Detection of non-radial pulsation and faint companion in the symbiotic star CH Cyg
dc.contributor.author | Pedretti, E. | en_US |
dc.contributor.author | Monnier, John D. | en_US |
dc.contributor.author | Lacour, S. | en_US |
dc.contributor.author | Traub, W. A. | en_US |
dc.contributor.author | Danchi, W. C. | en_US |
dc.contributor.author | Tuthill, P. G. | en_US |
dc.contributor.author | Thureau, N. D. | en_US |
dc.contributor.author | Millan-Gabet, R. | en_US |
dc.contributor.author | Berger, J.-P. | en_US |
dc.contributor.author | Lacasse, M. G. | en_US |
dc.contributor.author | Schuller, P. A. | en_US |
dc.contributor.author | Schloerb, F. P. | en_US |
dc.contributor.author | Carleton, N. P. | en_US |
dc.date.accessioned | 2010-06-01T22:33:49Z | |
dc.date.available | 2010-06-01T22:33:49Z | |
dc.date.issued | 2009-07-21 | en_US |
dc.identifier.citation | Pedretti, E.; Monnier, J. D.; Lacour, S.; Traub, W. A.; Danchi, W. C.; Tuthill, P. G.; Thureau, N. D.; Millan-Gabet, R.; Berger, J.-P.; Lacasse, M. G.; Schuller, P. A.; Schloerb, F. P.; Carleton, N. P. (2009). "Detection of non-radial pulsation and faint companion in the symbiotic star CH Cyg." Monthly Notices of the Royal Astronomical Society 397(1): 325-334. <http://hdl.handle.net/2027.42/75544> | en_US |
dc.identifier.issn | 0035-8711 | en_US |
dc.identifier.issn | 1365-2966 | en_US |
dc.identifier.uri | https://hdl.handle.net/2027.42/75544 | |
dc.description.abstract | We have detected asymmetry in the symbiotic star CH Cyg through the measurement of precision closure phase with the Integrated Optics Near-Infrared Camera (IONIC) beam combiner, at the infrared optical telescope array interferometer. The position of the asymmetry changes with time and is correlated with the phase of the 2.1-year period found in the radial velocity measurements for this star. We can model the time-dependent asymmetry either as the orbit of a low-mass companion around the M giant or as an asymmetric, 20 per cent change in brightness across the M giant. We do not detect a change in the size of the star during a 3-year monitoring period neither with respect to time nor with respect to wavelength. We find a spherical dust shell with an emission size of 2.2 ± 0.1 D * full width at half-maximum around the M giant star. The star to dust flux ratio is estimated to be 11.63 ± 0.3. While the most likely explanation for the 20 per cent change in brightness is non-radial pulsation, we argue that a low-mass companion in close orbit could be the physical cause of the pulsation. The combined effect of pulsation and low-mass companion could explain the behaviour revealed by the radial velocity curves and the time-dependent asymmetry detected in the closure-phase data. If CH Cyg is a typical long secondary period variable then these variations could be explained by the effect of an orbiting low-mass companion on the primary star. | en_US |
dc.format.extent | 2749976 bytes | |
dc.format.extent | 3109 bytes | |
dc.format.mimetype | application/pdf | |
dc.format.mimetype | text/plain | |
dc.publisher | Blackwell Publishing Ltd | en_US |
dc.rights | Journal compilation © 2009 RAS | en_US |
dc.subject.other | Techniques: High Angular Resolution | en_US |
dc.subject.other | Techniques: Interferometric | en_US |
dc.subject.other | Binaries: Symbiotic | en_US |
dc.subject.other | Stars: Imaging | en_US |
dc.subject.other | Stars: Individual: CH Cygni | en_US |
dc.title | Detection of non-radial pulsation and faint companion in the symbiotic star CH Cyg | en_US |
dc.type | Article | en_US |
dc.subject.hlbsecondlevel | Astronomy | en_US |
dc.subject.hlbtoplevel | Science | en_US |
dc.description.peerreviewed | Peer Reviewed | en_US |
dc.contributor.affiliationum | University of Michigan, Astronomy department, 914 Dennison bldg., 500 Church street, Ann Arbor, MI 40109, USA | en_US |
dc.contributor.affiliationother | School of Physics and Astronomy, University of St Andrews, North Haugh, St Andrews KY16 9SS | en_US |
dc.contributor.affiliationother | Laboratoire d'Astrophysique de l'Observatoire de Grenoble (LAOG), 414 rue de la Piscine, BP 53-X Grenoble, France | en_US |
dc.contributor.affiliationother | Jet Propulsion Laboratory, California Institute of Technology, M/S 301–451, 4800 Oak Grove Drive, Pasadena, CA 91109, USA | en_US |
dc.contributor.affiliationother | NASA Goddard Space Flight Center, 8800, Greenbelt Road, Greenbelt, MD 20771, USA | en_US |
dc.contributor.affiliationother | School of Physics, Sydney University, NSW 2006, Sydney, Australia | en_US |
dc.contributor.affiliationother | Michelson Science Center, California Institute of Technology, 770 S. Wilson Ave. MS 100-22, Pasadena, CA 91125, USA | en_US |
dc.contributor.affiliationother | Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA | en_US |
dc.contributor.affiliationother | Institut d'Astrophysique Spatiale, Universit Paris–Sud, bÂtiment 121, 91405 Orsay Cedex, France | en_US |
dc.contributor.affiliationother | University of Massachusetts, Astronomy Department, Amherst, MA 01003-4610, USA | en_US |
dc.description.bitstreamurl | http://deepblue.lib.umich.edu/bitstream/2027.42/75544/1/j.1365-2966.2009.14906.x.pdf | |
dc.identifier.doi | 10.1111/j.1365-2966.2009.14906.x | en_US |
dc.identifier.source | Monthly Notices of the Royal Astronomical Society | en_US |
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