T., Min, M., Pantin, E., Tielens, A.G.G.M., Verhoeff, A., Waelkens, C., Waters, L., and Boekel, R. van

Subjects
Research Programm of Institute for Mathematics, Astrophysics and Particle Physics, Spitzer Proposal, Astronomy
Abstract

Item does not contain fulltext

Published
2008

65. An asymmetry detected in the disk of Kappa CMa with the AMBER/VLTI

Author

Meilland, Anthony, Millour, Florentin, Stee, Philippe, Domiciano De Souza, Armando, Petrov, Romain, Mourard, Denis, Jankov, Slobodan, Robbe-Dubois, Sylvie, Spang, Alain, Arisitidi, Eric, Antonelli, P., Beckmann, U., Bresson, Y., Chelli, A., Dugué, M., Duvert, G., Glück, L., Kern, P., Lagarde, S., Le Coarer, E., Lisi, F., Malbet, F., Perraut, K., Puget, P., Robbe-Dubois, S., Weigelt, G., Zins, G., Accardo, M., Acke, B., Agabi, K., Arezki, B., Altariba, E., Baffa, C., Behrend, J., Blöcker, T., Bonhomme, S., Busoni, S., Cassaing, F., Clausse, J.-M., Connot, C., Delboulbé, A., Domicinano De Souza, A., Driebe, T., Feautrier, P., Ferruzzi, D., Forveille, T., Fossat, E., Foy, R., Fraix-Burnet, D., Gallardo, A., Gennari, S., Glentzlin, A., Giani, E., Gilinst, C., Heiden, M., Heininger, M., Hernandez, O., Hofmann, K.-H., Kamm, D., Kraus, S., Le Contel, D., Le Contel, J.-M., Lopez, B., Magnard, Y., Marconi, A., Mars, G., Martinot-Lagarde, G., Mathias, P., Millour, F., Monin, J.-L., Mouillet, D., Mourard, D., Mège, P., Nussbaum, E., Ohnaka, K., Pacini, F., Perrier, C., Rabbia, Y., Rebattu, S., Reynaud, F., Richichi, A., Roussel, A., Sacchettini, M., Salinari, P., Schertl, D., Solscheid, W., Stee, P., Stefanini, P., Tallon, M., Tallon-Bosc, I., Tasso, D., Tatulli, E., Testi, L., Valtier, J.-C., Vannier, M., Ventura, N., Kiekebusch, M., Schöller, M., Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars: emission-line, Astrophysics (astro-ph), Stars: individual (kappa CMa), FOS: Physical sciences, Be, Astrophysics, Techniques: high angular resolution, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars: Keplerian rotation, Techniques: interferometric, Stars: circumstellar matter, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

International audience; Aims. We study the geometry and kinematics of the circumstellar environment of the Be star Kappa CMa in the Br gamma emission line and its nearby continuum. Methods. We use the VLTI/AMBER instrument operating in the K band which provides a spatial resolution of about 6 mas with a spectral resolution of 1500 to study the kinematics within the disk and to infer its rotation law. In order to obtain more kinematical constraints we also use an high spectral resolution Pa beta line profile obtain in December 2005 at the Observatorio do Pico do Dios, Brazil and we compile V/R line profile variations and spectral energy distribution data points from the literature. Results. Using differential visibilities and differential phases across the Br gamma line we detect an asymmetry in the disk. Moreover, we found that kappa CMa seems difficult to fit within the classical scenario for Be stars, illustrated recently by alpha Arae observations, i.e. a fast rotating B star close to its breakup velocity surrounded by a Keplerian circumstellar disk with an enhanced polar wind. Finally we discuss the possibility for kappa CMa to be a critical rotator with a Keplerian rotating disk and try to see if the detected asymmetry can be interpreted within the "one-armed" viscous disk framework.

Published
2006
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66. Disk and wind interaction in the young stellar object MWC 297 spatially resolved with VLTI/AMBER

Author

Malbet, F., Benisty, M., de Wit, W.J., Kraus, S., Meilland, A., Millour, F., Tatulli, E., Berger, J.P., Chesneau, O., Hofmann, K.H., Isella, A., Natta, A., Petrov, R., Preibisch, T., Stee, P., Testi, L., Weigelt, G., Antonelli, P., Beckmann, U., Bresson, Y., Chelli, A., Duvert, G., Glück, L., Kern, P., Lagarde, S., Le Coarer, E., Lisi, F., Perraut, K., Robbe-Dubois, S., Roussel, A., Zins, G., Accardo, M., Acke, B., Agabi, K., Arezki, B., Aristidi, E., Baffa, C., Behrend, J., Blöcker, T., Bonhomme, S., Busoni, S., Cassaing, F., Clausse, J.-M., Colin, J., Connot, C., Delboulbé, A., Driebe, T., Dugué, M., Feautrier, P., Ferruzzi, D., Forveille, T., Fossat, E., Foy, Renaud, Fraix-Burnet, D., Gallardo, A., Gennari, S., Glentzlin, A., Giani, E., Gil, C., Heiden, M., Heininger, M., Kamm, D., Le Contel, D., Le Contel, J.-M., Lopez, B., Magnard, Y., Marconi, A., Mars, G., Martinot-Lagarde, G., Mathias, P., Monin, J.-L., Mouillet, D., Mourard, D., Mège, P., Nussbaum, E., Ohnaka, K., Pacheco, J., Pacini, F., Perrier, C., Puget, P., Rabbia, Y., Rebattu, S., Reynaud, François, Richichi, A., Sacchettini, M., Salinari, P., Schertl, D., Solscheid, W., Stefanini, P., Tallon, Michel, Tallon-Bosc, Isabelle, Tasso, D., Valtier, J.-C., Vannier, M., Ventura, N., Kiekebusch, M., Rantakyrö, F., Schöller, M., Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), ONERA - The French Aerospace Lab [Châtillon], ONERA, Centre de Recherche Astrophysique de Lyon (CRAL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Division technique INSU/SDU (DTI), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), PHOTONIQUE, XLIM (XLIM), Université de Limoges (UNILIM)-Centre National de la Recherche Scientifique (CNRS)-Université de Limoges (UNILIM)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), AMBER, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), ONERA-Université Paris Saclay (COmUE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Protoplanetary disks, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Pre-main-sequence stars, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Planetary systems, Early-type stars, Emission-line stars, Accretion disks, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Infrared, Interferometric Techniques, Astrophysics::Galaxy Astrophysics
Abstract

The young stellar object MWC 297 has been observed with the VLT interferometer equipped with the AMBER instrument. MWC 297 has been spatially resolved in the continuum with a visibility of 0.50 as well as in the Br gamma emission line where the visibility decrease to a lower value of 0.33. This change in the visibility with the wavelength can be interpreted by the presence of an optically thick disk responsible for the visibility in the continuum and of a stellar wind traced by Br gamma and whose apparent size is 40% larger. We validate this interpretation by building a model of the stellar environment that combines a geometrically thin, optically thick accretion disk model consisting of gas and dust, and a latitude-dependent stellar wind outflowing above the disk surface. The continuum emission and visibilities obtained from this model are fully consistent with the interferometric AMBER data. They agree also with existing optical, near-infrared spectra and other broad-band near-infrared interferometric visibilities. A picture emerges in which MWC 297 is surrounded by an equatorial flat disk that is possibly still accreting and an outflowing wind which has a much higher velocity in the polar region than at the equator. [abridged], Comment: 13 pages; to be published in A&A; Acceptance day: 11/10/2005

Published
2005
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67. Detection of solar-like oscillations in the bright red giant starsγPiscium andθ1 Tauri from a 190-day high-precision spectroscopic multi-site campaign

Author

Beck, P. G., primary, Kambe, E., additional, Hillen, M., additional, Corsaro, E., additional, Van Winckel, H., additional, Moravveji, E., additional, De Ridder, J., additional, Bloemen, S., additional, Saesen, S., additional, Mathias, P., additional, Degroote, P., additional, Kallinger, T., additional, Verhoelst, T., additional, Ando, H., additional, Carrier, F., additional, Acke, B., additional, Oreiro, R., additional, Miglio, A., additional, Eggenberger, P., additional, Sato, B., additional, Zwintz, K., additional, Pápics, P. I., additional, Marcos-Arenal, P., additional, Sans Fuentes, S. A., additional, Schmid, V. S., additional, Waelkens, C., additional, Østensen, R., additional, Matthews, J. M., additional, Yoshida, M., additional, Izumiura, H., additional, Koyano, H., additional, Nagayama, S., additional, Shimizu, Y., additional, Okada, N., additional, Okita, K., additional, Sakamoto, A., additional, Yamamuro, T., additional, and Aerts, C., additional

Published
2015
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68. ISO spectroscopy of disks around Herbig Ae/Be stars

Author

Van Den Ancker, M., Acke, Bram, Ancker, Mario, and Acke, B.

Subjects
Physics, Astrophysics (astro-ph), Infrared spectroscopy, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Spectral line, Silicate, Amorphous solid, Stars, chemistry.chemical_compound, chemistry, Space and Planetary Science, Ionization, Spectroscopy, Absorption (electromagnetic radiation)
Abstract

We have investigated the infrared spectra of all 46 Herbig Ae/Be stars for which spectroscopic data is available in the ISO data archive. Our quantitative analysis of these spectra focusses on the emission bands linked to polycyclic aromatic hydrocarbons (PAHs), the amorphous 10 micron silicate band and the crystalline silicate band at 11.3 micron. We have detected PAH emission in 57% of the Herbig stars in our sample. Clear examples of differences in the PAH spectra are present within our sample, indicating differences in PAH size, chemistry and/or ionization. Amorphous silicate emission was detected in the spectra of 52% of the sample stars, amorphous silicate absorption in 13%. We have detected crystalline silicate emission in 11 stars (24% of our sample), of which four (9%) also display strong PAH emission. We have classified the sample sources according to the strength of their mid-IR energy distribution. The systems with stronger mid-infared (20-100 um) excesses relative to their near-infrared (1-5 um) excess display significantly more PAH emission than those with weaker mid-infrared excesses. This provides strong observational support for the disk models by Dullemond (2002), in which systems with a flaring disk geometry display a strong mid-infrared excess, whereas those with disks that are strongly shadowed by the puffed-up inner rim of the disk only display modest amounts of mid-infrared emission. The PAH emission is expected to be produced mainly in the part of the disk atmosphere that is directly exposed to radiation from the central star. In this model, self-shadowed disks should display weaker PAH emission than flared disks, consistent with our observations., 27 pages, 26 figures, A&A accepted (22/06/2004)

Published
2004

70. EXTREME CONDITIONS IN A CLOSE ANALOG TO THE YOUNG SOLAR SYSTEM : HERSCHEL OBSERVATIONS OF is an element of ERIDANI

Author

Greaves, J. S., Sibthorpe, B., Acke, B., Pantin, E. E., Vandenbussche, B., Olofsson, Göran, Dominik, C., Barlow, M. J., Bendo, G. J., Blommaert, J. A. D. L., Brandeker, Alexis, de Vries, Bernard L., Dent, W. R. F., Di Francesco, J., Fridlund, M., Gear, W. K., Harvey, P. M., Hogerheijde, M. R., Holland, W. S., Ivison, R. J., Liseau, R., Matthews, B. C., Pilbratt, G. L., Walker, H. J., Waelkens, C., Greaves, J. S., Sibthorpe, B., Acke, B., Pantin, E. E., Vandenbussche, B., Olofsson, Göran, Dominik, C., Barlow, M. J., Bendo, G. J., Blommaert, J. A. D. L., Brandeker, Alexis, de Vries, Bernard L., Dent, W. R. F., Di Francesco, J., Fridlund, M., Gear, W. K., Harvey, P. M., Hogerheijde, M. R., Holland, W. S., Ivison, R. J., Liseau, R., Matthews, B. C., Pilbratt, G. L., Walker, H. J., and Waelkens, C.

Abstract

Far-infrared Herschel images of the is an element of Eridani system, seen at a fifth of the Sun's present age, resolve two belts of debris emission. Fits to the 160 mu m PACS image yield radial spans for these belts of 12-16 and 54-68 AU. The south end of the outer belt is approximate to 10% brighter than the north end in the PACS+SPIRE images at 160, 250, and 350 mu m, indicating a pericenter glow attributable to a planet c From this asymmetry and an upper bound on the offset of the belt center, this second planet should be mildly eccentric (e(c) approximate to 0.03-0.3). Compared to the asteroid and Kuiper Belts of the young Sun, the is an element of Eri belts are intermediate in brightness and more similar to each other, with up to 20 km sized collisional fragments in the inner belt totaling approximate to 5% of an Earth mass. This reservoir may feed the hot dust close to the star and could send many impactors through the Habitable Zone, especially if it is being perturbed by the suspected planet is an element of Eri b, at semi-major axis approximate to 3 AU., AuthorCount:25

Published
2014
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71. EXTREME CONDITIONS IN A CLOSE ANALOG TO THE YOUNG SOLAR SYSTEM: HERSCHEL OBSERVATIONS OF ϵ ERIDANI

Author

Greaves, J. S., primary, Sibthorpe, B., additional, Acke, B., additional, Pantin, E. E., additional, Vandenbussche, B., additional, Olofsson, G., additional, Dominik, C., additional, Barlow, M. J., additional, Bendo, G. J., additional, Blommaert, J. A. D. L., additional, Brandeker, A., additional, de Vries, B. L., additional, Dent, W. R. F., additional, Di Francesco, J., additional, Fridlund, M., additional, Gear, W. K., additional, Harvey, P. M., additional, Hogerheijde, M. R., additional, Holland, W. S., additional, Ivison, R. J., additional, Liseau, R., additional, Matthews, B. C., additional, Pilbratt, G. L., additional, Walker, H. J., additional, and Waelkens, C., additional

Published
2014
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72. The 69 μm forsterite band in spectra of protoplanetary disks. Results from the herschel digit programme

Author

Sturm, B., Bouwman, J., Henning, T., Evans, N.J., Waters, L.B.F.M., Dishoeck, E.F. van, Green, J.D., Olofsson, J., Meeus, G., Maaskant, K., Dominik, C., Augereau, J.C., Mulders, G.D., Acke, B., Merin, B., Herczeg, G.J., Sturm, B., Bouwman, J., Henning, T., Evans, N.J., Waters, L.B.F.M., Dishoeck, E.F. van, Green, J.D., Olofsson, J., Meeus, G., Maaskant, K., Dominik, C., Augereau, J.C., Mulders, G.D., Acke, B., Merin, B., and Herczeg, G.J.

Abstract

Contains fulltext : 122807.pdf (preprint version ) (Open Access)

Published
2013

73. Comet-like mineralogy of olivine crystals in an extrasolar proto-Kuiper belt

Author

Vries, B.L. de, Acke, B., Blommaert, J., Waelkens, C., Waters, L., Vandenbussche, B., Min, M., Olofsson, G., Dominik, C., Decin, L., Barlow, M.J., Brandeker, A., Francesco, J. Di, Glauser, A.M., Greaves, J., Harvey, P.M., Holland, W.S., Ivison, R.J., Liseau, R., Pantin, E.E., Pilbratt, G.L., Royer, P., Sibthorpe, B., Vries, B.L. de, Acke, B., Blommaert, J., Waelkens, C., Waters, L., Vandenbussche, B., Min, M., Olofsson, G., Dominik, C., Decin, L., Barlow, M.J., Brandeker, A., Francesco, J. Di, Glauser, A.M., Greaves, J., Harvey, P.M., Holland, W.S., Ivison, R.J., Liseau, R., Pantin, E.E., Pilbratt, G.L., Royer, P., and Sibthorpe, B.

Abstract

Item does not contain fulltext

Published
2012

74. CoRoT’s view on variable B8/9 stars: spots versus pulsations

Author

Degroote, P., Acke, B., Samadi, R., Aerts, Conny, Kurtz, D.W., Noels, A., Miglio, A., Montalbán, J., Bloemen, S.L.D., Baglin, A., Baudin, F., Catala, C., Michel, E., Auvergne, M., Degroote, P., Acke, B., Samadi, R., Aerts, Conny, Kurtz, D.W., Noels, A., Miglio, A., Montalbán, J., Bloemen, S.L.D., Baglin, A., Baudin, F., Catala, C., Michel, E., and Auvergne, M.

Abstract

Contains fulltext : 91637.pdf (preprint version ) (Open Access)

Published
2011

75. Low abundance, strong features: window-dressing crystalline forsterite in the disk wall of HD 100546

Author

Astrophysics, Sub Experiment. Astrophysics begr 1/1/14, Mulders, G. D., Waters, L.B.F.M., Dominik, C., Sturm, B., Bouwman, J., Min, M., Verhoeff, A. P., Acke, B., Augereau, J.C., Evans II, N.J., Henning, Th., Meeus, G., Olofsson, J., Astrophysics, Sub Experiment. Astrophysics begr 1/1/14, Mulders, G. D., Waters, L.B.F.M., Dominik, C., Sturm, B., Bouwman, J., Min, M., Verhoeff, A. P., Acke, B., Augereau, J.C., Evans II, N.J., Henning, Th., Meeus, G., and Olofsson, J.

Published
2011

76. This title is unavailable for guests, please login to see more information.

Author

Saesen, S. Pigulski, A. Carrier, F. Michalska, G. Aerts, C. De Ridder, J. Briquet, M. Handler, G. Kołaczkowski, Z. Acke, B. Bauwens, E. Beck Blom, Y. Blommaert, J. Broeders, E. Cherix, M. Davignon, G. Debosscher, J. Degroote, P. Decin, L. Dehaes, S. De Meester, W. Deroo, P. Desmet, M. Drummond, R. Eggen, J.R. Fu, J. Gazeas, K. Gelven, G.A. Gielen, C. Huygen, R. Jiang, X. Kalomeni, B. Kim, S.-L. Kim, D.H. Kopacki, G. Kwon, J.-H. Ladjal, D. Lee, C.-U. Lee, Y.-J. Lefever, K. Leitner, A. Lenz, P. Liakos, A. Lorenz, D. Narwid, A. Niarchos, P. Østensen, R. Poretti, E. Prins, S. Provencal, J. Puga Antolin, E. Puschnig, J. Raskin, G. Reed, M.D. Reyniers, M. Schmidt, E. Schmitzberger, L. Spano, M. Steininger, B. SteeLicki, M. Uytterhoeven, K. Vanautgaerden, J. Vandenbussche, B. Van Helshoecht, V. Vanhollebeke, E. Van Winckel, H. Verhoelst, T. Vućković, M. Waelkens, C. Wolf, G. Yakut, K. Zhang, C. Zima, W. and Saesen, S. Pigulski, A. Carrier, F. Michalska, G. Aerts, C. De Ridder, J. Briquet, M. Handler, G. Kołaczkowski, Z. Acke, B. Bauwens, E. Beck Blom, Y. Blommaert, J. Broeders, E. Cherix, M. Davignon, G. Debosscher, J. Degroote, P. Decin, L. Dehaes, S. De Meester, W. Deroo, P. Desmet, M. Drummond, R. Eggen, J.R. Fu, J. Gazeas, K. Gelven, G.A. Gielen, C. Huygen, R. Jiang, X. Kalomeni, B. Kim, S.-L. Kim, D.H. Kopacki, G. Kwon, J.-H. Ladjal, D. Lee, C.-U. Lee, Y.-J. Lefever, K. Leitner, A. Lenz, P. Liakos, A. Lorenz, D. Narwid, A. Niarchos, P. Østensen, R. Poretti, E. Prins, S. Provencal, J. Puga Antolin, E. Puschnig, J. Raskin, G. Reed, M.D. Reyniers, M. Schmidt, E. Schmitzberger, L. Spano, M. Steininger, B. SteeLicki, M. Uytterhoeven, K. Vanautgaerden, J. Vandenbussche, B. Van Helshoecht, V. Vanhollebeke, E. Van Winckel, H. Verhoelst, T. Vućković, M. Waelkens, C. Wolf, G. Yakut, K. Zhang, C. Zima, W.

Published
2010

77. Waters, dust evolution in protoplanetary disks around herbig ae/be stars—the spitzer view

Author

Astrophysics, Sub Experiment. Astrophysics begr 1/1/14, Juhász, A., Bouwman, J., Henning, Th., Acke, B., Van Den Ancker, M., Meeus, G., Dominik, C., Min, M., Tielens, A. G. G. M., Waters, L.B.F.M., Astrophysics, Sub Experiment. Astrophysics begr 1/1/14, Juhász, A., Bouwman, J., Henning, Th., Acke, B., Van Den Ancker, M., Meeus, G., Dominik, C., Min, M., Tielens, A. G. G. M., and Waters, L.B.F.M.

Published
2010

78. HD 95881: A gas rich to gas poor transition disk?

Author

Astrophysics, Sub Experiment. Astrophysics begr 1/1/14, Afd Astrophysics begr 1/1/17, Verhoeff, A. P., Min, M., Acke, B., Van Boekel, R., Pantin, E., Waters, L.B.F.M., Tielens, A. G. G. M., Van Den Ancker, M. E., Mulders, G. D., de Koter, A., Bouwman, J., Astrophysics, Sub Experiment. Astrophysics begr 1/1/14, Afd Astrophysics begr 1/1/17, Verhoeff, A. P., Min, M., Acke, B., Van Boekel, R., Pantin, E., Waters, L.B.F.M., Tielens, A. G. G. M., Van Den Ancker, M. E., Mulders, G. D., de Koter, A., and Bouwman, J.

Published
2010

79. Dust, Ice, and Gas In Time (DIGIT) Herschel program first results:a full PACS-SED scan of the gas line emission in protostar DK Chamaeleontis

Author

van Kempen, T. A., Green, J. D., Evans, N. J., II, van Dishoeck, E. F., Kristensen, L. E., Herczeg, G. J., Merín, B., Lee, J. -E., Jørgensen, Jes Kristian, Bouwman, Jildau, Acke, B., Adamkovics, M., Augereau, J. C., Bergin, E., Blake, G. A., Brown, P. M. J., Carr, J. S., Chen, J. -H., Cieza, L., Dominik, C., Dullemond, C. P., Dunham, M. M., Glassgold, A., Guedel, M., Harvey, P. M., Henning, Th., Hogerheijde, M. R., Jaffe, D., Kim, H. J., Knez, Claudia, Lacy, J. H., Maret, S., Meeus, G., Meijerink, R., Mulders, G. D., Mundy, L., Najita, J., Olofsson, J., Pontoppidan, K.M., Salyk, Colette, Sturm, B., Visser, R., Waters, L. B. F. M., Waelkens, C., Yildiz, U. A., van Kempen, T. A., Green, J. D., Evans, N. J., II, van Dishoeck, E. F., Kristensen, L. E., Herczeg, G. J., Merín, B., Lee, J. -E., Jørgensen, Jes Kristian, Bouwman, Jildau, Acke, B., Adamkovics, M., Augereau, J. C., Bergin, E., Blake, G. A., Brown, P. M. J., Carr, J. S., Chen, J. -H., Cieza, L., Dominik, C., Dullemond, C. P., Dunham, M. M., Glassgold, A., Guedel, M., Harvey, P. M., Henning, Th., Hogerheijde, M. R., Jaffe, D., Kim, H. J., Knez, Claudia, Lacy, J. H., Maret, S., Meeus, G., Meijerink, R., Mulders, G. D., Mundy, L., Najita, J., Olofsson, J., Pontoppidan, K.M., Salyk, Colette, Sturm, B., Visser, R., Waters, L. B. F. M., Waelkens, C., and Yildiz, U. A.

Published
2010

80. Evidence for CO depletion in the inner regions of gas-rich protoplanetary disks

Author

van der Plas, G., van den Ancker, M.E., Acke, B., Carmona, A., Dominik, C., Fedele, D., Waters, L.B.F.M., van der Plas, G., van den Ancker, M.E., Acke, B., Carmona, A., Dominik, C., Fedele, D., and Waters, L.B.F.M.

Abstract

Contains fulltext : 75700.pdf (preprint version ) (Open Access) Contains fulltext : 75700.pdf (publisher's version ) (Open Access)

Published
2009

82. Photometric multi-site campaign on massive B stars in the open cluster chi Persei (NGC 884)

Author

Saesen, S., Pigulski, A., Carrier, F., DeRidder, J., Aerts, C.C., Handler, G., Narwid, A., Fu, J.N., Zhang, C., Jiang, X.J., Kopacki, G., Vanautgaerden, J., Steslicki, M., Acke, B., Poretti, E., Uytterhoeven, K., DeMeester, W., Reed, M.D., Kolaczkowski, Z., Michalska, G., Schmidt, E., Østensen, R.H., Gielen, C., Yakut, K., Leitner, A., Kalomeni, B., Prins, S., Helshoecht, V. van, Zima, W., Huygen, R., Vandenbussche, B., Lenz, P., Ladjal, D., Antolin, E. Puga, Verhoelst, T., Niarchos, P., Liakos, A., Lorenz, D., Dehaes, S., Reyniers, M., Davignon, G., Kim, S.L., Kim, D.H., Lee, Y.J., Lee, C.U., Kwon, J.H., Broeders, E., Winckel, H. van, Vanhollebeke, E., Raskin, G., Blom, Y., Eggen, J.R., Beck, P., Puschnig, J., Schmitt, L., Gelven, G.A., Steiniger, B., Drummond, R., Saesen, S., Pigulski, A., Carrier, F., DeRidder, J., Aerts, C.C., Handler, G., Narwid, A., Fu, J.N., Zhang, C., Jiang, X.J., Kopacki, G., Vanautgaerden, J., Steslicki, M., Acke, B., Poretti, E., Uytterhoeven, K., DeMeester, W., Reed, M.D., Kolaczkowski, Z., Michalska, G., Schmidt, E., Østensen, R.H., Gielen, C., Yakut, K., Leitner, A., Kalomeni, B., Prins, S., Helshoecht, V. van, Zima, W., Huygen, R., Vandenbussche, B., Lenz, P., Ladjal, D., Antolin, E. Puga, Verhoelst, T., Niarchos, P., Liakos, A., Lorenz, D., Dehaes, S., Reyniers, M., Davignon, G., Kim, S.L., Kim, D.H., Lee, Y.J., Lee, C.U., Kwon, J.H., Broeders, E., Winckel, H. van, Vanhollebeke, E., Raskin, G., Blom, Y., Eggen, J.R., Beck, P., Puschnig, J., Schmitt, L., Gelven, G.A., Steiniger, B., and Drummond, R.

Abstract

Contains fulltext : 71457.pdf (publisher's version ) (Open Access)

Published
2008

83. Long term photometric monitoring with the Mercator telescope. Frequencies and mode identification of variable O-B stars

Author

Cat, P. de, Briquet, M., Aerts, C.C., Goossens, K., Saesen, S., Cuypers, J., Yakut, K., Scuflaire, R., Dupret, M.A., Uytterhoeven, K., Winckel, H. van, Raskin, G., Davignon, G., Guillou, L. Le, Malderen, R. van, Reyniers, M., Acke, B., Meester, W. de, Vanautgaerden, J., Vandenbussche, B., Verhoelst, T., Waelkens, C., Deroo, P., Reyniers, K., Ausseloos, M., Broeders, E., Daszynska-Daszkiewicz, J., Debosscher, J., Ruyter, S. de, Lefever, K., Decin, G., Kolenberg, K., Mazumdar, A., Kerckhoven, C. van, Ridder, J. de, Drummond, R., Barban, C., Vanhollebeke, E., Maas, T., Decin, L., Cat, P. de, Briquet, M., Aerts, C.C., Goossens, K., Saesen, S., Cuypers, J., Yakut, K., Scuflaire, R., Dupret, M.A., Uytterhoeven, K., Winckel, H. van, Raskin, G., Davignon, G., Guillou, L. Le, Malderen, R. van, Reyniers, M., Acke, B., Meester, W. de, Vanautgaerden, J., Vandenbussche, B., Verhoelst, T., Waelkens, C., Deroo, P., Reyniers, K., Ausseloos, M., Broeders, E., Daszynska-Daszkiewicz, J., Debosscher, J., Ruyter, S. de, Lefever, K., Decin, G., Kolenberg, K., Mazumdar, A., Kerckhoven, C. van, Ridder, J. de, Drummond, R., Barban, C., Vanhollebeke, E., Maas, T., and Decin, L.

Abstract

Contains fulltext : 34555.pdf (publisher's version ) (Open Access), Aims. We selected a large sample of O-B stars that were considered as (candidate) slowly pulsating B, beta Cep, and Maia stars after the analysis of their hipparcos data. We analysed our new seven passband geneva data collected for these stars during the first three years of scientific operations of the mercator telescope. We performed a frequency analysis for 28 targets with more than 50 high-quality measurements to improve their variability classification. For the pulsating stars, we tried both to identify the modes and to search for rotationally split modes. Methods: We searched for frequencies in all the geneva passbands and colours by using two independent frequency analysis methods and we applied a 3.6 S/N-level criterion to locate the significant peaks in the periodograms. The modes were identified by applying the method of photometric amplitudes for which we calculated a large, homogeneous grid of equilibrium models to perform a pulsational stability analysis. When both the radius and the projected rotational velocity of an object are known, we determined a lower limit for the rotation frequency to estimate the expected frequency spacings in rotationally split pulsation modes. Results: We detected 61 frequencies, among which 33 are new. We classified 21 objects as pulsating variables (7 new confirmed pulsating stars, including 2 hybrid beta Cep/SPB stars), 6 as non-pulsating variables (binaries or spotted stars), and 1 as photometrically constant. All the Maia candidates were reclassified into other variability classes. We performed mode identification for the pulsating variables for the first time. The most probable l value is 0, 1, 2, and 4 for 1, 31, 9, and 5 modes, respectively, including only 4 unambiguous identifications. For 7 stars we cannot rule out that some of the observed frequencies belong to the same rotationally split mode. For 4 targets we may begin to resolve close frequency multiplets. Based on observations collected with the p7 photometer

Published
2007

84. AMBER and MIDI interferometric observations of the post-AGB binary IRAS 08544-4431: the circumbinary disc resolved

Author

Deroo, P., Acke, B., Verhoelst, T., Dominik, C., Tatulli, E., Winckel, H. van, Deroo, P., Acke, B., Verhoelst, T., Dominik, C., Tatulli, E., and Winckel, H. van

Abstract

Contains fulltext : 35244.pdf (publisher's version ) (Open Access), Context: For a large group of post-AGB binaries, the presence of a stable reservoir of dust is postulated. Although this reservoir will influence the final evolution stages of these objects significantly, its actual geometry and structure remains largely unknown. Aims: We aim at determining the dust morphology of a member of this group, IRAS 08544-4431. Methods: We use the interferometric capabilities of the AMBER and MIDI instruments, operating in the K and N-band respectively. The high spatial resolution measurements are used in conjunction with the broad band spectral characteristics to determine the dust geometry, based on self consistent 2D radiative transfer models. Results: We resolve the object in both K and N. Moreover, using the closure phase capabilities of AMBER, we measure in the K-band a large asymmetry of the dusty environment. The interferometric data are clearly incompatible with a spherical outflow. We model the dusty environment with a passive irradiated dusty disc model. Although this model is constrained mainly on the basis of the spectral energy distribution, it reproduces simultaneously the amplitude and closure phase of the visibilities, in both wavelength bands. Conclusions: Our model of a passive, irradiated disc in equilibrium gives an excellent fit to both the K and N-band visibilities and closure phase. The dust around this evolved binary star is indeed locked in a circumbinary disc with a significant scale height. Grain growth, settling, radial mixing and crystallization are efficient in such an environment. We conclude that the circumbinary disc of this evolved object, is governed by the same physical processes that govern the proto-planetary discs around young stellar objects. Based on observations collected at the European Southern Observatory, Chile: ESO.076.D-0274, ESO.078.D-0113.

Published
2007

85. Herschel detects oxygen in the β Pictoris debris disk.

Author

Brandeker, A., Cataldi, G., Olofsson, G., Vandenbussche, B., Acke, B., Barlow, M. J., Blommaert, J. A. D. L., Cohen, M., Dent, W. R. F., Dominik, C., Francesco, J. Di, Fridlund, M., Gear, W. K., Glauser, A. M., Greaves, J. S., Harvey, P. M., Heras, A. M., Hogerheijde, M. R., Holland, W. S., and Huygen, R.

Abstract

The young star β Pictoris is well known for its dusty debris disk produced through collisional grinding of planetesimals, kilometre-sized bodies in orbit around the star. In addition to dust, small amounts of gas are also known to orbit the star; this gas is likely the result of vaporisation of violently colliding dust grains. The disk is seen edge on and from previous absorption spectroscopy we know that the gas is very rich in carbon relative to other elements. The oxygen content has been more difficult to assess, however, with early estimates finding very little oxygen in the gas at a C/O ratio that is 20× higher than the cosmic value. A C/O ratio that high is difficult to explain and would have far-reaching consequences for planet formation. Here we report on observations by the far-infrared space telescope Herschel, using PACS, of emission lines from ionised carbon and neutral oxygen. The detected emission from C+ is consistent with that previously reported observed by the HIFI instrument on Herschel, while the emission from O is hard to explain without assuming a higher density region in the disk, perhaps in the shape of a clump or a dense torus required to sufficiently excite the O atoms. A possible scenario is that the C/O gas is produced by the same process responsible for the CO clump recently observed by the Atacama Large Millimeter/submillimeter Array in the disk and that the redistribution of the gas takes longer than previously assumed. A more detailed estimate of the C/O ratio and the mass of O will have to await better constraints on the C/O gas spatial distribution. [ABSTRACT FROM AUTHOR]

Published
2016
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87. The orbits of subdwarf B + main-sequence binaries

Author

Vos, J., primary, Østensen, R. H., additional, Degroote, P., additional, De Smedt, K., additional, Green, E. M., additional, Heber, U., additional, Van Winckel, H., additional, Acke, B., additional, Bloemen, S., additional, De Cat, P., additional, Exter, K., additional, Lampens, P., additional, Lombaert, R., additional, Masseron, T., additional, Menu, J., additional, Neyskens, P., additional, Raskin, G., additional, Ringat, E., additional, Rauch, T., additional, Smolders, K., additional, and Tkachenko, A., additional

Published
2012
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88. Erratum: Asteroseismology of the β Cephei star 12 (DD) Lacertae: photometric observations, pulsational frequency analysis and mode identification

Author

Handler, G., primary, Jerzykiewicz, M., additional, Rodríguez, E., additional, Uytterhoeven, K., additional, Amado, P. J., additional, Dorokhova, T. N., additional, Dorokhov, N. I., additional, Poretti, E., additional, Sareyan, J.-P., additional, Parrao, L., additional, Lorenz, D., additional, Zsuffa, D., additional, Drummond, R., additional, Daszyńska-Daszkiewicz, J., additional, Verhoelst, T., additional, De Ridder, J., additional, Acke, B., additional, Bourge, P.-O., additional, Movchan, A. I., additional, Garrido, R., additional, Paparó, M., additional, Sahin, T., additional, Antoci, V., additional, Udovichenko, S. N., additional, Csorba, K., additional, Crowe, R., additional, Berkey, B., additional, Stewart, S., additional, Terry, D., additional, Mkrtichian, D. E., additional, and Aerts, C., additional

Published
2012
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89. Comet-like mineralogy of olivine crystals in an extrasolar proto-Kuiper belt

Author

de Vries, B. L., primary, Acke, B., additional, Blommaert, J. A. D. L., additional, Waelkens, C., additional, Waters, L. B. F. M., additional, Vandenbussche, B., additional, Min, M., additional, Olofsson, G., additional, Dominik, C., additional, Decin, L., additional, Barlow, M. J., additional, Brandeker, A., additional, Di Francesco, J., additional, Glauser, A. M., additional, Greaves, J., additional, Harvey, P. M., additional, Holland, W. S., additional, Ivison, R. J., additional, Liseau, R., additional, Pantin, E. E., additional, Pilbratt, G. L., additional, Royer, P., additional, and Sibthorpe, B., additional

Published
2012
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90. A background galaxy in the field of theβ Pictoris debris disk

Author

Regibo, S., primary, Vandenbussche, B., additional, Waelkens, C., additional, Acke, B., additional, Sibthorpe, B., additional, Nottebaere, M., additional, Voet, K., additional, Di Francesco, J., additional, Fridlund, M., additional, Gear, W. K., additional, Ivison, R. J., additional, and Olofsson, G., additional

Published
2012
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91. Herschelimages of Fomalhaut

Author

Acke, B., primary, Min, M., additional, Dominik, C., additional, Vandenbussche, B., additional, Sibthorpe, B., additional, Waelkens, C., additional, Olofsson, G., additional, Degroote, P., additional, Smolders, K., additional, Pantin, E., additional, Barlow, M. J., additional, Blommaert, J. A. D. L., additional, Brandeker, A., additional, De Meester, W., additional, Dent, W. R. F., additional, Exter, K., additional, Di Francesco, J., additional, Fridlund, M., additional, Gear, W. K., additional, Glauser, A. M., additional, Greaves, J. S., additional, Harvey, P. M., additional, Henning, Th., additional, Hogerheijde, M. R., additional, Holland, W. S., additional, Huygen, R., additional, Ivison, R. J., additional, Jean, C., additional, Liseau, R., additional, Naylor, D. A., additional, Pilbratt, G. L., additional, Polehampton, E. T., additional, Regibo, S., additional, Royer, P., additional, Sicilia-Aguilar, A., additional, and Swinyard, B. M., additional

Published
2012
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92. TheSpitzerspectroscopic survey of S-type stars

Author

Smolders, K., primary, Neyskens, P., additional, Blommaert, J. A. D. L., additional, Hony, S., additional, Van Winckel, H., additional, Decin, L., additional, Van Eck, S., additional, Sloan, G. C., additional, Cami, J., additional, Uttenthaler, S., additional, Degroote, P., additional, Barry, D., additional, Feast, M., additional, Groenewegen, M. A. T., additional, Matsuura, M., additional, Menzies, J., additional, Sahai, R., additional, van Loon, J. Th., additional, Zijlstra, A. A., additional, Acke, B., additional, Bloemen, S., additional, Cox, N., additional, de Cat, P., additional, Desmet, M., additional, Exter, K., additional, Ladjal, D., additional, Østensen, R., additional, Saesen, S., additional, van Wyk, F., additional, Verhoelst, T., additional, and Zima, W., additional

Published
2012
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95. CoRoT’s view on variable B8/9 stars: spots versus pulsations

Author

Degroote, P., primary, Acke, B., additional, Samadi, R., additional, Aerts, C., additional, Kurtz, D. W., additional, Noels, A., additional, Miglio, A., additional, Montalbán, J., additional, Bloemen, S., additional, Baglin, A., additional, Baudin, F., additional, Catala, C., additional, Michel, E., additional, and Auvergne, M., additional

Published
2011
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99. Towards ensemble asteroseismology of the young open clusters χ Persei and NGC 6910

Author

Saesen, S., primary, Pigulski, A., additional, Carrier, F., additional, Michalska, G., additional, Aerts, C., additional, De Ridder, J., additional, Briquet, M., additional, Handler, G., additional, Kołaczkowski, Z., additional, Acke, B., additional, Bauwens, E., additional, Beck, P.G., additional, Blom, Y., additional, Blommaert, J., additional, Broeders, E., additional, Cherix, M., additional, Davignon, G., additional, Debosscher, J., additional, Degroote, P., additional, Decin, L., additional, Dehaes, S., additional, De Meester, W., additional, Deroo, P., additional, Desmet, M., additional, Drummond, R., additional, Eggen, J.R., additional, Fu, J., additional, Gazeas, K., additional, Gelven, G.A., additional, Gielen, C., additional, Huygen, R., additional, Jiang, X., additional, Kalomeni, B., additional, Kim, S.‐L., additional, Kim, D.H., additional, Kopacki, G., additional, Kwon, J.‐H., additional, Ladjal, D., additional, Lee, C.‐U., additional, Lee, Y.‐J., additional, Lefever, K., additional, Leitner, A., additional, Lenz, P., additional, Liakos, A., additional, Lorenz, D., additional, Narwid, A., additional, Niarchos, P., additional, Østensen, R., additional, Poretti, E., additional, Prins, S., additional, Provencal, J., additional, Puga Antolin, E., additional, Puschnig, J., additional, Raskin, G., additional, Reed, M.D., additional, Reyniers, M., additional, Schmidt, E., additional, Schmitzberger, L., additional, Spano, M., additional, Steininger, B., additional, Stęślicki, M., additional, Uytterhoeven, K., additional, Vanautgaerden, J., additional, Vandenbussche, B., additional, Van Helshoecht, V., additional, Vanhollebeke, E., additional, Van Winckel, H., additional, Verhoelst, T., additional, Vučković, M., additional, Waelkens, C., additional, Wolf, G.W., additional, Yakut, K., additional, Zhang, C., additional, and Zima, W., additional

Published
2010
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